https://wiki.cosmos.esa.int/planckpla2015/api.php?action=feedcontributions&user=Bbarreir&feedformat=atomPlanck PLA 2015 Wiki - User contributions [en-gb]2024-03-29T07:04:18ZUser contributionsMediaWiki 1.31.6https://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10831CMB and astrophysical component maps2015-02-01T14:19:07Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the COMMANDER, NILC, SEVEM, and SMICA pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Appendices A-D of {{PlanckPapers|planck2014-a11}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_smica_tsig.png | '''smica temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''</gallery><br />
</center><br />
<br />
===Product description ===<br />
<br />
====COMMANDER====<br />
<br />
;Principle<br />
<br />
: COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration, bandpass corrections, monopole and dipoles, are fitted jointly with the astrophysical components. A new feature in the Planck 2015 analysis is that the astrophysical model is derived from a combination of Planck, WMAP and a 408 MHz (Haslam et al. 1982) survey, providing sufficient frequency support to resolve the low-frequency components into synchrotron, free-free and spinning dust. For full details, see {{PlanckPapers|planck2014-a12}}.<br />
<br />
; Resolution (effective beam)<br />
<br />
: The Commander sky maps have different angular resolutions depending on data products:<br />
* The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) have a 1 degree FWHM resolution, and are pixelized at N<sub>side</sub>=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood. <br />
* The Commander CMB temperature map derived from Planck-only observations have an angular resolution of ~5 arcmin and is pixelized at N<sub>side</sub>=2048. This map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-857 GHz data), 7.5 arcmin (using 143-857 GHz data), and 5 arcmin (using 217-857 GHz data) are coadded into a single map.<br />
* The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at N<sub>side</sub>=1024. As for the temperature case, this map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-353 GHz data) and 10 arcmin (using 100-353 GHz data) are coadded into a single map.<br />
<br />
; Confidence mask<br />
<br />
: The Commander confidence masks are produced by thresholding the chi-square map characterizing the global fits, combined with direct CO amplitude thresholding to eliminate known leakage effects. In addition, we exclude the 9-year WMAP point source mask in the temperature mask. For full details, see Sections 5 and 6 in {{PlanckPapers|planck2014-a12}}. A total of 81% of the sky is admitted for high-resolution temperature analysis, and 83% for polarization analysis. For low-resolution temperature analysis, for which the additional WMAP and 408 MHz observations improve foreground constraints, a total of 93% of the sky is admitted. <br />
<br />
====NILC====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:SEVEM produces clean CMB maps at several frequencies by using a procedure based on template fitting in real space. The templates are typically constructed from the lowest and highest Planck frequencies and then subtracted from the CMB-dominated channels, with coefficients that are chosen to minimize the variance of the clean map outside a considered mask. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Two single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
<br />
<br />
====SMICA====<br />
; Principle<br />
: SMICA produces CMBs map by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to <math>\ell = 4000</math>. Temperature and polarization maps are produced independently.<br />
; Resolution (effective beam)<br />
: The SMICA intensity map has an effective beam window function of 5 arc-minutes which is truncated at <math>\ell=4000</math> and is '''not''' deconvolved from the pixel window function. Thus the delivered beam window function is the product of a Gaussian beam at 5 arcminutes and the pixel window function for Nside=2048.<br />
: The SMICA Q and U maps are obtained similarly but are produced at Nside=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.<br />
<br />
===Production process===<br />
<br />
====COMMANDER====<br />
<br />
; Pre-processing<br />
<br />
: All sky maps are first convolved to a common resolution that is larger than the largest beam of any frequency channel. For the combined Planck, WMAP and 408 MHz temperature analysis, the common resolution is 1 degree FWHM; for the Planck-only all-frequency analysis it is 40 arcmin FWHM; and for the intermediate-resolution analysis it is 7.5 arcmin; while for the full-resolution analysis, we assume all frequencies between 217 and 857 GHz have a common resolution, and no additional convolution is performed. For polarization, only two smoothing scales are employed, 40 and 10 arcmin, respectively. The instrumental noise rms maps are convolved correspondingly, properly accouting for their matrix-like nature. <br />
<br />
; Priors<br />
<br />
: The following priors are enforced in the Commander analysis:<br />
* All foreground amplitudes are enforced to be positive definite in the low-resolution analysis, while no amplitude priors are enforced in the high-resolution analyses<br />
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies<br />
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky<br />
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors<br />
<br />
; Fitting procedure<br />
<br />
: Given data and priors, Commander either maximizes, or samples from, the Bayesian posterior, P(theta|data). Because this is a highly non-Gaussian and correlated distribution, involving millions of parameters, these operations are performed by means of the Gibbs sampling algorithm, in which joint samples from the full distributions are generated by iteratively sampling from the corresponding conditional posterior distributions, P(theta_i| data, theta_{j/=i}). For the low-resolution analysis, all parameters are optimized jointly, while in the high-resolution analyses, which employs fewer frequency channels, low signal-to-noise parameters are fixed to those derived at low resolution. Examples of such parameters include monopoles and dipoles, calibration and bandpass parameters, thermal dust temperature etc.<br />
<br />
====NILC====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
The templates used in the SEVEM pipeline are typically constructed by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using a total of four templates. Three of them are constructed as the difference of two consecutive Planck channels smoothed to a common resolution (30-44, 44-70 and 545-353) while the 857 GHz channel is chosen as the fourth template. First of all, the six frequency channels which are going to be part of the templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm. The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter the inpainted map with the 545 GHz beam.<br />
<br />
The coefficients are obtained by minimising the variance outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the original data. Our final CMB map is then constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by studying the differences between several SEVEM CMB reconstructions, which correspond to maps cleaned at different frequencies or using different analysis masks. The obtained mask leaves a useful sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. However, given that a narrower frequency coverage is available for polarization, the selected templates and maps to be cleaned are different. In particular, we clean the 70, 100 and 143 GHz using three templates for each channel. The first step of the pipeline is to inpaint the positions of the point sources using the MHW, in those channels which are going to be used in the construction of templates, following the same procedure as for the intensity case. The inpainting is performed in the frequency maps at their native resolution. These inpainted maps are then used to construct a total of four templates. To trace the synchrotron emission, we construct a template as the subtraction of the 30 GHz minus the 44 GHz <br />
map, after being convolved with the beam of each other. For the dust emission, the following templates are considered: 353-217 GHz (smoothed at 10' resolution), 217-143 GHz (used <br />
to clean 70 and 100 GHz) and 217-100 GHz (to clean 143 GHz). These two last templates are constructed at 1 degree resolution since an additional smoothing becomes necessary in<br />
order to increase the signal-to-noise ratio of the template. Conversely to the <br />
intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates. In this way, the 100 GHz <br />
map is used to clean the 143 GHz frequency channel and viceversa, making the clean maps less independent between them than in the intensity case.<br />
<br />
These templates are then used to clean the non-inpainted 70 (at its native resolution), 100 (at 10' resolution) and 143 GHz maps (also at 10'). The corresponding linear coefficients are estimated independently for Q and U by minimising the variance of the clean maps outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at the corresponding raw maps is carried out. The size of the holes to be inpainted takes<br />
into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10' (Gaussian beam) for a HEALPix parameter Nside=1024. Each map is weighted taking into account its <br />
corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky) to avoid the introduction of ringing around the Galactic centre in the filtering process.<br />
<br />
The confidence mask includes all the pixels above a given threshold in a smoothed version of the clean CMB map, the regions more contaminated by the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction of approximately 80 per cent.<br />
<br />
<br />
<br />
====SMICA====<br />
<br />
A) Production of the intensity map.<br />
<br />
; 1) Pre-processing<br />
: Before computing spherical harmonic coefficients, all input maps undergo a pre-processing step to deal with regions of very strong emission (such as the Galactic center) and point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. The diffusive inpainting process is also applied to some regions of very strong emissions. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHz are harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: A confidence mask is determined (see the Planck paper) and all regions which have been masked in the pre-processing step are added to it.<br />
<br />
<br />
<br />
<!--[[File:Smica_filter_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input intensity maps (after they are re-beamed to 5 arc-minutes and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]--><br />
<br />
B) Production of the Q and U polarisation maps.<br />
<br />
The production of the Q and U maps is similar to the production of the intensity map. The SMICA pipeline uses all the 7 polarized Planck channels. After point source masking and diffusive inpainting, the E and B modes are computed and combined to produce E and B modes of the CMB map. Those combined modes are then used to synthesize the U and Q CMB maps. The E and B parts of the input frequency maps being processed jointly, there are, at each multipole, 2*7=14 coefficients (weights) defined to produce the E modes of the CMB map and as many to produce the B part. The weights are displayed in the figure below. The Q and U maps were originally produced at Nside=2048 with a 5-arc-minute resolution, but were downgraded to Nside=1024 with a 10 arc-minute resolution for this release.<br />
<br />
<br />
<!--[[File:Smica_filterEB_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input E and B modes (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), in order to produce the E and B modes of the CMB map. A given frequency channel is encoded in a given color. Solid lines are for E modes and dashed lines are for B modes. The thick lines are for the EE or BB weights; the thin lines are for the EB or BE weights. See the paper for more details.''']]--><br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}.<br />
<br />
===Low-resolution temperature products===<br />
<br />
: The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors. <br />
<br />
====Inputs====<br />
<br />
The following data products are used for the low-resolution analysis:<br />
* Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}<br />
* Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}<br />
* Full-mission 70 GHz ds1 (18+23), ds2 (19+22), and ds3 (20+21) detector-set maps<br />
* Full-mission 100 GHz ds1 and ds2 detector set maps<br />
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps<br />
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps<br />
* Full-mission 353 GHz detector set ds2 and detector 1 maps<br />
* Full-mission 545 GHz detector 2 and 4 maps<br />
* Full-mission 857 GHz detector 2 map<br />
* Beam-symmetrized 9-year WMAP K-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Beam-symmetrized 9-year WMAP Ka-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Default 9-year WMAP Q1 and Q2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Default 9-year WMAP V1 and V2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Default 9-year WMAP W1, W2, W3, and W4 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Re-processed 408 MHz survey map, Remazeilles et al. (2014) [http://lambda.gsfc.nasa.gov/product/foreground/2014_haslam_408_info.cfm (Lambda)]<br />
All maps are smoothed to a common resolution of 1 degree FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256.<br />
<br />
====Outputs====<br />
<br />
=====Synchrotron emission=====<br />
<br />
<!--<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px> <br />
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''<br />
</gallery><br />
</center>--><br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}<br />
: Reference frequency: 408 MHz<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-Synchrotron<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|}<br />
<br />
<br />
=====Free-free emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}}<br />
: Reference frequency: NA<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-freefree<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|EM_ML || Real*4 || cm^-6 pc || Emission measure posterior maximum <br />
|-<br />
|EM_MEAN || Real*4 || cm^-6 pc || Emission measure posterior mean <br />
|-<br />
|EM_RMS || Real*4 || cm^-6 pc || Emission measure posterior rms<br />
|-<br />
|TEMP_ML || Real*4 || K || Electron temperature posterior maximum <br />
|-<br />
|TEMP_MEAN || Real*4 || K || Electron temperature posterior mean <br />
|-<br />
|TEMP_RMS || Real*4 || K || Electron temperature posterior rms<br />
|}<br />
<br />
<br />
=====Spinning dust emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
Note: The spinning dust component has two independent constituents, each corresponding to one spdust2 component, but with different peak frequencies. The two components are stored in the two first FITS extensions, and the template frequency spectrum is stored in the third extension. <br />
<br />
: Reference frequency: 22.8 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-AME1<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Primary amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Primary amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Primary amplitude posterior rms<br />
|-<br />
|FREQ_ML || Real*4 || GHz || Primary peak frequency posterior maximum <br />
|-<br />
|FREQ_MEAN || Real*4 || GHz || Primary peak frequency posterior mean <br />
|-<br />
|FREQ_RMS || Real*4 || GHz || Primary peak frequency posterior rms<br />
|}<br />
<br />
: Reference frequency: 41.0 GHz<br />
: Peak frequency: 33.35 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ Extension 1 -- COMP-MAP-AME2<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Secondary amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Secondary amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Secondary amplitude posterior rms<br />
|}<br />
<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ Extension 2 -- SPINNING-DUST-TEMP<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|nu || Real*4 || GHz || Frequency <br />
|-<br />
|j_nu/nH || Real*4 || Jy sr-1 cm2/H || spdust2 spectrum <br />
|}<br />
<br />
=====CO line emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
Note: The CO line emission component has three independent objects, corresponding to the J1->0, 2->1 and 3->2 lines, stored in separate extensions. <br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-co10<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior rms<br />
|}<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ Extension 1 -- COMP-MAP-co21<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior rms<br />
|}<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ Extension 2 -- COMP-MAP-co32<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior rms<br />
|}<br />
<br />
=====94/100 GHz line emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-xline<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_cmb || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_cmb || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_cmb || Amplitude posterior rms<br />
|}<br />
<br />
Note: The amplitude of this component is normalized according to the 100-ds1 detector set map, ie., it is the amplitude as measured by this detector combination.<br />
<br />
=====Thermal dust emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
: Reference frequency: 545 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-dust<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|-<br />
|TEMP_ML || Real*4 || K || Dust temperature posterior maximum <br />
|-<br />
|TEMP_MEAN || Real*4 || K || Dust temperature posterior mean <br />
|-<br />
|TEMP_RMS || Real*4 || K || Dust temperature posterior rms<br />
|-<br />
|BETA_ML || Real*4 || NA || Emissivity index posterior maximum <br />
|-<br />
|BETA_MEAN || Real*4 || NA || Emissivity index posterior mean <br />
|-<br />
|BETA_RMS || Real*4 || NA || Emissivity index posterior rms<br />
|}<br />
<br />
=====Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SZ-commander_0256_R2.00.fits|link=COM_CompMap_SZ-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-SZ<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Y_ML || Real*4 || y_SZ || Y parameter posterior maximum <br />
|-<br />
|Y_MEAN || Real*4 || y_SZ || Y parameter posterior mean <br />
|-<br />
|Y_RMS || Real*4 || y_SZ || Y parameter posterior rms<br />
|}<br />
<br />
===High-resolution temperature products===<br />
<br />
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz. <br />
<br />
====Inputs====<br />
<br />
The following data products are used for the low-resolution analysis:<br />
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps<br />
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps<br />
* Full-mission 353 GHz detector set ds2 and detector 1 maps<br />
* Full-mission 545 GHz detector 2 and 4 maps<br />
* Full-mission 857 GHz detector 2 map<br />
All maps are smoothed to a common resolution of 7.5 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=2048.<br />
<br />
====Outputs====<br />
<br />
=====CO J2->1 emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO21-commander_2048_R2.00.fits|link=COM_CompMap_CO21-commander_2048_R2.00.fits}}<br />
: Nside = 2048<br />
: Angular resolution = 7.5 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-CO21<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML_FULL || Real*4 || K_RJ km/s || Full-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HM1 || Real*4 || K_RJ km/s || First half-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HR1 || Real*4 || K_RJ km/s || First half-ring amplitude posterior maximum <br />
|-<br />
|I_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring amplitude posterior maximum <br />
|-<br />
|I_ML_YR1 || Real*4 || K_RJ km/s || "First year" amplitude posterior maximum <br />
|-<br />
|I_ML_YR2 || Real*4 || K_RJ km/s || "Second year" amplitude posterior maximum <br />
|}<br />
<br />
<br />
=====Thermal dust emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_ThermalDust-commander_2048_R2.00.fits|link=COM_CompMap_ThermalDust-commander_2048_R2.00.fits}}<br />
: Nside = 2048<br />
: Angular resolution = 7.5 arcmin<br />
<br />
: Reference frequency: 545 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-dust<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML_FULL || Real*4 || uK_RJ || Full-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HM1 || Real*4 || uK_RJ || First half-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HM2 || Real*4 || uK_RJ || Second half-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HR1 || Real*4 || uK_RJ || First half-ring amplitude posterior maximum <br />
|-<br />
|I_ML_HR2 || Real*4 || uK_RJ || Second half-ring amplitude posterior maximum <br />
|-<br />
|I_ML_YR1 || Real*4 || uK_RJ || "First year" amplitude posterior maximum <br />
|-<br />
|I_ML_YR2 || Real*4 || uK_RJ || "Second year" amplitude posterior maximum <br />
|-<br />
|BETA_ML_FULL || Real*4 || NA || Full-mission emissivity index posterior maximum <br />
|-<br />
|BETA_ML_HM1 || Real*4 || NA || First half-mission emissivity index posterior maximum <br />
|-<br />
|BETA_ML_HM2 || Real*4 || NA || Second half-mission emissivity index posterior maximum <br />
|-<br />
|BETA_ML_HR1 || Real*4 || NA || First half-ring emissivity index posterior maximum <br />
|-<br />
|BETA_ML_HR2 || Real*4 || NA || Second half-ring emissivity index posterior maximum <br />
|-<br />
|BETA_ML_YR1 || Real*4 || NA || "First year" emissivity index posterior maximum <br />
|-<br />
|BETA_ML_YR2 || Real*4 || NA || "Second year" emissivity index posterior maximum <br />
|-<br />
|}<br />
<br />
===Polarization products===<br />
<br />
Two polarization foreground products are provided, namely synchrotron and thermal dust emission. The spectral models are assumed identical to the corresponding temperature spectral models.<br />
<br />
====Inputs====<br />
<br />
The following data products are used for the polarization analysis:<br />
* (Only low-resolution analysis) Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}<br />
* (Only low-resolution analysis) Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}<br />
* (Only low-resolution analysis) Full-mission 70 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=70|period=Full|link=LFI 70 GHz frequency maps}}<br />
* Full-mission 100 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=100|period=Full|link=HFI 100 GHz frequency maps}}<br />
* Full-mission 143 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=143|period=Full|link=HFI 143 GHz frequency maps}}<br />
* Full-mission 217 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=217|period=Full|link=HFI 217 GHz frequency maps}}<br />
* Full-mission 353 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=353|period=Full|link=HFI 353 GHz frequency maps}}<br />
In the low-resolution analysis, all maps are smoothed to a common resolution of 40 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256. In the high-resolution analysis (including only CMB and thermal dust emission), the corresponding resolution is 10 arcmin FWHM and Nside=1024.<br />
<br />
====Outputs====<br />
=====Synchrotron emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits|link=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 40 arcmin<br />
<br />
: Reference frequency: 30 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-SynchrotronPol<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Q_ML_FULL || Real*4 || K_RJ km/s || Full-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_FULL || Real*4 || K_RJ km/s || Full-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HM1 || Real*4 || K_RJ km/s || First half-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_HM1 || Real*4 || K_RJ km/s || First half-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HR1 || Real*4 || K_RJ km/s || First half-ring Stokes Q posterior maximum <br />
|-<br />
|U_ML_HR1 || Real*4 || K_RJ km/s || First half-ring Stokes U posterior maximum <br />
|-<br />
|Q_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring Stokes Q posterior maximum <br />
|-<br />
|U_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring Stokes U posterior maximum <br />
|-<br />
|Q_ML_YR1 || Real*4 || K_RJ km/s || "First year" Stokes Q posterior maximum <br />
|-<br />
|U_ML_YR1 || Real*4 || K_RJ km/s || "First year" Stokes U posterior maximum <br />
|-<br />
|Q_ML_YR2 || Real*4 || K_RJ km/s || "Second year" Stokes Q posterior maximum <br />
|-<br />
|U_ML_YR2 || Real*4 || K_RJ km/s || "Second year" Stokes U posterior maximum <br />
|}<br />
<br />
<br />
=====Thermal dust emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_DustPol-commander_1024_R2.00.fits|link=COM_CompMap_DustPol-commander_1024_R2.00.fits}}<br />
: Nside = 1024<br />
: Angular resolution = 10 arcmin<br />
<br />
: Reference frequency: 353 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-DustPol<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Q_ML_FULL || Real*4 || uK_RJ || Full-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_FULL || Real*4 || uK_RJ || Full-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HM1 || Real*4 || uK_RJ || First half-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_HM1 || Real*4 || uK_RJ || First half-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HM2 || Real*4 || uK_RJ || Second half-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_HM2 || Real*4 || uK_RJ || Second half-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HR1 || Real*4 || uK_RJ || First half-ring Stokes Q posterior maximum <br />
|-<br />
|U_ML_HR1 || Real*4 || uK_RJ || First half-ring Stokes U posterior maximum <br />
|-<br />
|Q_ML_HR2 || Real*4 || uK_RJ || Second half-ring Stokes Q posterior maximum <br />
|-<br />
|U_ML_HR2 || Real*4 || uK_RJ || Second half-ring Stokes U posterior maximum <br />
|-<br />
|Q_ML_YR1 || Real*4 || uK_RJ || "First year" Stokes Q posterior maximum <br />
|-<br />
|U_ML_YR1 || Real*4 || uK_RJ || "First year" Stokes U posterior maximum <br />
|-<br />
|Q_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes Q posterior maximum <br />
|-<br />
|U_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes U posterior maximum <br />
|}<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10830CMB and astrophysical component maps2015-02-01T14:18:08Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the COMMANDER, NILC, SEVEM, and SMICA pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Appendices A-D of {{PlanckPapers|planck2014-a11}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_smica_tsig.png | '''smica temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''</gallery><br />
</center><br />
<br />
===Product description ===<br />
<br />
====COMMANDER====<br />
<br />
;Principle<br />
<br />
: COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration, bandpass corrections, monopole and dipoles, are fitted jointly with the astrophysical components. A new feature in the Planck 2015 analysis is that the astrophysical model is derived from a combination of Planck, WMAP and a 408 MHz (Haslam et al. 1982) survey, providing sufficient frequency support to resolve the low-frequency components into synchrotron, free-free and spinning dust. For full details, see {{PlanckPapers|planck2014-a12}}.<br />
<br />
; Resolution (effective beam)<br />
<br />
: The Commander sky maps have different angular resolutions depending on data products:<br />
* The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) have a 1 degree FWHM resolution, and are pixelized at N<sub>side</sub>=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood. <br />
* The Commander CMB temperature map derived from Planck-only observations have an angular resolution of ~5 arcmin and is pixelized at N<sub>side</sub>=2048. This map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-857 GHz data), 7.5 arcmin (using 143-857 GHz data), and 5 arcmin (using 217-857 GHz data) are coadded into a single map.<br />
* The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at N<sub>side</sub>=1024. As for the temperature case, this map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-353 GHz data) and 10 arcmin (using 100-353 GHz data) are coadded into a single map.<br />
<br />
; Confidence mask<br />
<br />
: The Commander confidence masks are produced by thresholding the chi-square map characterizing the global fits, combined with direct CO amplitude thresholding to eliminate known leakage effects. In addition, we exclude the 9-year WMAP point source mask in the temperature mask. For full details, see Sections 5 and 6 in {{PlanckPapers|planck2014-a12}}. A total of 81% of the sky is admitted for high-resolution temperature analysis, and 83% for polarization analysis. For low-resolution temperature analysis, for which the additional WMAP and 408 MHz observations improve foreground constraints, a total of 93% of the sky is admitted. <br />
<br />
====NILC====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:SEVEM produces clean CMB maps at several frequencies by using a procedure based on template fitting in real space. The templates are typically constructed from the lowest and highest Planck frequencies and then subtracted from the CMB-dominated channels, with coefficients that are chosen to minimize the variance of the clean map outside a considered mask. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Two single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
<br />
<br />
====SMICA====<br />
; Principle<br />
: SMICA produces CMBs map by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to <math>\ell = 4000</math>. Temperature and polarization maps are produced independently.<br />
; Resolution (effective beam)<br />
: The SMICA intensity map has an effective beam window function of 5 arc-minutes which is truncated at <math>\ell=4000</math> and is '''not''' deconvolved from the pixel window function. Thus the delivered beam window function is the product of a Gaussian beam at 5 arcminutes and the pixel window function for Nside=2048.<br />
: The SMICA Q and U maps are obtained similarly but are produced at Nside=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.<br />
<br />
===Production process===<br />
<br />
====COMMANDER====<br />
<br />
; Pre-processing<br />
<br />
: All sky maps are first convolved to a common resolution that is larger than the largest beam of any frequency channel. For the combined Planck, WMAP and 408 MHz temperature analysis, the common resolution is 1 degree FWHM; for the Planck-only all-frequency analysis it is 40 arcmin FWHM; and for the intermediate-resolution analysis it is 7.5 arcmin; while for the full-resolution analysis, we assume all frequencies between 217 and 857 GHz have a common resolution, and no additional convolution is performed. For polarization, only two smoothing scales are employed, 40 and 10 arcmin, respectively. The instrumental noise rms maps are convolved correspondingly, properly accouting for their matrix-like nature. <br />
<br />
; Priors<br />
<br />
: The following priors are enforced in the Commander analysis:<br />
* All foreground amplitudes are enforced to be positive definite in the low-resolution analysis, while no amplitude priors are enforced in the high-resolution analyses<br />
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies<br />
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky<br />
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors<br />
<br />
; Fitting procedure<br />
<br />
: Given data and priors, Commander either maximizes, or samples from, the Bayesian posterior, P(theta|data). Because this is a highly non-Gaussian and correlated distribution, involving millions of parameters, these operations are performed by means of the Gibbs sampling algorithm, in which joint samples from the full distributions are generated by iteratively sampling from the corresponding conditional posterior distributions, P(theta_i| data, theta_{j/=i}). For the low-resolution analysis, all parameters are optimized jointly, while in the high-resolution analyses, which employs fewer frequency channels, low signal-to-noise parameters are fixed to those derived at low resolution. Examples of such parameters include monopoles and dipoles, calibration and bandpass parameters, thermal dust temperature etc.<br />
<br />
====NILC====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
The templates used in the SEVEM pipeline are typically constructed by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using a total of four templates. Three of them are constructed as the difference of two consecutive Planck channels smoothed to a common resolution (30-44, 44-70 and 545-353) while the 857 GHz channel is chosen as the fourth template. First of all, the six frequency channels which are going to be part of the templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm. The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter the inpainted map with the 545 GHz beam.<br />
<br />
The coefficients are obtained by minimising the variance outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the original data. Our final CMB map is then constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by studying the differences between several SEVEM CMB reconstructions, which correspond to maps cleaned at different frequencies or using different analysis masks. The obtained mask leaves a useful sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. However, given that a narrower frequency coverage is available for polarization, the selected templates and maps to be cleaned are different. In particular, we clean the 70, 100 and 143 GHz using three templates for each channel. The first step of the pipeline is to inpaint the positions of the point sources using the MHW, in those channels which are going to be used in the construction of templates, following the same procedure as for the intensity case. The inpainting is performed in the frequency maps at their native resolution. These inpainted maps are then used to construct a total of four templates. To trace the synchrotron emission, we construct a template as the subtraction of the 30 GHz minus the 44 GHz <br />
map, after being convolved with the beam of each other. For the dust emission, the following templates are considered: 353-217 GHz (smoothed at 10' resolution), 217-143 GHz (used <br />
to clean 70 and 100 GHz) and 217-100 GHz (to clean 143 GHz). These two last templates are constructed at 1 degree resolution since an additional smoothing becomes necessary in<br />
order to increase the signal-to-noise ratio of the template. Conversely to the <br />
intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates. In this way, the 100 GHz <br />
map is used to clean the 143 GHz frequency channel and viceversa, making the clean maps less independent between them than in the intensity case.<br />
<br />
These templates are then used to clean the non-inpainted 70 (at its native resolution), 100 (at 10' resolution) and 143 GHz maps (also at 10'). The corresponding linear coefficients are estimated independently for Q and U by minimising the variance of the clean maps outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at the corresponding raw maps is carried out. The size of the holes to be inpainted takes<br />
into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10' (Gaussian beam) for a HEALPix parameter Nside=1024. Each map is weighted taking into account its <br />
corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky) to avoid the introduction of ringing around the Galactic centre in the filtering process.<br />
<br />
The confidence mask includes all the pixels above a given threshold in a smoothed version of the clean CMB map, the regions more contaminated by the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction of approximately 80 per cent.<br />
<br />
<br />
<br />
====SMICA====<br />
<br />
A) Production of the intensity map.<br />
<br />
; 1) Pre-processing<br />
: Before computing spherical harmonic coefficients, all input maps undergo a pre-processing step to deal with regions of very strong emission (such as the Galactic center) and point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. The diffusive inpainting process is also applied to some regions of very strong emissions. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHz are harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: A confidence mask is determined (see the Planck paper) and all regions which have been masked in the pre-processing step are added to it.<br />
<br />
<br />
<br />
<!--[[File:Smica_filter_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input intensity maps (after they are re-beamed to 5 arc-minutes and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]--><br />
<br />
B) Production of the Q and U polarisation maps.<br />
<br />
The production of the Q and U maps is similar to the production of the intensity map. The SMICA pipeline uses all the 7 polarized Planck channels. After point source masking and diffusive inpainting, the E and B modes are computed and combined to produce E and B modes of the CMB map. Those combined modes are then used to synthesize the U and Q CMB maps. The E and B parts of the input frequency maps being processed jointly, there are, at each multipole, 2*7=14 coefficients (weights) defined to produce the E modes of the CMB map and as many to produce the B part. The weights are displayed in the figure below. The Q and U maps were originally produced at Nside=2048 with a 5-arc-minute resolution, but were downgraded to Nside=1024 with a 10 arc-minute resolution for this release.<br />
<br />
<br />
<!--[[File:Smica_filterEB_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input E and B modes (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), in order to produce the E and B modes of the CMB map. A given frequency channel is encoded in a given color. Solid lines are for E modes and dashed lines are for B modes. The thick lines are for the EE or BB weights; the thin lines are for the EB or BE weights. See the paper for more details.''']]--><br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}.<br />
<br />
===Low-resolution temperature products===<br />
<br />
: The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors. <br />
<br />
====Inputs====<br />
<br />
The following data products are used for the low-resolution analysis:<br />
* Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}<br />
* Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}<br />
* Full-mission 70 GHz ds1 (18+23), ds2 (19+22), and ds3 (20+21) detector-set maps<br />
* Full-mission 100 GHz ds1 and ds2 detector set maps<br />
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps<br />
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps<br />
* Full-mission 353 GHz detector set ds2 and detector 1 maps<br />
* Full-mission 545 GHz detector 2 and 4 maps<br />
* Full-mission 857 GHz detector 2 map<br />
* Beam-symmetrized 9-year WMAP K-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Beam-symmetrized 9-year WMAP Ka-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Default 9-year WMAP Q1 and Q2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Default 9-year WMAP V1 and V2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Default 9-year WMAP W1, W2, W3, and W4 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]<br />
* Re-processed 408 MHz survey map, Remazeilles et al. (2014) [http://lambda.gsfc.nasa.gov/product/foreground/2014_haslam_408_info.cfm (Lambda)]<br />
All maps are smoothed to a common resolution of 1 degree FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256.<br />
<br />
====Outputs====<br />
<br />
=====Synchrotron emission=====<br />
<br />
<!--<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px> <br />
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''<br />
</gallery><br />
</center>--><br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}<br />
: Reference frequency: 408 MHz<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-Synchrotron<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|}<br />
<br />
<br />
=====Free-free emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}}<br />
: Reference frequency: NA<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-freefree<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|EM_ML || Real*4 || cm^-6 pc || Emission measure posterior maximum <br />
|-<br />
|EM_MEAN || Real*4 || cm^-6 pc || Emission measure posterior mean <br />
|-<br />
|EM_RMS || Real*4 || cm^-6 pc || Emission measure posterior rms<br />
|-<br />
|TEMP_ML || Real*4 || K || Electron temperature posterior maximum <br />
|-<br />
|TEMP_MEAN || Real*4 || K || Electron temperature posterior mean <br />
|-<br />
|TEMP_RMS || Real*4 || K || Electron temperature posterior rms<br />
|}<br />
<br />
<br />
=====Spinning dust emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
Note: The spinning dust component has two independent constituents, each corresponding to one spdust2 component, but with different peak frequencies. The two components are stored in the two first FITS extensions, and the template frequency spectrum is stored in the third extension. <br />
<br />
: Reference frequency: 22.8 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-AME1<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Primary amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Primary amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Primary amplitude posterior rms<br />
|-<br />
|FREQ_ML || Real*4 || GHz || Primary peak frequency posterior maximum <br />
|-<br />
|FREQ_MEAN || Real*4 || GHz || Primary peak frequency posterior mean <br />
|-<br />
|FREQ_RMS || Real*4 || GHz || Primary peak frequency posterior rms<br />
|}<br />
<br />
: Reference frequency: 41.0 GHz<br />
: Peak frequency: 33.35 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ Extension 1 -- COMP-MAP-AME2<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Secondary amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Secondary amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Secondary amplitude posterior rms<br />
|}<br />
<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ Extension 2 -- SPINNING-DUST-TEMP<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|nu || Real*4 || GHz || Frequency <br />
|-<br />
|j_nu/nH || Real*4 || Jy sr-1 cm2/H || spdust2 spectrum <br />
|}<br />
<br />
=====CO line emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
Note: The CO line emission component has three independent objects, corresponding to the J1->0, 2->1 and 3->2 lines, stored in separate extensions. <br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-co10<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior rms<br />
|}<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ Extension 1 -- COMP-MAP-co21<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior rms<br />
|}<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ Extension 2 -- COMP-MAP-co32<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior rms<br />
|}<br />
<br />
=====94/100 GHz line emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-xline<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_cmb || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_cmb || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_cmb || Amplitude posterior rms<br />
|}<br />
<br />
Note: The amplitude of this component is normalized according to the 100-ds1 detector set map, ie., it is the amplitude as measured by this detector combination.<br />
<br />
=====Thermal dust emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
: Reference frequency: 545 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-dust<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|-<br />
|TEMP_ML || Real*4 || K || Dust temperature posterior maximum <br />
|-<br />
|TEMP_MEAN || Real*4 || K || Dust temperature posterior mean <br />
|-<br />
|TEMP_RMS || Real*4 || K || Dust temperature posterior rms<br />
|-<br />
|BETA_ML || Real*4 || NA || Emissivity index posterior maximum <br />
|-<br />
|BETA_MEAN || Real*4 || NA || Emissivity index posterior mean <br />
|-<br />
|BETA_RMS || Real*4 || NA || Emissivity index posterior rms<br />
|}<br />
<br />
=====Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SZ-commander_0256_R2.00.fits|link=COM_CompMap_SZ-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-SZ<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Y_ML || Real*4 || y_SZ || Y parameter posterior maximum <br />
|-<br />
|Y_MEAN || Real*4 || y_SZ || Y parameter posterior mean <br />
|-<br />
|Y_RMS || Real*4 || y_SZ || Y parameter posterior rms<br />
|}<br />
<br />
===High-resolution temperature products===<br />
<br />
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz. <br />
<br />
====Inputs====<br />
<br />
The following data products are used for the low-resolution analysis:<br />
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps<br />
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps<br />
* Full-mission 353 GHz detector set ds2 and detector 1 maps<br />
* Full-mission 545 GHz detector 2 and 4 maps<br />
* Full-mission 857 GHz detector 2 map<br />
All maps are smoothed to a common resolution of 7.5 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=2048.<br />
<br />
====Outputs====<br />
<br />
=====CO J2->1 emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO21-commander_2048_R2.00.fits|link=COM_CompMap_CO21-commander_2048_R2.00.fits}}<br />
: Nside = 2048<br />
: Angular resolution = 7.5 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-CO21<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML_FULL || Real*4 || K_RJ km/s || Full-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HM1 || Real*4 || K_RJ km/s || First half-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HR1 || Real*4 || K_RJ km/s || First half-ring amplitude posterior maximum <br />
|-<br />
|I_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring amplitude posterior maximum <br />
|-<br />
|I_ML_YR1 || Real*4 || K_RJ km/s || "First year" amplitude posterior maximum <br />
|-<br />
|I_ML_YR2 || Real*4 || K_RJ km/s || "Second year" amplitude posterior maximum <br />
|}<br />
<br />
<br />
=====Thermal dust emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_ThermalDust-commander_2048_R2.00.fits|link=COM_CompMap_ThermalDust-commander_2048_R2.00.fits}}<br />
: Nside = 2048<br />
: Angular resolution = 7.5 arcmin<br />
<br />
: Reference frequency: 545 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-dust<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML_FULL || Real*4 || uK_RJ || Full-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HM1 || Real*4 || uK_RJ || First half-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HM2 || Real*4 || uK_RJ || Second half-mission amplitude posterior maximum <br />
|-<br />
|I_ML_HR1 || Real*4 || uK_RJ || First half-ring amplitude posterior maximum <br />
|-<br />
|I_ML_HR2 || Real*4 || uK_RJ || Second half-ring amplitude posterior maximum <br />
|-<br />
|I_ML_YR1 || Real*4 || uK_RJ || "First year" amplitude posterior maximum <br />
|-<br />
|I_ML_YR2 || Real*4 || uK_RJ || "Second year" amplitude posterior maximum <br />
|-<br />
|BETA_ML_FULL || Real*4 || NA || Full-mission emissivity index posterior maximum <br />
|-<br />
|BETA_ML_HM1 || Real*4 || NA || First half-mission emissivity index posterior maximum <br />
|-<br />
|BETA_ML_HM2 || Real*4 || NA || Second half-mission emissivity index posterior maximum <br />
|-<br />
|BETA_ML_HR1 || Real*4 || NA || First half-ring emissivity index posterior maximum <br />
|-<br />
|BETA_ML_HR2 || Real*4 || NA || Second half-ring emissivity index posterior maximum <br />
|-<br />
|BETA_ML_YR1 || Real*4 || NA || "First year" emissivity index posterior maximum <br />
|-<br />
|BETA_ML_YR2 || Real*4 || NA || "Second year" emissivity index posterior maximum <br />
|-<br />
|}<br />
<br />
===Polarization products===<br />
<br />
Two polarization foreground products are provided, namely synchrotron and thermal dust emission. The spectral models are assumed identical to the corresponding temperature spectral models.<br />
<br />
====Inputs====<br />
<br />
The following data products are used for the polarization analysis:<br />
* (Only low-resolution analysis) Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}<br />
* (Only low-resolution analysis) Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}<br />
* (Only low-resolution analysis) Full-mission 70 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=70|period=Full|link=LFI 70 GHz frequency maps}}<br />
* Full-mission 100 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=100|period=Full|link=HFI 100 GHz frequency maps}}<br />
* Full-mission 143 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=143|period=Full|link=HFI 143 GHz frequency maps}}<br />
* Full-mission 217 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=217|period=Full|link=HFI 217 GHz frequency maps}}<br />
* Full-mission 353 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=353|period=Full|link=HFI 353 GHz frequency maps}}<br />
In the low-resolution analysis, all maps are smoothed to a common resolution of 40 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256. In the high-resolution analysis (including only CMB and thermal dust emission), the corresponding resolution is 10 arcmin FWHM and Nside=1024.<br />
<br />
====Outputs====<br />
=====Synchrotron emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits|link=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits}}<br />
: Nside = 256<br />
: Angular resolution = 40 arcmin<br />
<br />
: Reference frequency: 30 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-SynchrotronPol<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Q_ML_FULL || Real*4 || K_RJ km/s || Full-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_FULL || Real*4 || K_RJ km/s || Full-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HM1 || Real*4 || K_RJ km/s || First half-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_HM1 || Real*4 || K_RJ km/s || First half-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HR1 || Real*4 || K_RJ km/s || First half-ring Stokes Q posterior maximum <br />
|-<br />
|U_ML_HR1 || Real*4 || K_RJ km/s || First half-ring Stokes U posterior maximum <br />
|-<br />
|Q_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring Stokes Q posterior maximum <br />
|-<br />
|U_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring Stokes U posterior maximum <br />
|-<br />
|Q_ML_YR1 || Real*4 || K_RJ km/s || "First year" Stokes Q posterior maximum <br />
|-<br />
|U_ML_YR1 || Real*4 || K_RJ km/s || "First year" Stokes U posterior maximum <br />
|-<br />
|Q_ML_YR2 || Real*4 || K_RJ km/s || "Second year" Stokes Q posterior maximum <br />
|-<br />
|U_ML_YR2 || Real*4 || K_RJ km/s || "Second year" Stokes U posterior maximum <br />
|}<br />
<br />
<br />
=====Thermal dust emission=====<br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_DustPol-commander_1024_R2.00.fits|link=COM_CompMap_DustPol-commander_1024_R2.00.fits}}<br />
: Nside = 1024<br />
: Angular resolution = 10 arcmin<br />
<br />
: Reference frequency: 353 GHz<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-DustPol<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Q_ML_FULL || Real*4 || uK_RJ || Full-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_FULL || Real*4 || uK_RJ || Full-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HM1 || Real*4 || uK_RJ || First half-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_HM1 || Real*4 || uK_RJ || First half-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HM2 || Real*4 || uK_RJ || Second half-mission Stokes Q posterior maximum <br />
|-<br />
|U_ML_HM2 || Real*4 || uK_RJ || Second half-mission Stokes U posterior maximum <br />
|-<br />
|Q_ML_HR1 || Real*4 || uK_RJ || First half-ring Stokes Q posterior maximum <br />
|-<br />
|U_ML_HR1 || Real*4 || uK_RJ || First half-ring Stokes U posterior maximum <br />
|-<br />
|Q_ML_HR2 || Real*4 || uK_RJ || Second half-ring Stokes Q posterior maximum <br />
|-<br />
|U_ML_HR2 || Real*4 || uK_RJ || Second half-ring Stokes U posterior maximum <br />
|-<br />
|Q_ML_YR1 || Real*4 || uK_RJ || "First year" Stokes Q posterior maximum <br />
|-<br />
|U_ML_YR1 || Real*4 || uK_RJ || "First year" Stokes U posterior maximum <br />
|-<br />
|Q_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes Q posterior maximum <br />
|-<br />
|U_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes U posterior maximum <br />
|}<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10781CMB and astrophysical component maps2015-01-31T21:44:35Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the COMMANDER, NILC, SEVEM, and SMICA pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Appendices A-D of {{PlanckPapers|planck2014-a11}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_smica_tsig.png | '''smica temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''</gallery><br />
</center><br />
<br />
===Product description ===<br />
<br />
====COMMANDER====<br />
<br />
;Principle<br />
<br />
: COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration, bandpass corrections, monopole and dipoles, are fitted jointly with the astrophysical components. A new feature in the Planck 2015 analysis is that the astrophysical model is derived from a combination of Planck, WMAP and a 408 MHz (Haslam et al. 1982) survey, providing sufficient frequency support to resolve the low-frequency components into synchrotron, free-free and spinning dust. For full details, see {{PlanckPapers|planck2014-a12}}.<br />
<br />
; Resolution (effective beam)<br />
<br />
: The Commander sky maps have different angular resolutions depending on data products:<br />
* The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) have a 1 degree FWHM resolution, and are pixelized at N<sub>side</sub>=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood. <br />
* The Commander CMB temperature map derived from Planck-only observations have an angular resolution of ~5 arcmin and is pixelized at N<sub>side</sub>=2048. This map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-857 GHz data), 7.5 arcmin (using 143-857 GHz data), and 5 arcmin (using 217-857 GHz data) are coadded into a single map.<br />
* The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at N<sub>side</sub>=1024. As for the temperature case, this map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-353 GHz data) and 10 arcmin (using 100-353 GHz data) are coadded into a single map.<br />
<br />
; Confidence mask<br />
<br />
: The Commander confidence masks are produced by thresholding the chi-square map characterizing the global fits, combined with direct CO amplitude thresholding to eliminate known leakage effects. In addition, we exclude the 9-year WMAP point source mask in the temperature mask. For full details, see Sections 5 and 6 in {{PlanckPapers|planck2014-a12}}. A total of 81% of the sky is admitted for high-resolution temperature analysis, and 83% for polarization analysis. For low-resolution temperature analysis, for which the additional WMAP and 408 MHz observations improve foreground constraints, a total of 93% of the sky is admitted. <br />
<br />
====NILC====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:SEVEM produces clean CMB maps at several frequencies by using a procedure based on template fitting in real space. The templates are typically constructed from the lowest and highest Planck frequencies and then subtracted from the CMB-dominated channels, with coefficients that are chosen to minimize the variance of the clean map outside a considered mask. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Two single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
<br />
<br />
====SMICA====<br />
; Principle<br />
: SMICA produces CMBs map by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to <math>\ell = 4000</math>. Temperature and polarization maps are produced independently.<br />
; Resolution (effective beam)<br />
: The SMICA intensity map has an effective beam window function of 5 arc-minutes which is truncated at <math>\ell=4000</math> and is '''not''' deconvolved from the pixel window function. Thus the delivered beam window function is the product of a Gaussian beam at 5 arcminutes and the pixel window function for Nside=2048.<br />
: The SMICA Q and U maps are obtained similarly but are produced at Nside=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.<br />
<br />
===Production process===<br />
<br />
====COMMANDER====<br />
<br />
; Pre-processing<br />
<br />
: All sky maps are first convolved to a common resolution that is larger than the largest beam of any frequency channel. For the combined Planck, WMAP and 408 MHz temperature analysis, the common resolution is 1 degree FWHM; for the Planck-only all-frequency analysis it is 40 arcmin FWHM; and for the intermediate-resolution analysis it is 7.5 arcmin; while for the full-resolution analysis, we assume all frequencies between 217 and 857 GHz have a common resolution, and no additional convolution is performed. For polarization, only two smoothing scales are employed, 40 and 10 arcmin, respectively. The instrumental noise rms maps are convolved correspondingly, properly accouting for their matrix-like nature. <br />
<br />
; Priors<br />
<br />
: The following priors are enforced in the Commander analysis:<br />
* All foreground amplitudes are enforced to be positive definite in the low-resolution analysis, while no amplitude priors are enforced in the high-resolution analyses<br />
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies<br />
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky<br />
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors<br />
<br />
; Fitting procedure<br />
<br />
: Given data and priors, Commander either maximizes, or samples from, the Bayesian posterior, P(theta|data). Because this is a highly non-Gaussian and correlated distribution, involving millions of parameters, these operations are performed by means of the Gibbs sampling algorithm, in which joint samples from the full distributions are generated by iteratively sampling from the corresponding conditional posterior distributions, P(theta_i| data, theta_{j/=i}). For the low-resolution analysis, all parameters are optimized jointly, while in the high-resolution analyses, which employs fewer frequency channels, low signal-to-noise parameters are fixed to those derived at low resolution. Examples of such parameters include monopoles and dipoles, calibration and bandpass parameters, thermal dust temperature etc.<br />
<br />
====NILC====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
The templates used in the SEVEM pipeline are typically constructed by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using a total of four templates. Three of them are constructed as the difference of two consecutive Planck channels smoothed to a common resolution (30-44, 44-70 and 545-353) while the 857 GHz channel is chosen as the fourth template. First of all, the six frequency channels which are going to be part of the templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm. The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter the inpainted map with the 545 GHz beam.<br />
<br />
The coefficients are obtained by minimising the variance outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the original data. Our final CMB map is then constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by studying the differences between several SEVEM CMB reconstructions, which correspond to maps cleaned at different frequencies or using different analysis masks. The obtained mask leaves a useful sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the $Q$ and $U$ maps independently. However, given that a narrower frequency coverage is available for polarization, the selected templates and maps to be cleaned are different. In particular, we clean the 70, 100 and 143 GHz using three templates for each channel. The first step of the pipeline is to inpaint the positions of the point sources using the MHW, in those channels which are going to be used in the construction of templates, following the same procedure as for the intensity case. The inpainting is performed in the frequency maps at their native resolution. These inpainted maps are then used to construct a total of four templates. To trace the synchrotron emission, we construct a template as the subtraction of the 30 GHz minus the 44 GHz <br />
map, after being convolved with the beam of each other. For the dust emission, the following templates are considered: 353--217 GHz (smoothed at 10$'$ resolution), 217--143 GHz (used <br />
to clean 70 and 100 GHz) and 217--100 GHz (to clean 143 GHz). These two last templates are constructed at 1 degree resolution since an additional smoothing becomes necessary in<br />
order to increase the signal-to-noise ratio of the template. Conversely to the <br />
intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates. In this way, the 100 GHz <br />
map is used to clean the 143 GHz frequency channel and viceversa, making the clean maps less independent between them than in the intensity case.<br />
<br />
These templates are then used to clean the non-inpainted 70 (at its native resolution), 100 (at 10$'$ resolution) and 143 GHz maps (also at 10$'$). The corresponding linear coefficients are estimated independently for $Q$ and $U$ by minimising the variance of the clean maps outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at the corresponding raw maps is carried out. The size of the holes to be inpainted takes<br />
into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using $E$ and $B$ decomposition, to produce the final CMB maps for the $Q$ and $U$ components at a resolution of 10$'$ (Gaussian beam) for a HEALPix parameter Nside=1024. Each map is weighted taking into account its <br />
corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky) to avoid the introduction of ringing around the Galactic centre in the filtering process.<br />
<br />
The confidence mask includes all the pixels above a given threshold in a smoothed version of the clean CMB map, the regions more contaminated by the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction of approximately 80 per cent.<br />
<br />
<br />
<br />
====SMICA====<br />
<br />
A) Production of the intensity map.<br />
<br />
; 1) Pre-processing<br />
: Before computing spherical harmonic coefficients, all input maps undergo a pre-processing step to deal with regions of very strong emission (such as the Galactic center) and point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. The diffusive inpainting process is also applied to some regions of very strong emissions. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHz are harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: A confidence mask is determined (see the Planck paper) and all regions which have been masked in the pre-processing step are added to it.<br />
<br />
<br />
<br />
<!--[[File:Smica_filter_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input intensity maps (after they are re-beamed to 5 arc-minutes and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]--><br />
<br />
B) Production of the Q and U polarisation maps.<br />
<br />
The production of the Q and U maps is similar to the production of the intensity map. The SMICA pipeline uses all the 7 polarized Planck channels. After point source masking and diffusive inpainting, the E and B modes are computed and combined to produce E and B modes of the CMB map. Those combined modes are then used to synthesize the U and Q CMB maps. The E and B parts of the input frequency maps being processed jointly, there are, at each multipole, 2*7=14 coefficients (weights) defined to produce the E modes of the CMB map and as many to produce the B part. The weights are displayed in the figure below. The Q and U maps were originally produced at Nside=2048 with a 5-arc-minute resolution, but were downgraded to Nside=1024 with a 10 arc-minute resolution for this release.<br />
<br />
<br />
<!--[[File:Smica_filterEB_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input E and B modes (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), in order to produce the E and B modes of the CMB map. A given frequency channel is encoded in a given color. Solid lines are for E modes and dashed lines are for B modes. The thick lines are for the EE or BB weights; the thin lines are for the EB or BE weights. See the paper for more details.''']]--><br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}.<br />
<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353, 545, 857 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=545|period=Nominal|zodi=uncorr|link=HFI 545 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=857|period=Nominal|zodi=uncorr|link=HFI 857 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
<br />
===Low-resolution temperature products===<br />
<br />
: The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors. The full set of data products derived from the low-resolution joint analysis are the following:<br />
<br />
=====Synchrotron emission=====<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px> <br />
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''<br />
</gallery><br />
</center><br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}<br />
: Reference frequency: 408 MHz<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-Synchrotron<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|}<br />
<br />
<br />
<br />
; Free-free emission<br />
: (Coming soon!)<br />
<br />
; Spinning dust emission<br />
: (Coming soon!)<br />
<br />
; CO line emission<br />
: (Coming soon!)<br />
<br />
; 94/100 GHz line emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
; Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters<br />
: (Coming soon!)<br />
<br />
===High-resolution temperature products===<br />
<br />
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz. These data products include the following:<br />
<br />
; CO(2-1) emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Astrophysical_component_separation&diff=10780Astrophysical component separation2015-01-31T21:31:37Z<p>Bbarreir: </p>
<hr />
<div>==CMB and foreground separation==<br />
<br />
See the Component Separation paper {{PlanckPapers|planck2013-p06}} for details.<br />
===NILC===<br />
NILC is a linear method for combining the input channels. It implements an ILC with weighting coefficients varying over the sky and over the multipole range up to <math>\ell=3200</math> and it does so using 'needlets' which are spherical wavelets. A special procedure is used for processing the coarsest needlet scale<br />
which contains the large scale multipoles.<br />
===SEVEM===<br />
The aim of Sevem is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations (Leach et al., 2008) and to WMAP polarisation data (Fernandez-Cobos et al., 2012). In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.<br />
<br />
The input maps used are all the Planck frequency channels. In particular for intensity, we have cleaned the 100, 143 GHz and 217 GHz maps using four templates. Three or them are constructed as the difference of the following Planck channels (smoothed to a common resolution to remove the CMB contribution): (30-44) GHz, (44-70) GHz, (545-353) GHz and a fourt template given by the 857 GHz channel (smoothed at the resolution of the 545 GHz channel). For polarization we clean maps at frequencies of 70, 100 and 143 GHz using three templates for each channel. In particular, we use (30-44) GHz smoothed to a common resolution, (353-217) at 10', and (217-143) GHz at 1 degree resolution to clean 70 and 100. To clean the 143 GHz channel, the last template is replaced by (217-100) GHz at 1 degree resolution. Before constructing the templates, for both intensity and polarization, we perform inpainting in the detected point sources positions to reduce its contamination in the final map. <br />
<br />
A linear combination of the templates is then subtracted from the Planck sky map at the considered frequency, in order to produce the clean CMB map. The coefficients of the linear combination are obtained by minimising the variance of the clean map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas). Inpainting of point sources is also carried out in the clean maps.<br />
<br />
The final CMB intensity map has then been constructed by combining the 143 and 217 GHz cleaned maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM=5 arcminutes at Nside=2048. The final CMB polarization map has been obtained by combining the 100 and 143 GHz clean maps at Nside=1024 and has a resolution of 10 arc minutes.<br />
<br />
===SMICA===<br />
<br />
<br />
A linear method, SMICA reconstructs a CMB map as a linear combination<br />
in the harmonic domain of <math>N_{chan}</math> input frequency maps<br />
with weights that depend on multipole <math>\ell</math>. Given the<br />
<math>N_{chan} × 1</math> vector <math>\mathbf{x}_{\ell m}</math> of<br />
spherical harmonic coefficients for the input maps, it computes<br />
coefficients <math>s_{\ell m}</math> for the CMB map as<br />
<br />
: <math>\label{eq:smica:shat} <br />
\hat{s}_{\ell m} = \mathbf{w}^†_\ell \mathbf{x}_{\ell m}</math><br />
<br />
where the <math>N_{chan} × 1</math> vector <math>\mathbf{w}_\ell<br />
</math> which contains the multipole-dependent weights is built to<br />
offer unit gain to the CMB with minimum variance. This is achieved<br />
with<br />
<br />
: <math>\label{eq:smica:w} <br />
\mathbf{w}_\ell = \frac{\mathbf{R}_\ell ^{-1} \mathbf{a}}{\mathbf{a}^† \mathbf{R}_\ell ^{-1} \mathbf{a}} </math><br />
<br />
where vector <math>\mathbf{a}</math> is the emission spectrum of the<br />
CMB evaluated at each channel (allowing for possible inter-channel<br />
recalibration factors) and <math> \mathbf{R}_\ell </math> is the<br />
<math>N_{chan} × N_{chan}</math> spectral covariance matrix of<br />
<math>\mathbf{x}_{\ell m}</math>. Taking <math>\mathbf{R}_\ell </math><br />
in Eq. \ref{eq:smica:w} to be the sample spectral covariance matrix<br />
<math>\mathbf{\hat{R}}_\ell </math> of the observations:<br />
<br />
: <math>\label{eq:smica:Rhat} <br />
\mathbf{\hat{R}}_\ell = \frac{1}{2 \ell + 1} \sum_m \mathbf{x}_{ \ell m} \mathbf{x}_{\ell m}^†</math> <br />
<br />
would implement a simple harmonic-domain ILC. This is not what SMICA<br />
does. As discussed below, we instead use a model <math>\mathbf{R}_\ell<br />
(θ)</math> and determine the covariance matrix to be used in<br />
Eq. \ref{eq:smica:w} by fitting <math>\mathbf{R}_\ell (θ)</math> to<br />
<math>\mathbf{\hat{R}}_\ell </math>. This is done in the maximum<br />
likelihood sense for stationary Gaussian fields, yielding the best fit<br />
model parameters θ as<br />
<br />
: <math>\label{eq:smica:thetahat}<br />
\hat{θ} = \rm{arg \, min}_θ \sum_\ell (2\ell + 1) ( \mathbf{\hat{R}}_\ell \mathbf{R}_\ell (θ)^{-1} \, +\, log \, det \, \mathbf{R}_\ell (θ)).</math><br />
<br />
<br />
SMICA models the data is a superposition of CMB, noise and<br />
foregrounds. The latter are not parametrically modelled; instead, we<br />
represent the total foreground emission by <math>d</math> templates<br />
with arbitrary frequency spectra, angular spectra and correlations:<br />
<br />
: <math> \label{eq:smica:Rmodel}<br />
\mathbf{R}_\ell (θ) = \mathbf{aa}^† \, C_\ell \, + \, \mathbf{A P}_\ell \mathbf{A}^† \, + \, \mathbf{N}_\ell <br />
</math> <br />
<br />
where <math>C_\ell </math> is the angular power spectrum of the CMB,<br />
<math>\mathbf{A}</math> is a <math>N_{chan} ×d</math> matrix,<br />
<math>\mathbf{P}_\ell </math> is a positive <math>d×d</math> matrix,<br />
and <math>\mathbf{N}_\ell </math> is a diagonal matrix representing<br />
the noise power spectrum. The parameter vector <math>θ</math> contains<br />
all or part of the quantities in Eq. (5).<br />
<br />
<br />
The above equations summarize the founding principles of SMICA; its<br />
actual operation depends on a choice for the spectral model<br />
<math>\mathbf{R}_\ell (θ)</math> and on several<br />
implementation-specific details.<br />
<br />
<br />
<br />
The actual implementation of SMICA includes the following steps:<br />
; Inputs<br />
: All nine Planck frequency channels from 30 to 857 GHz, harmonically transformed up to <math>\ell = 4000 </math>.<br />
; Fit<br />
: In practice, the SMICA fit,i.e.,the minimization of Eq. (4), is conducted in three successive steps: We first estimate the CMB spectral law by fitting all model parameters over a clean fraction of sky in the range <math> 100 ≤ \ell ≤ 680</math> and retaining the best fit value for vector <math> \mathbf{a}</math>. In the second step, we estimate the foreground emissivity by fixing a to its value from the previous step and fitting all the other parameters over a large fraction of sky in the range <math> 4 ≤ \ell ≤ 150</math> and retaining the best fit values for the matrix <math> \mathbf{A}</math>. In the last step, we fit all power spectrum parameters; that is, we fix <math>\mathbf{a}</math> and <math>\mathbf{A}</math> to their previously found values and fit for each <math> C_\ell </math> and <math>\mathbf{P}_\ell </math> at each <math>\ell</math>. <br />
;Beams<br />
: The discussion thus far assumes that all input maps have the same resolution and effective beam. Since the observed maps actually vary in resolution, we process the input maps in the following way. To the <math>i</math>-th input map with effective beam <math>b_i(\ell)</math> and sampled on an HEALPix grid with <math>N^i_{side}</math>, the CMB sky multipole <math>s_{\ell m}</math> actually contributes <math>s_{\ell m}a_i b_i(\ell) p_i(\ell)</math>, where <math>p_i(\ell)</math> is the pixel window function for the grid at <math>N^i_{side}</math>. Seeking a final CMB map at 5-arcmin resolution, the highest resolution of Planck, we work with input spherical harmonics re-beamed to 5 arcmins, <math>\mathbf{\tilde{x}}_{\ell m} </math>; that is, SMICA operates on vectors with entries <math>x ̃^i_{\ell m} = x^i_{\ell m} b_5(\ell) / b_i(\ell) / p_i(\ell)</math>, where <math>b_5(\ell)</math> is a 5 arcmin Gaussian beam function. By construction, SMICA then produces an CMB map with an effective Gaussian beam of 5 arcmin (without the pixel window function).<br />
; Pre-processing<br />
: We start by fitting point sources with SNR > 5 in the PCCS catalogue in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole in-painted. This is done at all frequencies but 545 and 857 GHz, where all point sources with SNR > 7.5 are masked and in-painted. <br />
; Masking and in-painting<br />
: In practice, SMICA uses a small Galactic mask leaving 97% of the sky. We deliver a full-sky CMB map in which the masked pixels (Galactic and point-source) are replaced by a constrained Gaussian realization.<br />
; Binning<br />
: In our implementation, we use binned spectra.<br />
; High <math>\ell</math><br />
: Since there is little point trying to model the spectral covariance at high multipoles, because the sample estimate is sufficient, SMICA implements a simple harmonic ILC at <math>\ell > 1500</math>; that is, it applies the filter (Eq. 2) with <math>\mathbf{R}_\ell = \mathbf{\hat{R}}_\ell</math>.<br />
<br />
Viewed as a filter, SMICA can be summarized by the weights <math>\mathbf{w}_\ell</math> applied to each input map as a function of multipole. In this sense, SMICA is strictly equivalent to co-adding the input maps after convolution by specific axi-symmetric kernels directly related to the corresponding entry of <math>\mathbf{w}_\ell</math>. The SMICA weights used here are shown in figure below for input maps in units of K<math>_\rm{RJ}</math>. They show, in particular, the (expected) progressive attenuation of the lowest resolution channels with increasing multipole.<br />
<br />
[[File:smica.jpg|thumb|center|600px|'''Weights <math>w_\ell</math> given by SMICA to the input maps, after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>, as a function of multipole.''']]<br />
<br />
===Commander-Ruler===<br />
<br />
The Commander-Ruler (C-R) approach implements Bayesian component separation in pixel space, fitting a parametric model to the data by sampling the posterior distribution for the model parameters. For computational reasons, the fit is performed in a two-step procedure: First, both foreground amplitudes and spectral parameters are found at low-resolution using MCMC/Gibbs sampling algorithms (Jewell et al. 2004; Wandelt et al. 2004; Eriksen et al. 2004, 2007, 2008). Second, the amplitudes are recalculated at high resolution by solving the generalized least squares system (GLSS) per pixel with the spectral parameters fixed to the their values from the low-resolution run.<br />
For the CMB-oriented analysis presented in this paper, we only use the seven lowest Planck frequencies, i.e., from 30 to 353 GHz. We first downgrade each frequency map from its native angular resolution to a common resolution of 40 arcminutes and re-pixelize at HEALPix N<math>_\rm{side}</math> = 256. Second, we set the monopoles and dipoles for each frequency band using a method that locally conserves spectral indices (Wehus et al. 2013, in preparation). We approximate the effective instrumental noise as white with an RMS per pixel given by the Planck scanning pattern and an amplitude calibrated by smoothing simulations of the instrumental noise including correlations to the same resolution. For the high-resolution analysis, the important pre-processing step is the upgrading of the effective low-resolution mixing matrices to full Planck resolution: this is done by repixelizing from N<math>_\rm{side}</math> = 256 to 2048 in harmonic space, ensuring that potential pixelization effects from the low-resolution map do not introduce sharp boundaries in the high-resolution map.<br />
<br />
<!--<br />
TBW.<br />
--><br />
<br />
== References ==<br />
<br />
<References /><br />
<br />
<br />
<br />
[[Category:HFI/LFI joint data processing|003]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10779CMB and astrophysical component maps2015-01-31T17:41:00Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the COMMANDER, NILC, SEVEM, and SMICA pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Appendices A-D of {{PlanckPapers|planck2014-a11}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_smica_tsig.png | '''smica temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''</gallery><br />
</center><br />
<br />
===Product description ===<br />
<br />
====COMMANDER====<br />
<br />
;Principle<br />
<br />
: COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration, bandpass corrections, monopole and dipoles, are fitted jointly with the astrophysical components. A new feature in the Planck 2015 analysis is that the astrophysical model is derived from a combination of Planck, WMAP and a 408 MHz (Haslam et al. 1982) survey, providing sufficient frequency support to resolve the low-frequency components into synchrotron, free-free and spinning dust. For full details, see {{PlanckPapers|planck2014-a12}}.<br />
<br />
; Resolution (effective beam)<br />
<br />
: The Commander sky maps have different angular resolutions depending on data products:<br />
* The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) have a 1 degree FWHM resolution, and are pixelized at N<sub>side</sub>=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood. <br />
* The Commander CMB temperature map derived from Planck-only observations have an angular resolution of ~5 arcmin and is pixelized at N<sub>side</sub>=2048. This map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-857 GHz data), 7.5 arcmin (using 143-857 GHz data), and 5 arcmin (using 217-857 GHz data) are coadded into a single map.<br />
* The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at N<sub>side</sub>=1024. As for the temperature case, this map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-353 GHz data) and 10 arcmin (using 100-353 GHz data) are coadded into a single map.<br />
<br />
; Confidence mask<br />
<br />
: The Commander confidence masks are produced by thresholding the chi-square map characterizing the global fits, combined with direct CO amplitude thresholding to eliminate known leakage effects. In addition, we exclude the 9-year WMAP point source mask in the temperature mask. For full details, see Sections 5 and 6 in {{PlanckPapers|planck2014-a12}}. A total of 81% of the sky is admitted for high-resolution temperature analysis, and 83% for polarization analysis. For low-resolution temperature analysis, for which the additional WMAP and 408 MHz observations improve foreground constraints, a total of 93% of the sky is admitted. <br />
<br />
====NILC====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:SEVEM produces clean CMB maps at several frequencies by using a procedure based on template fitting in real space. The templates are typically constructed from the lowest and highest Planck frequencies and then subtracted from the CMB-dominated channels, with coefficients that are chosen to minimize the variance of the clean map outside a considered mask. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Two single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
<br />
<br />
====SMICA====<br />
; Principle<br />
: SMICA produces CMBs map by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to <math>\ell = 4000</math>. Temperature and polarization maps are produced independently.<br />
; Resolution (effective beam)<br />
: The SMICA intensity map has an effective beam window function of 5 arc-minutes which is truncated at <math>\ell=4000</math> and is '''not''' deconvolved from the pixel window function. Thus the delivered beam window function is the product of a Gaussian beam at 5 arcminutes and the pixel window function for Nside=2048.<br />
: The SMICA Q and U maps are obtained similarly but are produced at Nside=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.<br />
<br />
===Production process===<br />
<br />
====COMMANDER====<br />
<br />
; Pre-processing<br />
<br />
: All sky maps are first convolved to a common resolution that is larger than the largest beam of any frequency channel. For the combined Planck, WMAP and 408 MHz temperature analysis, the common resolution is 1 degree FWHM; for the Planck-only all-frequency analysis it is 40 arcmin FWHM; and for the intermediate-resolution analysis it is 7.5 arcmin; while for the full-resolution analysis, we assume all frequencies between 217 and 857 GHz have a common resolution, and no additional convolution is performed. For polarization, only two smoothing scales are employed, 40 and 10 arcmin, respectively. The instrumental noise rms maps are convolved correspondingly, properly accouting for their matrix-like nature. <br />
<br />
; Priors<br />
<br />
: The following priors are enforced in the Commander analysis:<br />
* All foreground amplitudes are enforced to be positive definite in the low-resolution analysis, while no amplitude priors are enforced in the high-resolution analyses<br />
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies<br />
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky<br />
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors<br />
<br />
; Fitting procedure<br />
<br />
: Given data and priors, Commander either maximizes, or samples from, the Bayesian posterior, P(theta|data). Because this is a highly non-Gaussian and correlated distribution, involving millions of parameters, these operations are performed by means of the Gibbs sampling algorithm, in which joint samples from the full distributions are generated by iteratively sampling from the corresponding conditional posterior distributions, P(theta_i| data, theta_{j/=i}). For the low-resolution analysis, all parameters are optimized jointly, while in the high-resolution analyses, which employs fewer frequency channels, low signal-to-noise parameters are fixed to those derived at low resolution. Examples of such parameters include monopoles and dipoles, calibration and bandpass parameters, thermal dust temperature etc.<br />
<br />
====NILC====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
The templates used in the SEVEM pipeline are typically constructed by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using a total of four templates. Three of them are constructed as the difference of two consecutive Planck channels smoothed to a common resolution (30-44, 44-70 and 545-353) and the 857 GHz channel is chosen as the fourth template. First of all, the six frequency channels which are going to be part of the templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm. The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz after inpainting.<br />
<br />
The coefficients are obtained by minimising the variance outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the original map. Our final CMB map is then constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by studying the differences between different SEVEM CMB reconstructions, which correspond to maps cleaned at different frequencies or using different analysis masks. The obtained mask leaves a useful sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the $Q$ and $U$ maps independently. However, given that a narrower frequency coverage is available for polarization, the selected templates and maps to be cleaned are different. In particular, we clean the 70, 100 and 143 GHz using three templates for each channel. The first step of the pipeline is to inpaint the positions of the point sources using the MHW, in those channels which are going to be used to construct templates, following the same procedure as for the intensity case. the inpainting is performed in the frequency maps at their native resolution. These inpainted maps are then used to construct a total of four templates. To trace the synchrotron emission, we construct a template as the subtraction of the 30 GHz minus the 44 GHz <br />
map, after being convolved with the beam of each other. For the dust emission, the following templates are considered: 353--217 GHz (smoothed at 10$'$ resolution), 217--143 GHz (used <br />
to clean 70 and 100 GHz) and 217--100 GHz (to clean 143 GHz). These two last templates are constructed at 1 degree resolution since an additional smoothing becomes necessary in<br />
order to increase the signal-to-noise ratio of the template. Conversely to the <br />
intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates. In this way, the 100 GHz <br />
map is used to clean the 143 GHz frequency channel and viceversa, making the clean maps less independent between them than in the intensity case.<br />
<br />
These templates are then used to clean the non-inpainted 70 (at its native resolution), 100 (at 10$'$ resolution) and 143 GHz maps (also at 10$'$). The corresponding linear coefficients are estimated independently for $Q$ and $U$ by minimising the variance of the clean maps outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at the corresponding raw maps is carried out. The size of the holes to be inpainted takes<br />
into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using $E$ and $B$ decomposition, to produce the final CMB maps for the $Q$ and $U$ components at a resolution of 10$'$ (Gaussian beam) for a HEALPix parameter Nside=1024. Each map is weighted taking into account its <br />
corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky) to avoid the introduction of ringing around the Galactic centre in the filtering process.<br />
<br />
The confidence mask includes all the pixels above a given threshold in a smoothed version of the clean CMB map, the regions more contaminated by the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction of approximately 80 per cent.<br />
<br />
<br />
<br />
====SMICA====<br />
<br />
A) Production of the intensity map.<br />
<br />
; 1) Pre-processing<br />
: Before computing spherical harmonic coefficients, all input maps undergo a pre-processing step to deal with regions of very strong emission (such as the Galactic center) and point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. The diffusive inpainting process is also applied to some regions of very strong emissions. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHz are harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: A confidence mask is determined (see the Planck paper) and all regions which have been masked in the pre-processing step are added to it.<br />
<br />
<br />
<br />
<!--[[File:Smica_filter_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input intensity maps (after they are re-beamed to 5 arc-minutes and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]--><br />
<br />
B) Production of the Q and U polarisation maps.<br />
<br />
The production of the Q and U maps is similar to the production of the intensity map. The SMICA pipeline uses all the 7 polarized Planck channels. After point source masking and diffusive inpainting, the E and B modes are computed and combined to produce E and B modes of the CMB map. Those combined modes are then used to synthesize the U and Q CMB maps. The E and B parts of the input frequency maps being processed jointly, there are, at each multipole, 2*7=14 coefficients (weights) defined to produce the E modes of the CMB map and as many to produce the B part. The weights are displayed in the figure below. The Q and U maps were originally produced at Nside=2048 with a 5-arc-minute resolution, but were downgraded to Nside=1024 with a 10 arc-minute resolution for this release.<br />
<br />
<br />
<!--[[File:Smica_filterEB_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input E and B modes (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), in order to produce the E and B modes of the CMB map. A given frequency channel is encoded in a given color. Solid lines are for E modes and dashed lines are for B modes. The thick lines are for the EE or BB weights; the thin lines are for the EB or BE weights. See the paper for more details.''']]--><br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}.<br />
<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353, 545, 857 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=545|period=Nominal|zodi=uncorr|link=HFI 545 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=857|period=Nominal|zodi=uncorr|link=HFI 857 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
<br />
===Low-resolution temperature products===<br />
<br />
: The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors. The full set of data products derived from the low-resolution joint analysis are the following:<br />
<br />
=====Synchrotron emission=====<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px> <br />
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''<br />
</gallery><br />
</center><br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}<br />
: Reference frequency: 408 MHz<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-Synchrotron<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|}<br />
<br />
<br />
<br />
; Free-free emission<br />
: (Coming soon!)<br />
<br />
; Spinning dust emission<br />
: (Coming soon!)<br />
<br />
; CO line emission<br />
: (Coming soon!)<br />
<br />
; 94/100 GHz line emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
; Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters<br />
: (Coming soon!)<br />
<br />
===High-resolution temperature products===<br />
<br />
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz. These data products include the following:<br />
<br />
; CO(2-1) emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10778CMB and astrophysical component maps2015-01-31T17:39:15Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the COMMANDER, NILC, SEVEM, and SMICA pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Appendices A-D of {{PlanckPapers|planck2014-a11}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_smica_tsig.png | '''smica temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''</gallery><br />
</center><br />
<br />
===Product description ===<br />
<br />
====COMMANDER====<br />
<br />
;Principle<br />
<br />
: COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration, bandpass corrections, monopole and dipoles, are fitted jointly with the astrophysical components. A new feature in the Planck 2015 analysis is that the astrophysical model is derived from a combination of Planck, WMAP and a 408 MHz (Haslam et al. 1982) survey, providing sufficient frequency support to resolve the low-frequency components into synchrotron, free-free and spinning dust. For full details, see {{PlanckPapers|planck2014-a12}}.<br />
<br />
; Resolution (effective beam)<br />
<br />
: The Commander sky maps have different angular resolutions depending on data products:<br />
* The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) have a 1 degree FWHM resolution, and are pixelized at N<sub>side</sub>=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood. <br />
* The Commander CMB temperature map derived from Planck-only observations have an angular resolution of ~5 arcmin and is pixelized at N<sub>side</sub>=2048. This map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-857 GHz data), 7.5 arcmin (using 143-857 GHz data), and 5 arcmin (using 217-857 GHz data) are coadded into a single map.<br />
* The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at N<sub>side</sub>=1024. As for the temperature case, this map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-353 GHz data) and 10 arcmin (using 100-353 GHz data) are coadded into a single map.<br />
<br />
; Confidence mask<br />
<br />
: The Commander confidence masks are produced by thresholding the chi-square map characterizing the global fits, combined with direct CO amplitude thresholding to eliminate known leakage effects. In addition, we exclude the 9-year WMAP point source mask in the temperature mask. For full details, see Sections 5 and 6 in {{PlanckPapers|planck2014-a12}}. A total of 81% of the sky is admitted for high-resolution temperature analysis, and 83% for polarization analysis. For low-resolution temperature analysis, for which the additional WMAP and 408 MHz observations improve foreground constraints, a total of 93% of the sky is admitted. <br />
<br />
====NILC====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:SEVEM produces clean CMB maps at several frequencies by using a procedure based on template fitting in real space. The templates are typically constructed from the lowest and highest Planck frequencies and then subtracted from the CMB-dominated channels, with coefficients that are chosen to minimize the variance of the clean map outside a considered mask. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Two single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
<br />
<br />
====SMICA====<br />
; Principle<br />
: SMICA produces CMBs map by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to <math>\ell = 4000</math>. Temperature and polarization maps are produced independently.<br />
; Resolution (effective beam)<br />
: The SMICA intensity map has an effective beam window function of 5 arc-minutes which is truncated at <math>\ell=4000</math> and is '''not''' deconvolved from the pixel window function. Thus the delivered beam window function is the product of a Gaussian beam at 5 arcminutes and the pixel window function for Nside=2048.<br />
: The SMICA Q and U maps are obtained similarly but are produced at Nside=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.<br />
<br />
===Production process===<br />
<br />
====COMMANDER====<br />
<br />
; Pre-processing<br />
<br />
: All sky maps are first convolved to a common resolution that is larger than the largest beam of any frequency channel. For the combined Planck, WMAP and 408 MHz temperature analysis, the common resolution is 1 degree FWHM; for the Planck-only all-frequency analysis it is 40 arcmin FWHM; and for the intermediate-resolution analysis it is 7.5 arcmin; while for the full-resolution analysis, we assume all frequencies between 217 and 857 GHz have a common resolution, and no additional convolution is performed. For polarization, only two smoothing scales are employed, 40 and 10 arcmin, respectively. The instrumental noise rms maps are convolved correspondingly, properly accouting for their matrix-like nature. <br />
<br />
; Priors<br />
<br />
: The following priors are enforced in the Commander analysis:<br />
* All foreground amplitudes are enforced to be positive definite in the low-resolution analysis, while no amplitude priors are enforced in the high-resolution analyses<br />
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies<br />
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky<br />
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors<br />
<br />
; Fitting procedure<br />
<br />
: Given data and priors, Commander either maximizes, or samples from, the Bayesian posterior, P(theta|data). Because this is a highly non-Gaussian and correlated distribution, involving millions of parameters, these operations are performed by means of the Gibbs sampling algorithm, in which joint samples from the full distributions are generated by iteratively sampling from the corresponding conditional posterior distributions, P(theta_i| data, theta_{j/=i}). For the low-resolution analysis, all parameters are optimized jointly, while in the high-resolution analyses, which employs fewer frequency channels, low signal-to-noise parameters are fixed to those derived at low resolution. Examples of such parameters include monopoles and dipoles, calibration and bandpass parameters, thermal dust temperature etc.<br />
<br />
====NILC====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
The templates used in the SEVEM pipeline are typically constructed by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. <br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using a total of four templates. Three of them are constructed as the difference of two consecutive Planck channels smoothed to a common resolution (30-44, 44-70 and 545-353) and the 857 GHz channel is chosen as the fourth template. First of all, the six frequency channels which are going to be part of the templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm. The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz after inpainting.<br />
<br />
The coefficients are obtained by minimising the variance outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the original map. Our final CMB map is then constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by studying the differences between different SEVEM CMB reconstructions, which correspond to maps cleaned at different frequencies or using different analysis masks. The obtained mask leaves a useful sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the $Q$ and $U$ maps independently. However, given that a narrower frequency coverage is available for polarization, the selected templates and maps to be cleaned are different. In particular, we clean the 70, 100 and 143 GHz using three templates for each channel. <br />
<br />
The first step of the pipeline is to inpaint the positions of the point sources using the MHW, in those channels which are going to be used to construct templates, following the same procedure as for the intensity case. the inpainting is performed in the frequency maps at their native resolution.<br />
<br />
These inpainted maps are then used to construct a total of four templates. To trace the synchrotron emission, we construct a template as the subtraction of the 30 GHz minus the 44 GHz <br />
map, after being convolved with the beam of each other. For the dust emission, the following templates are considered: 353--217 GHz (smoothed at 10$'$ resolution), 217--143 GHz (used <br />
to clean 70 and 100 GHz) and 217--100 GHz (to clean 143 GHz). These two last templates are constructed at 1 degree resolution since an additional smoothing becomes necessary in<br />
order to increase the signal-to-noise ratio of the template. Conversely to the <br />
intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates. In this way, the 100 GHz <br />
map is used to clean the 143 GHz frequency channel and viceversa, making the clean maps less independent between them than in the intensity case.<br />
<br />
These templates are then used to clean the non-inpainted 70 (at its native resolution), 100 (at 10$'$ resolution) and 143 GHz maps (also at 10$'$). The corresponding linear coefficients are estimated independently for $Q$ and $U$ by minimising the variance of the clean maps outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at the corresponding raw maps is carried out. The size of the holes to be inpainted takes<br />
into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using $E$ and $B$ decomposition, to produce the final CMB maps for the $Q$ and $U$ components at a resolution of 10$'$ (Gaussian beam) for a HEALPix parameter Nside=1024. Each map is weighted taking into account its <br />
corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky) to avoid the introduction of ringing around the Galactic centre in the filtering process.<br />
<br />
The confidence mask includes all the pixels above a given threshold in a smoothed version of the clean CMB map, the regions more contaminated by the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction of approximately 80 per cent.<br />
<br />
<br />
<br />
====SMICA====<br />
<br />
A) Production of the intensity map.<br />
<br />
; 1) Pre-processing<br />
: Before computing spherical harmonic coefficients, all input maps undergo a pre-processing step to deal with regions of very strong emission (such as the Galactic center) and point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. The diffusive inpainting process is also applied to some regions of very strong emissions. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHz are harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: A confidence mask is determined (see the Planck paper) and all regions which have been masked in the pre-processing step are added to it.<br />
<br />
<br />
<br />
<!--[[File:Smica_filter_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input intensity maps (after they are re-beamed to 5 arc-minutes and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]--><br />
<br />
B) Production of the Q and U polarisation maps.<br />
<br />
The production of the Q and U maps is similar to the production of the intensity map. The SMICA pipeline uses all the 7 polarized Planck channels. After point source masking and diffusive inpainting, the E and B modes are computed and combined to produce E and B modes of the CMB map. Those combined modes are then used to synthesize the U and Q CMB maps. The E and B parts of the input frequency maps being processed jointly, there are, at each multipole, 2*7=14 coefficients (weights) defined to produce the E modes of the CMB map and as many to produce the B part. The weights are displayed in the figure below. The Q and U maps were originally produced at Nside=2048 with a 5-arc-minute resolution, but were downgraded to Nside=1024 with a 10 arc-minute resolution for this release.<br />
<br />
<br />
<!--[[File:Smica_filterEB_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input E and B modes (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), in order to produce the E and B modes of the CMB map. A given frequency channel is encoded in a given color. Solid lines are for E modes and dashed lines are for B modes. The thick lines are for the EE or BB weights; the thin lines are for the EB or BE weights. See the paper for more details.''']]--><br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}.<br />
<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353, 545, 857 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=545|period=Nominal|zodi=uncorr|link=HFI 545 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=857|period=Nominal|zodi=uncorr|link=HFI 857 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
<br />
===Low-resolution temperature products===<br />
<br />
: The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors. The full set of data products derived from the low-resolution joint analysis are the following:<br />
<br />
=====Synchrotron emission=====<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px> <br />
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''<br />
</gallery><br />
</center><br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}<br />
: Reference frequency: 408 MHz<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-Synchrotron<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|}<br />
<br />
<br />
<br />
; Free-free emission<br />
: (Coming soon!)<br />
<br />
; Spinning dust emission<br />
: (Coming soon!)<br />
<br />
; CO line emission<br />
: (Coming soon!)<br />
<br />
; 94/100 GHz line emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
; Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters<br />
: (Coming soon!)<br />
<br />
===High-resolution temperature products===<br />
<br />
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz. These data products include the following:<br />
<br />
; CO(2-1) emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10777CMB and astrophysical component maps2015-01-31T17:19:00Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the COMMANDER, NILC, SEVEM, and SMICA pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Appendices A-D of {{PlanckPapers|planck2014-a11}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_smica_tsig.png | '''smica temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''</gallery><br />
</center><br />
<br />
===Product description ===<br />
<br />
====COMMANDER====<br />
<br />
;Principle<br />
<br />
: COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration, bandpass corrections, monopole and dipoles, are fitted jointly with the astrophysical components. A new feature in the Planck 2015 analysis is that the astrophysical model is derived from a combination of Planck, WMAP and a 408 MHz (Haslam et al. 1982) survey, providing sufficient frequency support to resolve the low-frequency components into synchrotron, free-free and spinning dust. For full details, see {{PlanckPapers|planck2014-a12}}.<br />
<br />
; Resolution (effective beam)<br />
<br />
: The Commander sky maps have different angular resolutions depending on data products:<br />
* The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) have a 1 degree FWHM resolution, and are pixelized at N<sub>side</sub>=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood. <br />
* The Commander CMB temperature map derived from Planck-only observations have an angular resolution of ~5 arcmin and is pixelized at N<sub>side</sub>=2048. This map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-857 GHz data), 7.5 arcmin (using 143-857 GHz data), and 5 arcmin (using 217-857 GHz data) are coadded into a single map.<br />
* The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at N<sub>side</sub>=1024. As for the temperature case, this map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-353 GHz data) and 10 arcmin (using 100-353 GHz data) are coadded into a single map.<br />
<br />
; Confidence mask<br />
<br />
: The Commander confidence masks are produced by thresholding the chi-square map characterizing the global fits, combined with direct CO amplitude thresholding to eliminate known leakage effects. In addition, we exclude the 9-year WMAP point source mask in the temperature mask. For full details, see Sections 5 and 6 in {{PlanckPapers|planck2014-a12}}. A total of 81% of the sky is admitted for high-resolution temperature analysis, and 83% for polarization analysis. For low-resolution temperature analysis, for which the additional WMAP and 408 MHz observations improve foreground constraints, a total of 93% of the sky is admitted. <br />
<br />
====NILC====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:SEVEM produces clean CMB maps at several frequencies by using a procedure based on template fitting in real space. The templates are typically constructed from the lowest and highest Planck frequencies and then subtracted from the CMB-dominated channels, with coefficients that are chosen to minimize the variance of the clean map outside a considered mask. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Two single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
<br />
<br />
====SMICA====<br />
; Principle<br />
: SMICA produces CMBs map by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to <math>\ell = 4000</math>. Temperature and polarization maps are produced independently.<br />
; Resolution (effective beam)<br />
: The SMICA intensity map has an effective beam window function of 5 arc-minutes which is truncated at <math>\ell=4000</math> and is '''not''' deconvolved from the pixel window function. Thus the delivered beam window function is the product of a Gaussian beam at 5 arcminutes and the pixel window function for Nside=2048.<br />
: The SMICA Q and U maps are obtained similarly but are produced at Nside=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.<br />
<br />
===Production process===<br />
<br />
====COMMANDER====<br />
<br />
; Pre-processing<br />
<br />
: All sky maps are first convolved to a common resolution that is larger than the largest beam of any frequency channel. For the combined Planck, WMAP and 408 MHz temperature analysis, the common resolution is 1 degree FWHM; for the Planck-only all-frequency analysis it is 40 arcmin FWHM; and for the intermediate-resolution analysis it is 7.5 arcmin; while for the full-resolution analysis, we assume all frequencies between 217 and 857 GHz have a common resolution, and no additional convolution is performed. For polarization, only two smoothing scales are employed, 40 and 10 arcmin, respectively. The instrumental noise rms maps are convolved correspondingly, properly accouting for their matrix-like nature. <br />
<br />
; Priors<br />
<br />
: The following priors are enforced in the Commander analysis:<br />
* All foreground amplitudes are enforced to be positive definite in the low-resolution analysis, while no amplitude priors are enforced in the high-resolution analyses<br />
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies<br />
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky<br />
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors<br />
<br />
; Fitting procedure<br />
<br />
: Given data and priors, Commander either maximizes, or samples from, the Bayesian posterior, P(theta|data). Because this is a highly non-Gaussian and correlated distribution, involving millions of parameters, these operations are performed by means of the Gibbs sampling algorithm, in which joint samples from the full distributions are generated by iteratively sampling from the corresponding conditional posterior distributions, P(theta_i| data, theta_{j/=i}). For the low-resolution analysis, all parameters are optimized jointly, while in the high-resolution analyses, which employs fewer frequency channels, low signal-to-noise parameters are fixed to those derived at low resolution. Examples of such parameters include monopoles and dipoles, calibration and bandpass parameters, thermal dust temperature etc.<br />
<br />
====NILC====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
The templates used in the SEVEM pipeline are typically constructed by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. <br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using a total of four templates. Three of them are constructed as the difference of two consecutive Planck channels smoothed to a common resolution (30-44, 44-70 and 545-353) and the 857 GHz channel is chosen as the fourth template. First of all, the six frequency channels which are going to part of the templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz after inpainting.<br />
<br />
The coefficients are obtained by minimising the variance outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the original map. Our final CMB map is then constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by studying the differences between different SEVEM CMB reconstructions, which correspond to maps cleaned at different frequencies or using different analysis masks. The obtained mask leaves a useful sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
<br />
<br />
====SMICA====<br />
<br />
A) Production of the intensity map.<br />
<br />
; 1) Pre-processing<br />
: Before computing spherical harmonic coefficients, all input maps undergo a pre-processing step to deal with regions of very strong emission (such as the Galactic center) and point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. The diffusive inpainting process is also applied to some regions of very strong emissions. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHz are harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: A confidence mask is determined (see the Planck paper) and all regions which have been masked in the pre-processing step are added to it.<br />
<br />
<br />
<br />
<!--[[File:Smica_filter_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input intensity maps (after they are re-beamed to 5 arc-minutes and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]--><br />
<br />
B) Production of the Q and U polarisation maps.<br />
<br />
The production of the Q and U maps is similar to the production of the intensity map. The SMICA pipeline uses all the 7 polarized Planck channels. After point source masking and diffusive inpainting, the E and B modes are computed and combined to produce E and B modes of the CMB map. Those combined modes are then used to synthesize the U and Q CMB maps. The E and B parts of the input frequency maps being processed jointly, there are, at each multipole, 2*7=14 coefficients (weights) defined to produce the E modes of the CMB map and as many to produce the B part. The weights are displayed in the figure below. The Q and U maps were originally produced at Nside=2048 with a 5-arc-minute resolution, but were downgraded to Nside=1024 with a 10 arc-minute resolution for this release.<br />
<br />
<br />
<!--[[File:Smica_filterEB_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input E and B modes (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), in order to produce the E and B modes of the CMB map. A given frequency channel is encoded in a given color. Solid lines are for E modes and dashed lines are for B modes. The thick lines are for the EE or BB weights; the thin lines are for the EB or BE weights. See the paper for more details.''']]--><br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}.<br />
<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353, 545, 857 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=545|period=Nominal|zodi=uncorr|link=HFI 545 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=857|period=Nominal|zodi=uncorr|link=HFI 857 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
<br />
===Low-resolution temperature products===<br />
<br />
: The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors. The full set of data products derived from the low-resolution joint analysis are the following:<br />
<br />
=====Synchrotron emission=====<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px> <br />
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''<br />
</gallery><br />
</center><br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}<br />
: Reference frequency: 408 MHz<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-Synchrotron<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|}<br />
<br />
<br />
<br />
; Free-free emission<br />
: (Coming soon!)<br />
<br />
; Spinning dust emission<br />
: (Coming soon!)<br />
<br />
; CO line emission<br />
: (Coming soon!)<br />
<br />
; 94/100 GHz line emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
; Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters<br />
: (Coming soon!)<br />
<br />
===High-resolution temperature products===<br />
<br />
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz. These data products include the following:<br />
<br />
; CO(2-1) emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10776CMB and astrophysical component maps2015-01-31T16:52:20Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the COMMANDER, NILC, SEVEM, and SMICA pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Appendices A-D of {{PlanckPapers|planck2014-a11}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_smica_tsig.png | '''smica temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''</gallery><br />
</center><br />
<br />
===Product description ===<br />
<br />
====COMMANDER====<br />
<br />
;Principle<br />
<br />
: COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration, bandpass corrections, monopole and dipoles, are fitted jointly with the astrophysical components. A new feature in the Planck 2015 analysis is that the astrophysical model is derived from a combination of Planck, WMAP and a 408 MHz (Haslam et al. 1982) survey, providing sufficient frequency support to resolve the low-frequency components into synchrotron, free-free and spinning dust. For full details, see {{PlanckPapers|planck2014-a12}}.<br />
<br />
; Resolution (effective beam)<br />
<br />
: The Commander sky maps have different angular resolutions depending on data products:<br />
* The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) have a 1 degree FWHM resolution, and are pixelized at N<sub>side</sub>=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood. <br />
* The Commander CMB temperature map derived from Planck-only observations have an angular resolution of ~5 arcmin and is pixelized at N<sub>side</sub>=2048. This map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-857 GHz data), 7.5 arcmin (using 143-857 GHz data), and 5 arcmin (using 217-857 GHz data) are coadded into a single map.<br />
* The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at N<sub>side</sub>=1024. As for the temperature case, this map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-353 GHz data) and 10 arcmin (using 100-353 GHz data) are coadded into a single map.<br />
<br />
; Confidence mask<br />
<br />
: The Commander confidence masks are produced by thresholding the chi-square map characterizing the global fits, combined with direct CO amplitude thresholding to eliminate known leakage effects. In addition, we exclude the 9-year WMAP point source mask in the temperature mask. For full details, see Sections 5 and 6 in {{PlanckPapers|planck2014-a12}}. A total of 81% of the sky is admitted for high-resolution temperature analysis, and 83% for polarization analysis. For low-resolution temperature analysis, for which the additional WMAP and 408 MHz observations improve foreground constraints, a total of 93% of the sky is admitted. <br />
<br />
====NILC====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:SEVEM produces clean CMB maps at several frequencies by using a procedure based on template fitting in real space. The templates are typically constructed from the lowest and highest Planck frequencies and then subtracted from the CMB-dominated channels, with coefficients that are chosen to minimize the variance of the clean map outside a considered mask. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Two single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
<br />
<br />
====SMICA====<br />
; Principle<br />
: SMICA produces CMBs map by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to <math>\ell = 4000</math>. Temperature and polarization maps are produced independently.<br />
; Resolution (effective beam)<br />
: The SMICA intensity map has an effective beam window function of 5 arc-minutes which is truncated at <math>\ell=4000</math> and is '''not''' deconvolved from the pixel window function. Thus the delivered beam window function is the product of a Gaussian beam at 5 arcminutes and the pixel window function for Nside=2048.<br />
: The SMICA Q and U maps are obtained similarly but are produced at Nside=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.<br />
<br />
===Production process===<br />
<br />
====COMMANDER====<br />
<br />
; Pre-processing<br />
<br />
: All sky maps are first convolved to a common resolution that is larger than the largest beam of any frequency channel. For the combined Planck, WMAP and 408 MHz temperature analysis, the common resolution is 1 degree FWHM; for the Planck-only all-frequency analysis it is 40 arcmin FWHM; and for the intermediate-resolution analysis it is 7.5 arcmin; while for the full-resolution analysis, we assume all frequencies between 217 and 857 GHz have a common resolution, and no additional convolution is performed. For polarization, only two smoothing scales are employed, 40 and 10 arcmin, respectively. The instrumental noise rms maps are convolved correspondingly, properly accouting for their matrix-like nature. <br />
<br />
; Priors<br />
<br />
: The following priors are enforced in the Commander analysis:<br />
* All foreground amplitudes are enforced to be positive definite in the low-resolution analysis, while no amplitude priors are enforced in the high-resolution analyses<br />
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies<br />
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky<br />
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors<br />
<br />
; Fitting procedure<br />
<br />
: Given data and priors, Commander either maximizes, or samples from, the Bayesian posterior, P(theta|data). Because this is a highly non-Gaussian and correlated distribution, involving millions of parameters, these operations are performed by means of the Gibbs sampling algorithm, in which joint samples from the full distributions are generated by iteratively sampling from the corresponding conditional posterior distributions, P(theta_i| data, theta_{j/=i}). For the low-resolution analysis, all parameters are optimized jointly, while in the high-resolution analyses, which employs fewer frequency channels, low signal-to-noise parameters are fixed to those derived at low resolution. Examples of such parameters include monopoles and dipoles, calibration and bandpass parameters, thermal dust temperature etc.<br />
<br />
====NILC====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
The first step in the SEVEM pipeline is to produce the required templates. They are usually <br />
constructed by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. <br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using a total of four templates. Three of them are constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
<br />
<br />
====SMICA====<br />
<br />
A) Production of the intensity map.<br />
<br />
; 1) Pre-processing<br />
: Before computing spherical harmonic coefficients, all input maps undergo a pre-processing step to deal with regions of very strong emission (such as the Galactic center) and point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. The diffusive inpainting process is also applied to some regions of very strong emissions. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHz are harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: A confidence mask is determined (see the Planck paper) and all regions which have been masked in the pre-processing step are added to it.<br />
<br />
<br />
<br />
<!--[[File:Smica_filter_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input intensity maps (after they are re-beamed to 5 arc-minutes and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]--><br />
<br />
B) Production of the Q and U polarisation maps.<br />
<br />
The production of the Q and U maps is similar to the production of the intensity map. The SMICA pipeline uses all the 7 polarized Planck channels. After point source masking and diffusive inpainting, the E and B modes are computed and combined to produce E and B modes of the CMB map. Those combined modes are then used to synthesize the U and Q CMB maps. The E and B parts of the input frequency maps being processed jointly, there are, at each multipole, 2*7=14 coefficients (weights) defined to produce the E modes of the CMB map and as many to produce the B part. The weights are displayed in the figure below. The Q and U maps were originally produced at Nside=2048 with a 5-arc-minute resolution, but were downgraded to Nside=1024 with a 10 arc-minute resolution for this release.<br />
<br />
<br />
<!--[[File:Smica_filterEB_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input E and B modes (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), in order to produce the E and B modes of the CMB map. A given frequency channel is encoded in a given color. Solid lines are for E modes and dashed lines are for B modes. The thick lines are for the EE or BB weights; the thin lines are for the EB or BE weights. See the paper for more details.''']]--><br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}.<br />
<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353, 545, 857 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=545|period=Nominal|zodi=uncorr|link=HFI 545 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=857|period=Nominal|zodi=uncorr|link=HFI 857 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
<br />
===Low-resolution temperature products===<br />
<br />
: The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors. The full set of data products derived from the low-resolution joint analysis are the following:<br />
<br />
=====Synchrotron emission=====<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px> <br />
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''<br />
</gallery><br />
</center><br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}<br />
: Reference frequency: 408 MHz<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-Synchrotron<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|}<br />
<br />
<br />
<br />
; Free-free emission<br />
: (Coming soon!)<br />
<br />
; Spinning dust emission<br />
: (Coming soon!)<br />
<br />
; CO line emission<br />
: (Coming soon!)<br />
<br />
; 94/100 GHz line emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
; Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters<br />
: (Coming soon!)<br />
<br />
===High-resolution temperature products===<br />
<br />
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz. These data products include the following:<br />
<br />
; CO(2-1) emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10775CMB and astrophysical component maps2015-01-31T16:46:46Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the COMMANDER, NILC, SEVEM, and SMICA pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Appendices A-D of {{PlanckPapers|planck2014-a11}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_smica_tsig.png | '''smica temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''</gallery><br />
</center><br />
<br />
===Product description ===<br />
<br />
====COMMANDER====<br />
<br />
;Principle<br />
<br />
: COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration, bandpass corrections, monopole and dipoles, are fitted jointly with the astrophysical components. A new feature in the Planck 2015 analysis is that the astrophysical model is derived from a combination of Planck, WMAP and a 408 MHz (Haslam et al. 1982) survey, providing sufficient frequency support to resolve the low-frequency components into synchrotron, free-free and spinning dust. For full details, see {{PlanckPapers|planck2014-a12}}.<br />
<br />
; Resolution (effective beam)<br />
<br />
: The Commander sky maps have different angular resolutions depending on data products:<br />
* The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) have a 1 degree FWHM resolution, and are pixelized at N<sub>side</sub>=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood. <br />
* The Commander CMB temperature map derived from Planck-only observations have an angular resolution of ~5 arcmin and is pixelized at N<sub>side</sub>=2048. This map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-857 GHz data), 7.5 arcmin (using 143-857 GHz data), and 5 arcmin (using 217-857 GHz data) are coadded into a single map.<br />
* The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at N<sub>side</sub>=1024. As for the temperature case, this map is produced by harmonic space hybridiziation, in which independent solutions derived at 40 arcmin (using 30-353 GHz data) and 10 arcmin (using 100-353 GHz data) are coadded into a single map.<br />
<br />
; Confidence mask<br />
<br />
: The Commander confidence masks are produced by thresholding the chi-square map characterizing the global fits, combined with direct CO amplitude thresholding to eliminate known leakage effects. In addition, we exclude the 9-year WMAP point source mask in the temperature mask. For full details, see Sections 5 and 6 in {{PlanckPapers|planck2014-a12}}. A total of 81% of the sky is admitted for high-resolution temperature analysis, and 83% for polarization analysis. For low-resolution temperature analysis, for which the additional WMAP and 408 MHz observations improve foreground constraints, a total of 93% of the sky is admitted. <br />
<br />
====NILC====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:SEVEM produces clean CMB maps at several frequencies by using a procedure based on template fitting in real space. The templates are typically constructed from the lowest and highest Planck frequencies and then subtracted from the CMB-dominated channels, with coefficients that are chosen to minimize the variance of the clean map outside a considered mask. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Two single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
<br />
<br />
====SMICA====<br />
; Principle<br />
: SMICA produces CMBs map by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to <math>\ell = 4000</math>. Temperature and polarization maps are produced independently.<br />
; Resolution (effective beam)<br />
: The SMICA intensity map has an effective beam window function of 5 arc-minutes which is truncated at <math>\ell=4000</math> and is '''not''' deconvolved from the pixel window function. Thus the delivered beam window function is the product of a Gaussian beam at 5 arcminutes and the pixel window function for Nside=2048.<br />
: The SMICA Q and U maps are obtained similarly but are produced at Nside=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.<br />
<br />
===Production process===<br />
<br />
====COMMANDER====<br />
<br />
; Pre-processing<br />
<br />
: All sky maps are first convolved to a common resolution that is larger than the largest beam of any frequency channel. For the combined Planck, WMAP and 408 MHz temperature analysis, the common resolution is 1 degree FWHM; for the Planck-only all-frequency analysis it is 40 arcmin FWHM; and for the intermediate-resolution analysis it is 7.5 arcmin; while for the full-resolution analysis, we assume all frequencies between 217 and 857 GHz have a common resolution, and no additional convolution is performed. For polarization, only two smoothing scales are employed, 40 and 10 arcmin, respectively. The instrumental noise rms maps are convolved correspondingly, properly accouting for their matrix-like nature. <br />
<br />
; Priors<br />
<br />
: The following priors are enforced in the Commander analysis:<br />
* All foreground amplitudes are enforced to be positive definite in the low-resolution analysis, while no amplitude priors are enforced in the high-resolution analyses<br />
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies<br />
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky<br />
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors<br />
<br />
; Fitting procedure<br />
<br />
: Given data and priors, Commander either maximizes, or samples from, the Bayesian posterior, P(theta|data). Because this is a highly non-Gaussian and correlated distribution, involving millions of parameters, these operations are performed by means of the Gibbs sampling algorithm, in which joint samples from the full distributions are generated by iteratively sampling from the corresponding conditional posterior distributions, P(theta_i| data, theta_{j/=i}). For the low-resolution analysis, all parameters are optimized jointly, while in the high-resolution analyses, which employs fewer frequency channels, low signal-to-noise parameters are fixed to those derived at low resolution. Examples of such parameters include monopoles and dipoles, calibration and bandpass parameters, thermal dust temperature etc.<br />
<br />
====NILC====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
<br />
<br />
====SMICA====<br />
<br />
A) Production of the intensity map.<br />
<br />
; 1) Pre-processing<br />
: Before computing spherical harmonic coefficients, all input maps undergo a pre-processing step to deal with regions of very strong emission (such as the Galactic center) and point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. The diffusive inpainting process is also applied to some regions of very strong emissions. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHz are harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: A confidence mask is determined (see the Planck paper) and all regions which have been masked in the pre-processing step are added to it.<br />
<br />
<br />
<br />
<!--[[File:Smica_filter_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input intensity maps (after they are re-beamed to 5 arc-minutes and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]--><br />
<br />
B) Production of the Q and U polarisation maps.<br />
<br />
The production of the Q and U maps is similar to the production of the intensity map. The SMICA pipeline uses all the 7 polarized Planck channels. After point source masking and diffusive inpainting, the E and B modes are computed and combined to produce E and B modes of the CMB map. Those combined modes are then used to synthesize the U and Q CMB maps. The E and B parts of the input frequency maps being processed jointly, there are, at each multipole, 2*7=14 coefficients (weights) defined to produce the E modes of the CMB map and as many to produce the B part. The weights are displayed in the figure below. The Q and U maps were originally produced at Nside=2048 with a 5-arc-minute resolution, but were downgraded to Nside=1024 with a 10 arc-minute resolution for this release.<br />
<br />
<br />
<!--[[File:Smica_filterEB_dx11.png|thumb|center|600px|'''Weights given by SMICA to the input E and B modes (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), in order to produce the E and B modes of the CMB map. A given frequency channel is encoded in a given color. Solid lines are for E modes and dashed lines are for B modes. The thick lines are for the EE or BB weights; the thin lines are for the EB or BE weights. See the paper for more details.''']]--><br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}.<br />
<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353, 545, 857 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=545|period=Nominal|zodi=uncorr|link=HFI 545 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=857|period=Nominal|zodi=uncorr|link=HFI 857 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
<br />
===Low-resolution temperature products===<br />
<br />
: The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors. The full set of data products derived from the low-resolution joint analysis are the following:<br />
<br />
=====Synchrotron emission=====<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px> <br />
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''<br />
</gallery><br />
</center><br />
<br />
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}<br />
: Reference frequency: 408 MHz<br />
: Nside = 256<br />
: Angular resolution = 60 arcmin<br />
<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ HDU -- COMP-MAP-Synchrotron<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum <br />
|-<br />
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean <br />
|-<br />
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms<br />
|}<br />
<br />
<br />
<br />
; Free-free emission<br />
: (Coming soon!)<br />
<br />
; Spinning dust emission<br />
: (Coming soon!)<br />
<br />
; CO line emission<br />
: (Coming soon!)<br />
<br />
; 94/100 GHz line emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
; Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters<br />
: (Coming soon!)<br />
<br />
===High-resolution temperature products===<br />
<br />
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz. These data products include the following:<br />
<br />
; CO(2-1) emission<br />
: (Coming soon!)<br />
<br />
; Thermal dust emission<br />
: (Coming soon!)<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10667CMB and astrophysical component maps2015-01-29T17:53:36Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png | '''simca temperature'''<br />
File:CMB_smica_tnoi.png | '''smica noise'''<br />
File:CMB_smica_tmask.png | '''smica mask'''<br />
File:CMB_sevem_tsig.png | '''sevem temperature'''<br />
File:CMB_sevem_tnoi.png | '''sevem noise'''<br />
File:CMB_sevem_tmask.png | '''sevem mask'''<br />
File:CMB_nilc_tsig.png | '''nilc temperature'''<br />
File:CMB_nilc_tnoi.png | '''nilc noise'''<br />
File:CMB_nilc_tmask.png | '''nilc mask'''<br />
File:CMB_commander_tsig.png | '''commander temperature'''<br />
File:CMB_commander_tnoi.png | '''commander noise'''<br />
File:CMB_commander_tmask.png | '''commander mask'''<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting in real space. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing).<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10640CMB and astrophysical component maps2015-01-29T16:12:21Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files <br />
* ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. <br />
The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting in real space. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The single frequency clean maps are then combined to obtain the final CMB map.<br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is constructed up to a maximum <math>\ell=4000</math> at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).<br />
:For polarization the clean CMB map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum <math>\ell=3071</math>.<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing).<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB maps produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or Q or U map <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Astrophysical_component_separation&diff=10612Astrophysical component separation2015-01-29T12:01:07Z<p>Bbarreir: </p>
<hr />
<div>==CMB and foreground separation==<br />
<br />
See the Component Separation paper {{PlanckPapers|planck2013-p06}} for details.<br />
===NILC===<br />
NILC is a linear method for combining the input channels. It implements an ILC with weighting coefficients varying over the sky and over the multipole range up to <math>\ell=3200</math> and it does so using 'needlets' which are spherical wavelets. A special procedure is used for processing the coarsest needlet scale<br />
which contains the large scale multipoles.<br />
===SEVEM===<br />
The aim of Sevem is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations Leach et al., 2008 and to WMAP polarisation data Fernandez-Cobos et al., 2012. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.<br />
<br />
The input maps used are all the Planck frequency channels. In particular for intensity, we have cleaned the 100, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44) GHz, (44-70) GHz, (545-353) GHz and 857 GHz (smoothed at the resolution of the 545 GHz channel). For polarization the clean maps are at 70, 100 and 143 GHz and the templates are: (30-44) GHz smoothed to a common resolution, (353-217) GHz smoothed at 10', (217-143) GHz and (217-100) GHz smoothed at 1 degree. Before the subtraction we perform in painting to reduce the point source contamination.<br />
<br />
A linear combination of the templates is then subtracted from the Planck sky map at the frequency to be cleaned, in order to produce the clean CMB. The coefficients of the linear combination are obtained by minimising the variance of the clean map outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
The final CMB intensity map has then been constructed by combining the 143 and 217 GHz cleaned maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of FWHM =5 arcminutes at nside=2048. The final CMB polarization map has been obtained by combining the 100 and 143 GHz clean maps with nside=1024 and resolution of 10 arc minutes.<br />
<br />
===SMICA===<br />
<br />
<br />
A linear method, SMICA reconstructs a CMB map as a linear combination<br />
in the harmonic domain of <math>N_{chan}</math> input frequency maps<br />
with weights that depend on multipole <math>\ell</math>. Given the<br />
<math>N_{chan} × 1</math> vector <math>\mathbf{x}_{\ell m}</math> of<br />
spherical harmonic coefficients for the input maps, it computes<br />
coefficients <math>s_{\ell m}</math> for the CMB map as<br />
<br />
: <math>\label{eq:smica:shat} <br />
\hat{s}_{\ell m} = \mathbf{w}^†_\ell \mathbf{x}_{\ell m}</math><br />
<br />
where the <math>N_{chan} × 1</math> vector <math>\mathbf{w}_\ell<br />
</math> which contains the multipole-dependent weights is built to<br />
offer unit gain to the CMB with minimum variance. This is achieved<br />
with<br />
<br />
: <math>\label{eq:smica:w} <br />
\mathbf{w}_\ell = \frac{\mathbf{R}_\ell ^{-1} \mathbf{a}}{\mathbf{a}^† \mathbf{R}_\ell ^{-1} \mathbf{a}} </math><br />
<br />
where vector <math>\mathbf{a}</math> is the emission spectrum of the<br />
CMB evaluated at each channel (allowing for possible inter-channel<br />
recalibration factors) and <math> \mathbf{R}_\ell </math> is the<br />
<math>N_{chan} × N_{chan}</math> spectral covariance matrix of<br />
<math>\mathbf{x}_{\ell m}</math>. Taking <math>\mathbf{R}_\ell </math><br />
in Eq. \ref{eq:smica:w} to be the sample spectral covariance matrix<br />
<math>\mathbf{\hat{R}}_\ell </math> of the observations:<br />
<br />
: <math>\label{eq:smica:Rhat} <br />
\mathbf{\hat{R}}_\ell = \frac{1}{2 \ell + 1} \sum_m \mathbf{x}_{ \ell m} \mathbf{x}_{\ell m}^†</math> <br />
<br />
would implement a simple harmonic-domain ILC. This is not what SMICA<br />
does. As discussed below, we instead use a model <math>\mathbf{R}_\ell<br />
(θ)</math> and determine the covariance matrix to be used in<br />
Eq. \ref{eq:smica:w} by fitting <math>\mathbf{R}_\ell (θ)</math> to<br />
<math>\mathbf{\hat{R}}_\ell </math>. This is done in the maximum<br />
likelihood sense for stationary Gaussian fields, yielding the best fit<br />
model parameters θ as<br />
<br />
: <math>\label{eq:smica:thetahat}<br />
\hat{θ} = \rm{arg \, min}_θ \sum_\ell (2\ell + 1) ( \mathbf{\hat{R}}_\ell \mathbf{R}_\ell (θ)^{-1} \, +\, log \, det \, \mathbf{R}_\ell (θ)).</math><br />
<br />
<br />
SMICA models the data is a superposition of CMB, noise and<br />
foregrounds. The latter are not parametrically modelled; instead, we<br />
represent the total foreground emission by <math>d</math> templates<br />
with arbitrary frequency spectra, angular spectra and correlations:<br />
<br />
: <math> \label{eq:smica:Rmodel}<br />
\mathbf{R}_\ell (θ) = \mathbf{aa}^† \, C_\ell \, + \, \mathbf{A P}_\ell \mathbf{A}^† \, + \, \mathbf{N}_\ell <br />
</math> <br />
<br />
where <math>C_\ell </math> is the angular power spectrum of the CMB,<br />
<math>\mathbf{A}</math> is a <math>N_{chan} ×d</math> matrix,<br />
<math>\mathbf{P}_\ell </math> is a positive <math>d×d</math> matrix,<br />
and <math>\mathbf{N}_\ell </math> is a diagonal matrix representing<br />
the noise power spectrum. The parameter vector <math>θ</math> contains<br />
all or part of the quantities in Eq. (5).<br />
<br />
<br />
The above equations summarize the founding principles of SMICA; its<br />
actual operation depends on a choice for the spectral model<br />
<math>\mathbf{R}_\ell (θ)</math> and on several<br />
implementation-specific details.<br />
<br />
<br />
<br />
The actual implementation of SMICA includes the following steps:<br />
; Inputs<br />
: All nine Planck frequency channels from 30 to 857 GHz, harmonically transformed up to <math>\ell = 4000 </math>.<br />
; Fit<br />
: In practice, the SMICA fit,i.e.,the minimization of Eq. (4), is conducted in three successive steps: We first estimate the CMB spectral law by fitting all model parameters over a clean fraction of sky in the range <math> 100 ≤ \ell ≤ 680</math> and retaining the best fit value for vector <math> \mathbf{a}</math>. In the second step, we estimate the foreground emissivity by fixing a to its value from the previous step and fitting all the other parameters over a large fraction of sky in the range <math> 4 ≤ \ell ≤ 150</math> and retaining the best fit values for the matrix <math> \mathbf{A}</math>. In the last step, we fit all power spectrum parameters; that is, we fix <math>\mathbf{a}</math> and <math>\mathbf{A}</math> to their previously found values and fit for each <math> C_\ell </math> and <math>\mathbf{P}_\ell </math> at each <math>\ell</math>. <br />
;Beams<br />
: The discussion thus far assumes that all input maps have the same resolution and effective beam. Since the observed maps actually vary in resolution, we process the input maps in the following way. To the <math>i</math>-th input map with effective beam <math>b_i(\ell)</math> and sampled on an HEALPix grid with <math>N^i_{side}</math>, the CMB sky multipole <math>s_{\ell m}</math> actually contributes <math>s_{\ell m}a_i b_i(\ell) p_i(\ell)</math>, where <math>p_i(\ell)</math> is the pixel window function for the grid at <math>N^i_{side}</math>. Seeking a final CMB map at 5-arcmin resolution, the highest resolution of Planck, we work with input spherical harmonics re-beamed to 5 arcmins, <math>\mathbf{\tilde{x}}_{\ell m} </math>; that is, SMICA operates on vectors with entries <math>x ̃^i_{\ell m} = x^i_{\ell m} b_5(\ell) / b_i(\ell) / p_i(\ell)</math>, where <math>b_5(\ell)</math> is a 5 arcmin Gaussian beam function. By construction, SMICA then produces an CMB map with an effective Gaussian beam of 5 arcmin (without the pixel window function).<br />
; Pre-processing<br />
: We start by fitting point sources with SNR > 5 in the PCCS catalogue in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole in-painted. This is done at all frequencies but 545 and 857 GHz, where all point sources with SNR > 7.5 are masked and in-painted. <br />
; Masking and in-painting<br />
: In practice, SMICA uses a small Galactic mask leaving 97% of the sky. We deliver a full-sky CMB map in which the masked pixels (Galactic and point-source) are replaced by a constrained Gaussian realization.<br />
; Binning<br />
: In our implementation, we use binned spectra.<br />
; High <math>\ell</math><br />
: Since there is little point trying to model the spectral covariance at high multipoles, because the sample estimate is sufficient, SMICA implements a simple harmonic ILC at <math>\ell > 1500</math>; that is, it applies the filter (Eq. 2) with <math>\mathbf{R}_\ell = \mathbf{\hat{R}}_\ell</math>.<br />
<br />
Viewed as a filter, SMICA can be summarized by the weights <math>\mathbf{w}_\ell</math> applied to each input map as a function of multipole. In this sense, SMICA is strictly equivalent to co-adding the input maps after convolution by specific axi-symmetric kernels directly related to the corresponding entry of <math>\mathbf{w}_\ell</math>. The SMICA weights used here are shown in figure below for input maps in units of K<math>_\rm{RJ}</math>. They show, in particular, the (expected) progressive attenuation of the lowest resolution channels with increasing multipole.<br />
<br />
[[File:smica.jpg|thumb|center|600px|'''Weights <math>w_\ell</math> given by SMICA to the input maps, after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>, as a function of multipole.''']]<br />
<br />
===Commander-Ruler===<br />
<br />
The Commander-Ruler (C-R) approach implements Bayesian component separation in pixel space, fitting a parametric model to the data by sampling the posterior distribution for the model parameters. For computational reasons, the fit is performed in a two-step procedure: First, both foreground amplitudes and spectral parameters are found at low-resolution using MCMC/Gibbs sampling algorithms (Jewell et al. 2004; Wandelt et al. 2004; Eriksen et al. 2004, 2007, 2008). Second, the amplitudes are recalculated at high resolution by solving the generalized least squares system (GLSS) per pixel with the spectral parameters fixed to the their values from the low-resolution run.<br />
For the CMB-oriented analysis presented in this paper, we only use the seven lowest Planck frequencies, i.e., from 30 to 353 GHz. We first downgrade each frequency map from its native angular resolution to a common resolution of 40 arcminutes and re-pixelize at HEALPix N<math>_\rm{side}</math> = 256. Second, we set the monopoles and dipoles for each frequency band using a method that locally conserves spectral indices (Wehus et al. 2013, in preparation). We approximate the effective instrumental noise as white with an RMS per pixel given by the Planck scanning pattern and an amplitude calibrated by smoothing simulations of the instrumental noise including correlations to the same resolution. For the high-resolution analysis, the important pre-processing step is the upgrading of the effective low-resolution mixing matrices to full Planck resolution: this is done by repixelizing from N<math>_\rm{side}</math> = 256 to 2048 in harmonic space, ensuring that potential pixelization effects from the low-resolution map do not introduce sharp boundaries in the high-resolution map.<br />
<br />
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TBW.<br />
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<br />
== References ==<br />
<br />
<References /><br />
<br />
<br />
<br />
[[Category:HFI/LFI joint data processing|003]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10610CMB and astrophysical component maps2015-01-29T11:45:01Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. <br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is at nside=2048 with 5' resolution and up to lmax=4000; note that SEVEM also produces additional clean single frequency maps at 100, 143 and 217 GHz at their native resolution.<br />
:For polarization the clean CMB map is at nside=1024 with a resolution of 10' and lmax=3071; the additional clean maps are at 70 GHz (native resolution) and at 100 and 143 GHz (with 10' resolution).<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10609CMB and astrophysical component maps2015-01-29T11:43:41Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
:The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. <br />
<br />
;Resolution<br />
<br />
:For intensity the clean CMB map is at nside=2048 with 5' resolution and up to lmax=4000; note that SEVEM also produces additional clean single frequency maps at 100, 143 and 217 GHz at their native resolution.<br />
:For polarization the clean CMB map is at nside=1024 with a resolution of 10' and lmax=3071; the additional clean maps are at 70 GHz (native resolution) and at 100 and 143 GHz (with 10' resolution).<br />
<br />
;Confidence masks<br />
<br />
:The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10608CMB and astrophysical component maps2015-01-29T11:41:05Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. <br />
<br />
;Resolution<br />
<br />
Fot intensity the clean CMB map is at nside=2048 with 5' resolution and up to lmax=4000; note that SEVEM also produces additional clean single frequency maps at 100, 143 and 217 GHz at their native resolution.<br />
For polarization the clean CMB map is at nside=1024 with a resolution of 10' and lmax=3071; the additional clean maps are at 70 GHz (native resolution) and at 100 and 143 GHz (with 10' resolution).<br />
<br />
;Confidence masks<br />
<br />
The confidence masks cover the most contaminated regions of the sky, leaving approximately 85 per cent of useful sky for intensity and 80 per cent for polarization.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10607CMB and astrophysical component maps2015-01-29T11:28:56Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
;Principle<br />
<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. <br />
<br />
;Resolution<br />
<br />
Fot intensity the CMB map is at nside=2048 with 5' resolution and up to lmax=4000; note that SEVEM also produces clean single frequency maps<br />
<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10605CMB and astrophysical component maps2015-01-29T11:19:59Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations{{BibCite|leach2008}} and to WMAP polarisation data{{BibCite|fernandezcobos2012}}. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Note that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB. On the other hand, it provides ''channel maps'' and 100, 143, and 217 GHz for Intensity and 70, 100 and 143 GHz for Polarization which are used as the building blocks of the final map.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Note that the same expression applies for I, Q and U. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10601CMB and astrophysical component maps2015-01-29T11:16:34Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations{{BibCite|leach2008}} and to WMAP polarisation data{{BibCite|fernandezcobos2012}}. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Note that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB. On the other hand, it provides ''channel maps'' and 100, 143, and 217 GHz for Intensity and 70, 100 and 143 GHz for Polarization which are used as the building blocks of the final map.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
Usually we construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done in real space at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. The <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
The confidence mask is produced by looking at differences between three different SEVEM CMB reconstructions, leaving a suitable sky fraction of approximately 85 per cent.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
The confidence mask includes all the pixels above a given threshold, the CO emission and those pixels more affected by the high-pass filtering, leaving a useful sky fraction os approximately 80 per cent.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10595CMB and astrophysical component maps2015-01-29T10:48:23Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations{{BibCite|leach2008}} and to WMAP polarisation data{{BibCite|fernandezcobos2012}}. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Note that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB. On the other hand, it provides ''channel maps'' and 100, 143, and 217 GHz for Intensity and 70, 100 and 143 GHz for Polarization which are used as the building blocks of the final map.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
;Polarization<br />
<br />
To clean the polarization maps, a procedure similar to the one used for intensity data is applied to the Q and U maps independently. In particular, we clean the 70, 100 and 143 GHz using four templates: 30-44 (after being convolved with the beam of each other), 353-217 (smoothed at 10' resolution) and 217-143 and 217-100 (both at 1 degree resolution). Conversely to the intensity case and due to the lower availability of frequency channels, it becomes necessary to use the maps to be cleaned as part of one of the templates: the 100 GHz map is used in the 217-100 template to clean the 143 GHz one and the 143 GHz map is used in the 217-143 template to clean the 100 GHz one, making the clean maps less independent between them than in the intensity case.<br />
<br />
The linear coefficients are estimated independently for Q and U outside a mask, that covers point sources and the 3 per cent brightest Galactic emission. Once the maps have been cleaned, inpainting of the point sources detected at each map is carried out. The size of the holes to be inpainted takes into account the additional smoothing of the 100 and 143 GHz maps. The 100 and 143 GHz clean maps are then combined in harmonic space, using E and B decomposition, to produce the final CMB maps for the Q and U components at a resolution of 10′ (Gaussian beam) for a HEALPix parameter nside = 1024. Each map is weighted taking into account its corresponding noise level at each multipole. Finally, before applying the post-processing HPF to the clean polarization data, the region with the brightest Galactic residuals is inpainted (5 per cent of the sky).<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10594CMB and astrophysical component maps2015-01-29T10:32:31Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations{{BibCite|leach2008}} and to WMAP polarisation data{{BibCite|fernandezcobos2012}}. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Note that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB. On the other hand, it provides ''channel maps'' and 100, 143, and 217 GHz for Intensity and 70, 100 and 143 GHz for Polarization which are used as the building blocks of the final map.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
It should be stressed that the method is very fast and permits the generation of thousands of simulations to characterize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
;Intensity<br />
<br />
For the CMB intensity map, we have cleaned the 100 GHz, 143 GHz and 217 GHz maps using three templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and 857 as the fourth template. For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). First of all, the six frequency channels which are going to be used to construct templates are inpainted at the point source positions detected using the Mexican Hat Wavelet algorithm (Planck Collaboration A35 2014). The size of the holes to be inpainted is determined taking into account the beam size of the channel as well as the flux of each source. The inpainting algorithm is based on simple diffuse inpainting, which fills one pixel with the mean value of the neighbouring pixels in an iterative way. To avoid inconsistencies when subtracting two channels, each frequency map is inpainted on the sources detected in that map and on the second map (if any) used to construct the template. Then the maps are smoothed to a common resolution (the first channel in the subtraction is smoothed with the beam of the second map and viceversa). For the 857 GHz template, we simply filter this map with the beam from 545 GHz (this is for comparison with the previous pipeline, where the 857 GHz was smoothed at this resolution when using it to construct the 857–545 template). <br />
<br />
The coefficients are obtained outside the analysis mask, that covers the 1 per cent brightest emission of the sky as well as point sources detected at all frequency channels. Once the maps are cleaned, each of them is inpainted on the point sources positions detected at that (raw) channel. Then, the MHW algorithm is run again, now on the clean maps. A relatively small number of new sources are found and are also inpainted at each channel. The resolution of the clean map is the same as that of the raw map. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreirhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=CMB_and_astrophysical_component_maps&diff=10593CMB and astrophysical component maps2015-01-29T10:22:11Z<p>Bbarreir: </p>
<hr />
<div>== Overview ==<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in {{PlanckPapers|planck2013-p06}}.<br />
<br />
==CMB maps==<br />
CMB maps have been produced by the SMICA SEVEM, NILC and COMMANDER pipelines, which are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation | CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.. For each pipeline we provide:<br />
* Full-mission CMB intensity map, confidence mask and beam transfer function.<br />
* Full-mission high-pass filtered CMB polarisation map, <br />
* A confidence mask.<br />
* A beam transfer function.<br />
In addition, and for characterisation purposes, there are six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. And for each of these data splits we provide half-sum and half-difference maps. The half-difference maps can be used to provide an approximate noise estimate for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise correlations between the half-ring maps, and missing pixels in the other splits. The Intensity maps are provided at Nside = 2048, at 5 arcmin resolution, while the Polarisation ones are provided at Nside = 1024 at 10 arcmin resolution. All maps are in units of K<sub>cmb</sub>.<br />
<br />
These maps can be found in the files ''COM_CMB_IQU-{pipeline}-field-{Int/Pol}_Nside_R2.00.fits''. The ''Int'' files have two extensions, for the Intensity maps and the beam transfer function, the ''Pol'' files have three extensions, for Q and U maps, and for the beam transfer function.<br />
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.<br />
<br />
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order SMICA, SEVEM, NILC and COMMANDER, from top to bottom. The Intensity maps scale is [–500.+500] μK, and the noise are between [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180> <br />
File:CMB_smica_tsig.png<br />
File:CMB_smica_tnoi.png<br />
File:CMB_smica_tmask.png<br />
File:CMB_sevem_tsig.png<br />
File:CMB_sevem_tnoi.png<br />
File:CMB_sevem_tmask.png<br />
File:CMB_nilc_tsig.png<br />
File:CMB_nilc_tnoi.png<br />
File:CMB_nilc_tmask.png<br />
File:CMB_commander_tsig.png<br />
File:CMB_commander_tnoi.png<br />
File:CMB_commander_tmask.png<br />
</gallery><br />
</center><br />
<br />
===Product description ===<br />
====SMICA====<br />
; Principle<br />
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
; Resolution (effective beam)<br />
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''. It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function. Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.<br />
; Confidence mask<br />
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. <br />
; Masks and inpainting<br />
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.<br />
<br />
====NILC (done by CB, checks with producers in progress)====<br />
<br />
;Principle<br />
<br />
: The Needlet-ILC (hereafter NILC) CMB map is constructed both in total intensity as well as polarization, Q and U Stokes parameters. For total intensity, all Planck frequency channels are included. For polarization, all polarization sensitive frequency channels are included, from 30 to 353 GHz. The solution, for T, Q and U is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range. <br />
<br />
; Resolution (effective beam)<br />
<br />
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent of a Gaussian circular beam with FWHM=5 arcminutes. <br />
<br />
; Confidence mask<br />
<br />
: The same procedure is followed by SMICA and NILC for producing confidence masks, though with different parametrizations. A low resolution smoothed version of the NILC map, noise subtracted, is thresholded to 73.5 squared micro-K for T, and 6,75 squared micro-K for Q and U.<br />
<br />
{{PlanckPapers|planck2014-p11}}<br />
<br />
====SEVEM====<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations{{BibCite|leach2008}} and to WMAP polarisation data{{BibCite|fernandezcobos2012}}. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Note that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB. On the other hand, it provides ''channel maps'' and 100, 143, and 217 GHz for Intensity and 70, 100 and 143 GHz for Polarization which are used as the building blocks of the final map.<br />
<br />
====COMMANDER-Ruler====<br />
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at N<sub>side</sub>=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which <br />
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of: <br />
<br />
* Maps of the Amplitudes of the CMB at low resolution, N<sub>side</sub>=256, along with the standard deviations of the outputs, beam profiles derived from the production process. <br />
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, N<sub>side=2048, beam profiles derived from the production process. <br />
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.<br />
<br />
===Production process===<br />
====SMICA====<br />
; 1) Pre-processing<br />
: All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.<br />
; 2) Linear combination<br />
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.<br />
; 3) Post-processing<br />
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.<br />
<br />
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.<br />
<br />
<br />
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
====NILC (done by CB, check by producers in progress)====<br />
<br />
; Pre-processing<br />
<br />
: All sky frequency maps are deconvolved using the DPC beam transfer function provided, and re-convolved with a 5 arcminutes FWHM circular Gaussian beam. In polarization, prior to the smoothing process, all sky E and B maps are derived from Q and U using standard HEALPix tools from each individual frequency channels <br />
<br />
; Linear combination<br />
<br />
: Pre-processed input frequency maps are decomposed in needlet coefficients, specified in the Appendix B of the Planck A11 paper, with shape given by Table B.1. Minimum variance coefficients are then obtained, using all channels for T, from 30 to 353 for E and B. <br />
<br />
; Post-processing<br />
<br />
: E and B maps are re-combined into Q and U products using standard HEALPix tools. <br />
<br />
====SEVEM====<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math><br />
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
An additional level of flexibility can also be considered: the linear coefficients can be the same for all the sky, or several regions with different sets of coefficients can be considered. The regions are then combined in a smooth way, by weighting the pixels at the boundaries, to avoid discontinuities in the clean maps.<br />
Since the method is linear, we may easily propagate the noise properties to the final CMB map. Moreover, it is very fast and permits the generation of thousands of simulations to character- ize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
In particular, we have cleaned the 143 GHz and 217 GHz maps using four templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and (857-545). For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). In order to take into account the different spectral behaviour of the foregrounds at low and high galactic latitudes, we have considered two independent regions of the sky, for which we have used a different set of coefficients. The first region corresponds to the 3 per cent brightest Galactic emission, whereas the second region is defined by the remaining 97 per cent of the sky. For the first region, the coefficients are actually estimated over the whole sky (we find that this is more optimal than perform the minimisation only on the 3 per cent brightest region, where the CMB emission is very sub-dominant) while for the second region, we exclude the 3 per cent brightest region of the sky, point sources detected at any frequency and those pixels which have not been observed at all channels.<br />
Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
Moreover, additional CMB clean maps (at frequencies between 44 and 353 GHz) have also been produced using different combinations of templates for some of the analyses carried out in {{PlanckPapers|planck2013-p09}} and {{PlanckPapers|planck2013-p14}}. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in {{PlanckPapers|planck2013-p14}}, while frequencies from 70 to 217 GHz were used for consistency tests in {{PlanckPapers|planck2013-p09}}.<br />
<br />
====COMMANDER-Ruler====<br />
The production process consist in low and high resolution runs according to the description above. <br />
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA. <br />
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA. <br />
<br />
===Inputs===<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz. <br />
<br />
===File names and structure===<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.nn.fits''<br />
<br />
where ''method'' is mica, nilc, sevem, or commander, and Int and Pol indicate whether the file contains the temperature (Int) or the polarisation (Pol) maps. For this release the temperature maps are provided at Nside = 2048, and the polarisation maps at Nside = 1024. <br />
<br />
The files contain <br />
* a minimal primary extension with no data;<br />
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 14 columns in which the first 13 columns is a CMB map produced from the full or a subset of the data, as described in the table below, and the last column in a confidence mask. There is a single extension for ''Int'' files, and two, for Q and U, for ''Pol'' files. <br />
* a ''BINTABLE'' extension containing the beam window function.<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I or Q or U || Real*4 || uK_cmb || I or U or Q map<br />
|-<br />
|U || Real*4 || uK_cmb || U-polarization <br />
|- <br />
|HM1 || Real*4 || uK_cmb || Half-miss 1 <br />
|-<br />
|HM2 || Real*4 || uK_cmb || Half-miss 2 <br />
|-<br />
|YR1 || Real*4 || uK_cmb || Year 1 <br />
|-<br />
|YR2 || Real*4 || uK_cmb || Year 2 <br />
|-<br />
|HR1 || Real*4 || uK_cmb || Half-ring 1 <br />
|-<br />
|HR2 || Real*4 || uK_cmb || Half-ring 2 <br />
|-<br />
|HMHS || Real*4 || uK_cmb || Half-miss, half sum <br />
|-<br />
|HMHD || Real*4 || uK_cmb || Half-miss, half diff <br />
|-<br />
|YRHS || Real*4 || uK_cmb || Year, half sum <br />
|-<br />
|YRHD || Real*4 || uK_cmb || Year, half diff <br />
|-<br />
|HRHS || Real*4 || uK_cmb || Half-ring half sum <br />
|-<br />
|HRHD || Real*4 || uK_cmb || Half-ring half diff <br />
|-<br />
|MASK || BYTE || || Confidence mask <br />
|-<br />
<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|POLCCONV || String || COSMO || Polarization convention<br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (smica/nilc/sevem/commander)<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function. See Note 1.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
Notes:<br />
# The beam window function <math>B_\ell</math> given here includes the pixel window function <math>p_\ell</math> for the Nside=2048 pixelization. It means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.<br />
<br />
<!--- mi sembra che questa non serva più <br />
The low resolution COMMANDER-Ruler CMB product is organized in the following way:<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB low resolution COMMANDER-Ruler map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || CMB temperature map obtained as average over 1000 samples<br />
|-<br />
|I_stdev || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples<br />
|-<br />
|VALMASK|| Byte || none || Confidence mask<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_SIM01 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM02 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM03 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM04 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM05 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM06 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM07 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM08 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM09 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|I_SIM10 || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || none || The effective beam window function, including the pixel window function.<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)<br />
|-<br />
|}<br />
<br />
---><br />
<br />
<!---- anche queste non servono più <br />
<br />
The FITS files containing the ''union'' (or common) maks is:<br />
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}<br />
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.<br />
<br />
For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here<br />
*{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits|link=COM_CompMap_CMB-smica-field-I_2048_R1.20.fits}}<br />
This file contains a single extension with a single column containing the SMICA cmb temperature map.<br />
<br />
---><br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper {{PlanckPapers|planck2013-p06}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper {{PlanckPapers|planck2013-p06}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
None. <br />
<br />
===File names===<br />
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
====Low frequency foreground component====<br />
=====Low frequency component at N<sub>side</sub> = 256=====<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
=====Low frequency component at N<sub>side</sub> = 2048=====<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<sub>CMB</sub>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<sub>CMB</sub> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<sub>CMB</sub> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Thermal dust====<br />
=====Thermal dust component at N<sub>side</sub>=256=====<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<sub>CMB</sub> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<sub>CMB</sub> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
=====Thermal dust component at N<sub>side</sub>=2048=====<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
====Sky mask====<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
<br />
== References ==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Bbarreir