Difference between revisions of "CMB and astrophysical component maps"

From Planck Legacy Archive Wiki
Jump to: navigation, search
(→‎Production process)
(→‎Synchrotron emission)
 
(291 intermediate revisions by 15 users not shown)
Line 1: Line 1:
 +
{{DISPLAYTITLE:2015 CMB maps}}
 +
 
== Overview ==
 
== Overview ==
 +
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 each product and how it is obtained, followed by a description of the FITS file containing the data and associated information.
 +
All the details can be found in {{PlanckPapers|planck2014-a11}} and {{PlanckPapers|planck2014-a12}}.
 +
 +
==CMB maps==
 +
CMB maps have been produced using four different methods: COMMANDER, NILC, SEVEM, and SMICA, as 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.
 +
 +
'''As discussed extensively in {{PlanckPapers|planck2014-a01}}, {{PlanckPapers|planck2014-a07}}, {{PlanckPapers|planck2014-a09}}, and {{PlanckPapers|planck2014-a11}}, the residual systematics in the Planck 2015 polarization maps have been dramatically reduced compared to 2013, by as much as two orders of magnitude on large angular scales. Nevertheless, on angular scales greater than 10 degrees, correponding to l < 20, systematics are still non-negligible compared to the expected cosmological signal.'''
  
−
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.
+
'''It was not possible, for this data release, to fully characterize the large-scale residuals from the data or from simulations. Therefore all results published by the Planck Collaboration in 2015 which are based on CMB polarization have used maps which have been high-pass filtered to remove the large angular scales. We warn all users of the CMB polarization maps that they cannot yet be used for cosmological studies at large angular scales.'''
−
All the details can be found in <cite>#planck2013-p06</cite>.
 
  
−
==CMB maps==
+
'''For convenience, we provide as default polarized CMB maps from which all angular scales at l < 30 have been filtered out. '''
 +
 
 +
For each method we provide the following:
 +
* Full-mission CMB intensity map, confidence mask and beam transfer function.
 +
* Full-mission CMB polarisation map,
 +
* A confidence mask.
 +
* A beam transfer function.
 +
In addition, and for characterisation purposes, we include six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. For the year-1,2 and half-mission-1,2 data splits we provide half-sum and half-difference maps which are produced by running the corresponding sums and differences inputs through the pipelines. The half-difference maps can be used to provide an approximate noise estimates 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>.
 +
 
 +
In addition, for each method we provide three sets of files, each categorized by the "R2.0X" label as follows:
 +
 
 +
; ''R2.02''
 +
<pre style="white-space: pre-wrap;
 +
white-space: -moz-pre-wrap;
 +
white-space: -pre-wrap;
 +
white-space: -o-pre-wrap;
 +
word-wrap: break-word;">
 +
This set of intensity and polarisation maps are provided at a resolution of Nside=1024. The Stokes Q and U maps are high-pass filtered to contain only modes above l > 30, as explained above and as used for analysis by the Planck Collaboration; THESE ARE THE POLARISATION MAPS WHICH SHOULD BE USED FOR COSMOLOGICAL ANALYSIS. Each type of map is packaged into a separate fits file (as for "R2.01"), resulting in file sizes which are easier to download (as opposed to the "R2.00" files), and more convenient to use with commonly used analysis software.
 +
</pre>
 +
 
 +
; ''R2.01''
 +
<pre style="white-space: pre-wrap;
 +
white-space: -moz-pre-wrap;
 +
white-space: -pre-wrap;
 +
white-space: -o-pre-wrap;
 +
word-wrap: break-word;">
 +
This is the most complete set of 2015 CMB maps, containing Intensity products at a resolution of Nside=2048, and both Intensity and Polarisation at resolution of Nside=1024. For polarisation (Q and U), they contain all angular resolution modes. WE CAUTION USERS ONCE AGAIN THAT THE STOKES Q AND U MAPS ARE NOT CONSIDERED USEABLE FOR COSMOLOGICAL ANALYSIS AT l < 30. The structure of these files is the same as for "R2.02".
 +
</pre>
 +
 
 +
; ''R2.00''
 +
<pre style="white-space: pre-wrap;
 +
white-space: -moz-pre-wrap;
 +
white-space: -pre-wrap;
 +
white-space: -o-pre-wrap;
 +
word-wrap: break-word;">
 +
This set of files is equivalent to the "R2.01" set, but are packaged into only two large files. Warning: downloading these files could be very lengthy...
 +
</pre>
 +
 
 +
For a complete description of the above data structures, see [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.
  
−
Four pipelines have been used to produce maps of the CMB: Commander-Ruler, NILC, SEVEM and SMICA. The last three have been delivered as Legacy Archive products.
 
  
−
The front-runner CMB map is the SMICA one. This product is labeled as "Main product" in the Planck Legacy Archive Java interface while the two others (NILC, SEVEM) are labeled as "Additional product".
+
The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order COMMANDER, NILC, SEVEM and SMICA, from top to bottom. The Intensity maps' scale is [–500.+500] μK, and the noise spans [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.
  
−
The component separation pipelines 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 <cite>#planck2013-p06</cite> {{P2013|12}} and references therein.
+
<center>
 +
<gallery style="padding:0 0 0 0;" perrow=3 widths=300px heights=180>
 +
File:CMB_commander_tsig.png | '''commander temperature'''
 +
File:CMB_commander_tnoi.png | '''commander noise'''
 +
File:CMB_commander_tmask.png | '''commander mask'''
 +
File:CMB_nilc_tsig.png | '''nilc temperature'''
 +
File:CMB_nilc_tnoi.png | '''nilc noise'''
 +
File:CMB_nilc_tmask.png | '''nilc mask'''
 +
File:CMB_sevem_tsig.png | '''sevem temperature'''
 +
File:CMB_sevem_tnoi.png | '''sevem noise'''
 +
File:CMB_sevem_tmask.png | '''sevem mask'''
 +
File:CMB_smica_tsig.png | '''smica temperature'''
 +
File:CMB_smica_tnoi.png | '''smica noise'''
 +
File:CMB_smica_tmask.png | '''smica mask'''</gallery>
 +
</center>
  
 
===Product description ===
 
===Product description ===
  
−
; SMICA
+
====COMMANDER====
 +
 
 +
;Principle
 +
 
 +
: 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}}.
 +
 
 +
; Resolution (effective beam)
 +
 
 +
: The Commander sky maps have different angular resolutions depending on data products:
 +
* 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.
 +
* The Commander CMB temperature map derived from Planck-only observations has 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.
 +
* 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.
 +
 
 +
; Confidence mask
 +
 
 +
: 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.
 +
 
 +
====NILC====
 +
 
 +
;Principle
 +
 
 +
: 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.
 +
 
 +
; Resolution (effective beam)
 +
 
 +
: The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum <math>\ell=4000</math>. The effective beam is equivalent to a Gaussian circular beam with FWHM=5 arcminutes.
 +
 
 +
; Confidence mask
 +
 
 +
: 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.
 +
 
 +
 
 +
====SEVEM====
 +
; Principle
 +
 
 +
: 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.
 +
 
 +
;Resolution
 +
 
 +
: 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).
 +
: 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>.
 +
 
 +
; Confidence masks
 +
 
 +
: 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.
 +
 
 +
=====Foregrounds-subtracted maps=====
 +
 
 +
In addition to the regular CMB maps, SEVEM provides maps cleaned of the foregrounds for selected frequency channels (categorized as fgsub-sevem in the archive). In particular, for intensity there are clean CMB maps available at 100, 143 and 217 GHz, provided at the original resolution of the uncleaned channel and at Nside=2048. For polarization, there are Q/U clean CMB maps for the 70, 100 and 143 GHz (at Nside=1024). The 70 GHz clean map is provided at its original resolution, whereas the 100 and 143 GHz maps have a resolution given by a Gaussian beam with fwhm=10 arcminutes.
 +
 
 +
====SMICA====
 +
; Principle
 +
: SMICA produces CMB maps 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.
 +
; Resolution (effective beam)
 +
: 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 <math>N_{side}</math>=2048.
 +
: The SMICA Q and U maps are obtained similarly but are produced at <math>N_{side}</math>=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).
 +
; Confidence mask
 +
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and masked point sources.  This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel.  See section below detailing the production process.
 +
 
 +
 
 +
====Common Masks====
 +
 
 +
A number of common masks have been defined for analysis of the CMB temperature and polarization maps. They are based on the confidence masks provided by the component separation methods. One mask for temperature and one mask for polarization have been chosen as the preferred masks based on subsequent analyses.
 +
 
 +
The common masks for the CMB temperature maps are:
  
−
SMICA produces a CMB map by linearly  combining all Planck input channels
+
* UT78: union of the Commander, SEVEM, and SMICA temperature confidence masks (the NILC mask was not included since it masks much less of the sky). It has f<sub>sky</sub> = 77.6%. This is the preferred mask for temperature.
−
(from 30 to 857 GHz) with weights which vary with the multipole.
 
  
−
The SMICA map has an effective beam window function of 5 arc-minutes,  deconvolved from the pixel window.
+
* UTA76: in addition to the UT78 mask, it masks pixels where standard deviation between the four CMB maps is greater than 10 &mu;K. It has f<sub>sky</sub> = 76.1%.
−
It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_{(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_{(5')}</math> is a 5-arcminute Gaussian beam function.
 
  
−
The SMICA map has been inpainted over 3% of the sky using a constrained Gaussian realisation.
+
The common masks for the CMB polarization maps are:
−
A binary mask describing the inpainted area is provided.
 
  
−
We provide a confidence mask which excludes some parts of the Galactic
+
* UP78: the union of the Commander, SEVEM and SMICA polarization confidence masks (the NILC mask was not included since it masks much less of the sky). It has f<sub>sky</sub> = 77.6%.
−
plane and also the masked point sources.
 
  
 +
* UPA77: In addition to the UP78 mask, it masks pixels where the standard deviation between the four CMB maps, averaged in Q and U, is greater than 4 &mu;K.  It has f<sub>sky</sub> = 76.7%.
  
 +
* UPB77: in addition to the UP78 mask, it masks polarized point sources detected in the frequency channel maps. It has f<sub>sky</sub> = 77.4%. This is the preferred mask for polarization.
  
−
; NILC
+
====CMB-subtracted frequency maps ("Foreground maps")====
  
−
Needlet-ILC (hereafter NILC) produces a CMB map by applying the Internal
+
These are the full-sky, full-mission frequency maps in intensity from which the CMB has been subtracted. The maps contain foregrounds and noise. They are provided for each frequency channel and for each component separation method. They are grouped into 8 files, two for each method of which there is one for each instrument. The maps are are at N<sub>side</sub> = 1024 for the three LFI channels and at N<sub>side</sub> = 2048 for the six HFI channels. The filenames are:
−
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.
 
  
−
It uses all Planck channels from 44 to 857 GHz.
+
* ''LFI_Foregrounds-{method}_1024_Rn.nn.fits''  (145 MB each)
 +
* ''HFI_Foregrounds-{method}_2048_Rn.nn.fits''  (1.2 GB each)
  
 +
To remove the CMB, the respective CMB map was first deconvolved with the 5 arcmin beam, then convolved with the beam of the frequency channel, and finally subtracted from the frequency map. This was done using the <math>B_\rm{l}</math> in harmonic space, assuming a symmetric beam.
  
 +
The CMB-subtracted maps have complicated noise properties. The CMB maps contain a noise contribution from each of the frequency maps, depending on the weights with which they were combined. Therefore subtracting the CMB map from a frequency channel contributes additional noise from the other frequency channels.
  
−
; SEVEM
+
====Quadrupole Residual Maps====
  
−
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 <cite>#leach2008</cite> and to WMAP polarisation data Fernandez-Cobos et al., 2012 <cite>xx</cite>. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.
+
The second-order (kinematic) quadrupole is a frequency-dependent effect. During the production of the frequency maps the frequency-independent part was subtracted, which leaves a frequency-dependent residual quadrupole. The residuals in the component-separated CMB temperature maps have been estimated by simulating the effect in the frequency maps and propagating it through the component separation pipelines. The residuals have an amplitude of around 2 &mu;K peak-to-peak. The maps of the estimated residuals can be used to remove the effect by subtracting them from the CMB maps.
  
 
===Production process===
 
===Production process===
  
−
; SMICA
+
====COMMANDER====
 +
 
 +
; Pre-processing
 +
 
 +
: 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.
  
 +
; Priors
 +
 +
: The following priors are enforced in the Commander analysis:
 +
* 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
 +
* Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies
 +
* Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky
 +
* The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors
 +
 +
; Fitting procedure
 +
 +
: 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.
 +
 +
====NILC====
  
−
The actual implementation of SMICA includes the following steps:
 
−
; Inputs
 
−
: All nine Planck frequency channels from 30 to 857 GHz, harmonically transformed up to  <math>\ell = 4000 </math>.
 
−
; Fit
 
−
: In practice, the SMICA fit,i.e.,the minimization of Eq. (4) in the [[Astrophysical component separation#SMICA|SMICA]] description section, 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>.
 
−
;Beams
 
−
: 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).
 
 
; Pre-processing
 
; Pre-processing
−
: 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. 
 
−
; Masking and in-painting
 
−
: 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.
 
−
; Binning
 
−
: In our implementation, we use binned spectra.
 
−
; High <math>\ell</math>
 
−
: 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) in the [[Astrophysical component separation#SMICA|SMICA]] description section) with <math>\mathbf{R}_\ell = \mathbf{\hat{R}}_\ell</math>.
 
  
−
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 the 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.
+
: 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  
  
−
[[File:smica.jpg|thumb|center|600px|'''Figure 1. 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.''']]
+
; Linear combination
  
−
; NILC
+
: 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.
  
−
The ability linearly to combine input maps varying over the sky and over multipoles is called ‘localisation’. In the needlet framework, harmonic localisation is achieved using a set of bandpass filters defining ‘scales’ and spatial localization is achieved, at each scale, by defining zones over the sky. The harmonic localisation used here uses 9 spectral bands covering multipoles up to <math>\ell</math> = 3200 (see Figure 2). The spatial localisation depends on the scale: at the coarsest scale, which include the multipoles of lowest degree, we use a single zone (no localization) while at the finest scales (which include the highest degree multipoles), the sky is partitioned in up to 20 zones (again, see Figure 2).
+
; Post-processing
  
−
<center>
+
: E and B maps are re-combined into Q and U products using standard HEALPix tools.
−
<gallery perrow=2 widths=300px heights=180px>
+
 
−
File:Nilc1.jpg | Spectral window functions defining nine ''needlet scales''
+
====SEVEM====
−
File:Nilc2.jpg | The 2-zone partition
+
 
−
File:Nilc3.jpg | The 4-zone partition
+
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>
−
File:Nilc4.jpg | The 20-zone partition.
+
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).
−
</gallery>
 
−
'''Figure 2. Spectral localization for NILC using with nine spectral window functions defining nine ‘needlet scales’ (top left panel). The scale-dependent spatial localization partitions the sky in 1 zone (for scale 1), 2 zones (for scale 2), 4 zones (for scale 3), or 20 zones (for scales 5, 6, 7, 8, 9).'''
 
−
</center>
 
  
−
The NILC method amounts to applying an ILC in each zone of each scale, allowing the ILC weights to adapt naturally to the varying strength of the contaminants as a function of direction and multipole. A complete description of the basic NILC method can be found in Delabrouille et al. (2009) <cite>#delabrouille2009</cite>. In this work, however, we have implemented an important difference for the processing of the coarsest scale.
+
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, and these intermediate products (clean maps at individual frequencies for intensity and polarization) are also provided in the archive. 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.
  
−
The actual processing differs from the above scenario in several respects: pre-processing of point sources, dealing with frequency-dependent beams, and dealing with statistical issues (the ILC bias) in the coarsest scale.
+
;Intensity
−
* ''Pre-processing of point sources''. Identical to the SMICA pre-processing.
 
−
* ''Masking and inpainting''. The NILC CMB map is actually produced in a two step process. In a first step, the NILC weights are computed from needlet statistics evaluated using a Galactic mask which covers about 98% of the sky (and is apodiwed at 1 degree). In a second step, those NILC weights on are applied to needlet coefficients computed over the whole sky (the point sources having been subtracted or fitted at the pre-processing stage), yielding a NILC CMB estimate over the whole sky, except for the point source mask. In a final step, those masked pixels are replaced by the values of a constrained Gaussian realization.
 
−
* ''Beam control and transfer function''. As in the SMICA processing (see that section), the input maps are represented by their spherical harmonic coefficients. By internally rebeaming to a 5 arcmin resolution and by the unbiasedness property of the ILC, the resulting CMB map is automatically synthesized with an effective Gaussian beam of 5 arcmin.
 
−
* ''ILC bias and spectral statistics for the coarsest scale''. The coarsest scale of the NILC filter is not localized. Therefore, the NILC map at the coarsest scale is equivalent to a plain pixel-based ILC which is known to be quite susceptible to an ‘ILC bias’ due to chance correlations between the CMB and foregrounds. In order to mitigate that effect, the covariance matrix which determines the ILC coefficients at the coarsest scale is not computed as a pixel average but is rather estimated in the spectral domain with a spectral weight which equalizes the power of the CMB modes (based on a fiducial spectrum).
 
−
* ''Using SMICA recalibration''. In our current rendering, the NILC uses for the CMB emission law the values determined by SMICA.
 
  
−
; SEVEM
+
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.
  
−
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; Casaponsa et al. 2011 <cite>#Casaponsa2011</cite>) 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.
+
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.
  
−
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:
+
In addition, the clean CMB maps produced at 100, 143 and 217 GHz frequencies are also provided. The resolution of these maps is the same as that of the uncleaned frequency channels and have been constructed at Nside=2048. They have been inpainted at the position of the detected point sources. Note that these three clean maps should be close to independent, although some level of correlation will be present since the same templates have been used to clean the maps.
  
−
:<math> \label{eq:eq4}
+
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.
−
T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x})
 
−
</math>
 
  
−
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).
+
;Polarization
  
−
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.
+
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
−
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.
+
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
 +
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
 +
order to increase the signal-to-noise ratio of the template. 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. In this way, the 100 GHz
 +
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.
  
−
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.
+
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
 +
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) to avoid the introduction of ringing around the Galactic centre in the filtering process.
  
−
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.
+
The clean CMB maps at individual frequency channels produced as intermediate steps of SEVEM are also provided for Q and U, constructed at Nside=1024. The clean 70 GHz map is provided at its native resolution, while the clean maps at 100 and 143 GHz frequencies have a resolution of 10 arcminutes (Gaussian beam). The three maps have been inpainted in the positions of the detected point sources. Note that, due to the availability of a smaller number of templates for polarization than for intensity, these maps are less independent than for the temperature case, since, for instance, the 100 GHz map is used to clean the 143 GHz one and viceversa.
−
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.
 
  
−
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 <cite>#planck2013-p09</cite> {{P2013|23}} and <cite>#planck2013-p14</cite> {{P2013|19}}. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in <cite>#planck2013-p14</cite>, while frequencies from 70 to 217 GHz were used for consistency tests in <cite>#planck2013-p09</cite>.
+
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.
  
−
The method has been successfully applied to Planck simulations <cite>#leach2008</cite> and to WMAP polarisation data <cite>#Fernandez-Cobos2012</cite>.
 
  
−
===Inputs===
 
  
−
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section.
+
====SMICA====
  
−
; SMICA
+
A) Production of the intensity map.
  
−
SMICA uses all nine Planck frequency channels from 30 to 857 GHz. SMICA uses a pre-processing step in which point sources are subtracted or masked as described above.
+
; 1) Pre-processing
 +
: 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.
 +
; 2) Linear combination
 +
: 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.
 +
; 3) Post-processing
 +
: 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.
  
−
; NILC
+
<!--[[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.''']]-->
  
−
NILC uses eight frequency channels from 44 to 857 GHz and the same pre-processing step as SMICA.
+
B) Production of the Q and U polarisation maps.
  
−
; SEVEM
+
The SMICA pipeline for polarization uses all the 7 polarized Planck channels.  The production of the Q and U maps is similar to the production of the intensity map.  However, there is no input point source pre-processing of the input maps.  The regions of very strong emission are masked out using an apodized mask before computing the E and B modes of the input maps and combining them to produce the E and B modes of the CMB map.  Those 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.
  
−
SEVEM uses all nine Planck frequency channel maps. The 30 - 70 GHz and 353 - 857 GHz maps are used to construct templates by taking the differences (30 - 44) GHz, (44 - 70) GHz, (545 - 353) GHz and (857 - 545) GHz, after smoothing to a common resolution. The 100, 143 and 217 GHz maps are cleaned using the templates.
+
<!--[[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.''']]-->
  
−
===Related products===
+
===Inputs===
 +
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.
  
 
===File names and structure===
 
===File names and structure===
  
−
The FITS files corresponding to the three CMB products are the following:
+
Three sets of files  FITS files containing the CMB products are available.  In the first set all maps (i.e., covering different parts of the mission) and all characterisation products for a given method and a given Stokes parameter are grouped into a single extension, and there are two files per ''method'' (smica, nilc, sevem, and commander), one for the high resolution data (I only, Nside=2048) and one for low resolution data (Q and U only, Nside=1024).  Each file also contains the associated confidence mask(s) and beam transfer function.  '''These are the R2.00 files''' which have names like
 +
*''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.00.fits''
 +
There are 7 coverage periods:''full'', ''halfyear-1,2'', ''halfmission-1,2'', or ''ringhalf-1,2'', and 4 characterisation products: ''half-sum'' and half-difference'' for the year and the half-mission periods.
  
−
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.11.fits|link=COM_CompMap_CMB-nilc_2048_R1.11.fits}}
+
In the second second set the different coverages are split into different files which in most cases have a single extension with I only (Nside=1024) and I, Q, and U (Nside=1024). This second set was built in order to allow users to use standard codes like ''spice'' or ''anafast'' on them, directly. So this set contains the I maps at Nside=1024, which are not contained in the R2.00; on the other hand this set does not contain the half-sum and half-difference maps.   '''These are the 2.01 files''' which have names like
−
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.11.fits|link=COM_CompMap_CMB-sevem_2048_R1.11.fits}}
+
*''COM_CMB_IQU-{method}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits'' for the regular CMB maps, and
−
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.11.fits|link=COM_CompMap_CMB-smica_2048_R1.11.fits}}
+
*''COM_CMB_IQU-{fff}-{fgsub-sevem}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits'' for the sevem frequency-dependent, foregrounds-subtracted maps,
 +
where ''field-Int|Pol'' is used to indicate that only Int or only Pol data are contained (at present only ''field-Int'' is used for the high-res data), and is not included in the low-res data which contains all three Stokes parameters, and ''coverage'' is one of ''full'', ''halfyear-1,2'', ''halfmission-1,2'', or ''ringhalf-1,2''. Also, the coverage=''full'' files contain also the confidence mask(s) and beam transfer function(s) which are valid for all products of the same method (one for Int and one for Pol when both are available).
  
−
and the CMB they contain is shows below.
+
The third set has the same structure as the Nside=1024 products of R2.01, but '''the Q and U maps have been high-pass filtered to remove modes at l < 30 for the reasons indicated earlier.  These are the default products for use in polarisation studies.  They are the R2.02 files''' which have names like:
 +
*''COM_CMB_IQU-{method}_1024_R2.02_{coverage}.fits''
  
−
<center>
+
====Version 2.00 files====
−
<gallery perrow=3 widths=260px heights=170px>
 
−
File: CMB-smica.png | SMICA
 
−
File: CMB-nilc.png | NILC
 
−
File: CMB-sevem.png | SEVEM
 
−
</gallery></center>
 
  
 +
These have names like
 +
*''COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.00.fits'',
 +
as indicated above.  They contain:
 +
* a minimal primary extension with no data;
 +
* 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. 
 +
* a ''BINTABLE'' extension containing the beam transfer  function (mistakenly called window function in the files).
  
−
The files contains a minimal primary extension with no data and four data extensions which are described in the table below:
+
If Nside=1024 the files contain I, Q and U maps, whereas if Nside=2048 only the I map is given.
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
−
|+ '''CMB map file data structure'''
+
|+ '''CMB R2.00 map file data structure'''
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)
+
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I         || Real*4 || uK_cmb || The CMB temperature map
+
|I or Q or U    || Real*4 || uK_cmb || I or Q or U map                            
 +
|- 
 +
|HM1  || Real*4 || uK_cmb || Half-miss 1                                   
 +
|-
 +
|HM2  || Real*4 || uK_cmb || Half-miss 2                                   
 +
|-
 +
|YR1  || Real*4 || uK_cmb || Year 1                                       
 +
|-
 +
|YR2  || Real*4 || uK_cmb || Year 2                                       
 +
|-
 +
|HR1  || Real*4 || uK_cmb || Half-ring 1                                   
 +
|-
 +
|HR2  || Real*4 || uK_cmb || Half-ring 2                                   
 +
|-
 +
|HMHS || Real*4 || uK_cmb || Half-miss, half sum                           
 +
|-
 +
|HMHD || Real*4 || uK_cmb || Half-miss, half diff                           
 +
|-
 +
|YRHS || Real*4 || uK_cmb || Year, half sum                                 
 +
|-
 +
|YRHD || Real*4 || uK_cmb || Year, half diff                               
 
|-
 
|-
−
|NOISE  || Real*4 || uK_cmb || Estimated noise map (Note 1)
+
|HRHS || Real*4 || uK_cmb || Half-ring half sum                           
 
|-
 
|-
−
|VALMASK|| Byte || none || Validity, or confidence mask (note 2)
+
|HRHD || Real*4 || uK_cmb || Half-ring half diff                           
 
|-
 
|-
−
|INPMASK || Byte || none || Inpainted mask (Optional - see Note 3)
+
|MASK || BYTE ||   || Confidence mask                              
 
|-
 
|-
 +
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Keyword || Data Type || Value || Description
 
! Keyword || Data Type || Value || Description
Line 179: Line 327:
 
|-
 
|-
 
|COORDSYS ||  String || GALACTIC ||Coordinate system  
 
|COORDSYS ||  String || GALACTIC ||Coordinate system  
 +
|-
 +
|POLCCONV || String || COSMO  || Polarization convention
 
|-
 
|-
 
|ORDERING || String || NESTED  || Healpix ordering
 
|ORDERING || String || NESTED  || Healpix ordering
 
|-
 
|-
−
|NSIDE  ||  Int || 2048 || Healpix Nside
+
|NSIDE  ||  Int || 1024 or 2048 || Healpix Nside
 +
|-
 +
|METHOD  || String ||name || Cleaning method (smica/nilc/sevem/commander)
 +
|-
 +
|- bgcolor="ffdead" 
 +
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE) .  See Note 1
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|BEAMWF          || Real*4 || none || The effective beam transfer function, including the pixel window function.  See Note 2.
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data Type || Value || Description
 +
|-
 +
|LMIN ||  Int || value || First multipole of beam TF
 +
|-
 +
|LMAX ||  Int || value || Last multipole of beam TF
 
|-
 
|-
−
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM)
+
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
 
|-
 
|-
 +
|}
 +
 +
Notes:
 +
# Actually this is a beam ''transfer'' function, so BEAM_TF would have been more appropriate.
 +
# The beam transfer 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>. The beam ''Window'' function is given by <math>W_\ell = B_\ell^2</math>
 +
 +
 +
====Version 2.01 files====
 +
 +
These files have names like:
 +
*''COM_CMB_IQU-{method}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits'' for the regular CMB maps, and
 +
*''COM_CMB_IQU-{fff}-{fgsub-sevem}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits'' for the sevem frequency-dependent, foregrounds-subtracted maps,
 +
as indicated above. They contain:
 +
* a minimal primary extension with no data, but with a NUMEXT keyword giving the number of extensions contained.
 +
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 1-5 columns depending on the file, as described above: the minimum begin I only, the maximum begin I, Q, U, and confidence masks for I and P. 
 +
* a ''BINTABLE'' extension containing the beam transfer function(s): one for I, and a second one that applies to both Q and U, if Nslde=1024.
 +
 +
If Nside=1024 the files contain I, Q and U maps, whereas if Nside=2048 only the I map is given. The basic structure, including information on the most important keywords, is given in the table below.  For full details, see the FITS header.
 +
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|+ '''CMB R2.01 map file data structure'''
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
!colspan="4" | Ext. 2. EXTNAME = ''FGDS-LFI'' (BINTABLE) - Note 4
+
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|LFI_030  || Real*4 || K_cmb || 30 GHz foregrounds
+
|I_Stokes    || Real*4 || uK_cmb || I map (Nside=1024,2048)
 +
|- 
 +
|Q_Stokes    || Real*4 || uK_cmb || Q map (Nside=1024)                                 
 
|-
 
|-
−
|LFI_044  || Real*4 || K_cmb || 44 GHz foregrounds
+
|U_Stokes    || Real*4 || uK_cmb || U map (Nside=2048)                                   
 
|-
 
|-
−
|LFI_070   || Real*4 || K_cmb || 70 GHz foregrounds
+
|TMASK    || Int || none   || optional Temperature confidence mask                                 
 +
|-
 +
|PMASK    || Int || none  || optional Polarisation confidence mask                                   
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Keyword || Data Type || Value || Description
 
! Keyword || Data Type || Value || Description
 +
|-
 +
|AST-COMP ||  String || CMB || Astrophysical compoment name
 
|-
 
|-
 
|PIXTYPE ||  String || HEALPIX ||
 
|PIXTYPE ||  String || HEALPIX ||
 
|-
 
|-
 
|COORDSYS ||  String || GALACTIC ||Coordinate system  
 
|COORDSYS ||  String || GALACTIC ||Coordinate system  
 +
|-
 +
|POLCCONV || String || COSMO  || Polarization convention
 
|-
 
|-
 
|ORDERING || String || NESTED  || Healpix ordering
 
|ORDERING || String || NESTED  || Healpix ordering
 
|-
 
|-
−
|NSIDE  ||  Int || 1024 || Healpix Nside
+
|NSIDE  ||  Int || 1024 or 2048 || Healpix Nside
 
|-
 
|-
 
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM)
 
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM)
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
!colspan="4" | Ext. 3. EXTNAME = ''FGDS-HFI'' (BINTABLE) - Note 4
+
!colspan="4" | Optional Ext. 2. or 3. EXTNAME = ''BEAM_TF'' (BINTABLE)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|HFI_100  || Real*4 || K_cmb || 100 GHz foregrounds
+
|INT_BEAM          || Real*4 || none || Effective beam transfer function. See Note 1.
 
|-
 
|-
−
|HFI_143    || Real*4 || K_cmb || 143 GHz foregrounds
+
|POL_BEAM        || Real*4 || none || Effective beam transfer function. See Note 1.
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data Type || Value || Description
 +
|-
 +
|LMIN ||  Int || value || First multipole of beam WF
 +
|-
 +
|LMAX_I ||  Int || value || Last multipole for Int beam TF
 +
|-
 +
|LMAX_P ||  Int || value || Last multipole for Pol beam TF
 +
|-
 +
|METHOD  || String ||name || Cleaning method
 +
|-
 +
|}
 +
Notes:
 +
# The beam transfer 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>. The beam ''Window'' function is given by <math>W_\ell = B_\ell^2</math>
 +
 
 +
====Version 2.02 files====
 +
 
 +
'''For polarisation work, this is the default set of files to be used for cosmological analysis. Their content is identical to the "R2.01" files, except that angular scales above l < 30 have been filtered out of the Q and U maps. '''
 +
 
 +
These files have names like:
 +
*''COM_CMB_IQU-{method}_1024_R2.02_{coverage}.fits''
 +
as indicated above. They contain:
 +
The files contain
 +
* a minimal primary extension with no data, but with a NUMEXT keyword giving the number of extensions contained.
 +
* one or two ''BINTABLE'' data extensions with a table of Npix lines by 1-5 columns depending on the file, as described above: the minimum begin I only, the maximum begin I, Q, U, and confidence masks for I and P. 
 +
* a ''BINTABLE'' extension containing 2 beam transfer functions: one for I and one that applies to both Q and U.
 +
 
 +
If Nside=1024 the files contain I, Q and U maps, whereas if Nside=2048 only the I map is given. The basic structure, including information on the most important keywords, is given in the table below.  For full details, see the FITS header.
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|+ '''CMB R2.02 map file data structure'''
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Ext. 1. or 2. EXTNAME = ''COMP-MAP'' (BINTABLE)
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|HFI_217   || Real*4 || K_cmb || 217 GHz foregrounds
+
|I_Stokes   || Real*4 || uK_cmb || I map (Nside=1024)
 +
|- 
 +
|Q_Stokes    || Real*4 || uK_cmb || Q map (Nside=1024)                                 
 
|-
 
|-
−
|HFI_353  || Real*4 || K_cmb || 353 GHz foregrounds
+
|U_Stokes    || Real*4 || uK_cmb || U map (Nside=2048)                           
 
|-
 
|-
−
|HFI_545   || Real*4 || MJy/sr || 545 GHz foregrounds
+
|TMASK   || Int || none  || optional Temperature confidence mask                                 
 
|-
 
|-
−
|HFI_857   || Real*4 || MJy/sr || 857 GHz foregrounds
+
|PMASK   || Int || none  || optional Polarisation confidence mask                                   
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Keyword || Data Type || Value || Description
 
! Keyword || Data Type || Value || Description
 +
|-
 +
|AST-COMP ||  String || CMB || Astrophysical compoment name
 
|-
 
|-
 
|PIXTYPE ||  String || HEALPIX ||
 
|PIXTYPE ||  String || HEALPIX ||
 
|-
 
|-
 
|COORDSYS ||  String || GALACTIC ||Coordinate system  
 
|COORDSYS ||  String || GALACTIC ||Coordinate system  
 +
|-
 +
|POLCCONV || String || COSMO  || Polarization convention
 
|-
 
|-
 
|ORDERING || String || NESTED  || Healpix ordering
 
|ORDERING || String || NESTED  || Healpix ordering
 
|-
 
|-
−
|NSIDE  ||  Int || 2048 || Healpix Nside
+
|NSIDE  ||  Int || 1024 or 2048 || Healpix Nside
 
|-
 
|-
 
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM)
 
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM)
 +
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)
+
!colspan="4" | Optional Ext. 2. or 3. EXTNAME = ''BEAM_TF'' (BINTABLE)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|BEAM_WF         || Real*4 || uK_cmb || The CMB temperature map
+
|INT_BEAM         || Real*4 || none || Effective beam transfer function. See Note 1.
 +
|-
 +
|POL_BEAM        || Real*4 || none || Effective beam transfer function. See Note 1.
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
Line 251: Line 491:
 
|LMIN ||  Int || value || First multipole of beam WF
 
|LMIN ||  Int || value || First multipole of beam WF
 
|-
 
|-
−
|LMAX ||  Int || value || Lsst multipole of beam WF
+
|LMAX_I ||  Int || value || Last multipole for Int beam TF
 +
|-
 +
|LMAX_P ||  Int || value || Last multipole for Pol beam TF
 
|-
 
|-
−
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM)
+
|METHOD  || String ||name || Cleaning method  
 
|-
 
|-
 
|}
 
|}
−
 
−
 
 
Notes:
 
Notes:
−
# The half-ring half-difference (HRHD) map is made by passing the half-ring frequency maps independently through the component separation pipeline, then computing half their difference. It approximates a noise realisation, and gives an indication of the uncertainties due to instrumental noise in the corresponding CMB map.
+
# The beam transfer 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>. The beam ''Window'' function is given by <math>W_\ell = B_\ell^2</math>
−
# The confidence mask indicates where the CMB map is considered valid.
 
−
# NILC and SMICA CMB maps have been inpainted in the Galactic plane and around some bright sources with a constrained realisation of the signal. The inpainted area covers approximately 3% of the sky. This column is not present in the SEVEM product file.
 
−
# The subtraction of the CMB from the sky maps in order to produce the foregrounds map is done after convolving the CMB map to the resolution of the given frequency.
 
  
−
===Cautionary notes===
+
====Common masks====
  
−
# The half-ring CMB maps are produced by the pipelines with parameters/weights fixed to the values obtained from the full maps. Therefore the CMB HRHD maps do not capture all of the uncertainties due to foreground modelling on large angular scales.
+
The common masks are stored into two different files for Temperature and Polarisation respectively:
−
# The HRHD maps for the HFI frequency channels underestimate the noise power spectrum at high l by typically a few percent. This is caused by correlations induced in the pre-processing to remove cosmic ray hits. The CMB is mostly constrained by the HFI channels at high l, and so the CMB HRHD maps will inherit this deficiency in power.
+
* ''COM_CMB_IQU-common-field-MaskInt_2048_R2.nn.fits'' with the UT78 and UTA76 masks
−
# The beam transfer functions do not account for uncertainties in the beams of the frequency channel maps.
+
* ''COM_CMB_IQU-common-field-MaskPol_1024_R2.nn.fits'' with the UP78, UPA77, and UPB77 masks
 +
Both files contain also a map of the missing pixels for the half mission and year coverage periods. The 2 (for Temp) or 3 (for Pol) masks and the missing pixels maps are stored in 4 or 5 column a ''BINTABLE'' extension 1 of each file, named ''MASK-INT'' and ''MASK-POL'', respectively. See the FITS file headers for details.
  
−
== Astrophysical foregrounds from parametric component separation ==
+
====Quadrupole residual maps====
  
−
We describe diffuse foreground products for the Planck 2013 release. See Planck paper P06-Component Separation <cite>#planck2013-p06</cite> for a detailed description and astrophysical discussion of those.
+
The quadrupole residual maps are stored in files called:
 +
* ''COM_CMB_IQU-kq-resid-{method}-field-Int_2048_R2.02.fits''
  
−
===Product description===
+
They contain:
 +
* a minimal primary extension with no data, but with a NUMEXT keyword giving the number of extensions contained.
 +
* a single ''BINTABLE'' extension with a single column of Npix lines containing the HEALPIX map indicated
  
−
; Low frequency foreground component
+
The basic structure of the data extension is shown below. For full details see the extension header.  
−
: 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 Nside 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at Nside=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 Nside 2048 product.
 
  
−
; Thermal dust
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
−
: 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 Nside 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at Nside=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.
+
|+ '''Kinetic quadrupole residual map file data structure'''
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|INTENSITY    || Real*4 || K_cmb || the residual map                           
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data Type || Value || Description
 +
|-
 +
|AST-COMP ||  String || KQ-RESID || Astrophysical compoment name
 +
|-
 +
|PIXTYPE ||  String || HEALPIX ||
 +
|-
 +
|COORDSYS ||  String || GALACTIC ||Coordinate system
 +
|-
 +
|POLCCONV || String || COSMO  || Polarization convention
 +
|-
 +
|ORDERING || String || NESTED  || Healpix ordering
 +
|-
 +
|NSIDE  ||  Int || 2048 || Healpix Nside
 +
|-
 +
|METHOD  || String ||name || Cleaning method
 +
|-
 +
|}
  
−
; Sky mask
+
== Astrophysical foregrounds from parametric component separation ==
−
: 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.
+
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}}.
  
−
===Production process===
+
===Low-resolution temperature products===
  
−
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input
+
: 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.  
−
frequency channels is reduced to Nside=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution
 
−
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is
 
−
applied to the data at full resolution in order to obtain the provided products at Nside=2048. In the Planck paper P06-Component Separation <cite>#planck2013-p06</cite> additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.
 
  
−
===Inputs===
+
====Inputs====
  
−
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAMaps|inst=LFI|freq=30|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix.  
+
The following data products are used for the low-resolution analysis:
−
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].
+
* Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}
 +
* Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}
 +
* Full-mission 70 GHz ds1 (18+23), ds2 (19+22), and ds3 (20+21) detector-set maps
 +
* Full-mission 100 GHz ds1 and ds2 detector set maps
 +
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
 +
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps
 +
* Full-mission 353 GHz detector set ds2 and detector 1 maps
 +
* Full-mission 545 GHz detector 2 and 4 maps
 +
* Full-mission 857 GHz detector 2 map
 +
* Beam-symmetrized 9-year WMAP K-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Beam-symmetrized 9-year WMAP Ka-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Default 9-year WMAP Q1 and Q2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Default 9-year WMAP V1 and V2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Default 9-year WMAP W1, W2, W3, and W4 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Re-processed 408 MHz survey map, Remazeilles et al. (2014) [http://lambda.gsfc.nasa.gov/product/foreground/2014_haslam_408_info.cfm (Lambda)]
 +
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.
  
−
===Related products===
+
====Outputs====
  
−
None.
+
=====Synchrotron emission=====
  
−
===File names===
+
<!--<center>
 +
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px>
 +
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''
 +
</gallery>
 +
</center>-->
  
−
* Low frequency component at Nside 256:  
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}
−
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}
+
: Reference frequency: 408 MHz
−
* Low frequency component at Nside 2048:  
+
: Nside = 256
−
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}
+
: Angular resolution = 60 arcmin
−
* Thermal dust at Nside 256:
 
−
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}
 
−
* Thermal dust at Nside 2048:
 
−
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}
 
  
−
* Mask:  
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}
+
|+ HDU -- COMP-MAP-Synchrotron
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum   
 +
|-
 +
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean
 +
|-
 +
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms
 +
|}
  
−
===Meta Data===
 
  
−
====Low frequency foreground component====
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ Extension 1 -- SYNC-TEMP
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|nu  || Real*4 || Hz || Frequency   
 +
|-
 +
|intensity || Real*4 || W/Hz/m2/sr || GALPROP z10LMPD_SUNfE spectrum   
 +
|}
  
−
=====Low frequency component at Nside 256=====
+
=====Free-free emission=====
  
−
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}}
−
: '''Name HDU -- COMP-MAP'''
+
: Reference frequency: NA
 +
: Nside = 256
 +
: Angular resolution = 60 arcmin
  
−
The Fits extension is composed by the columns described below:
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ FITS header
+
|+ HDU -- COMP-MAP-freefree
 
|-
 
|-
 +
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I || Real*4 || uK<math>_{CMB}</math>|| Intensity
+
|EM_ML || Real*4 || cm^-6 pc || Emission measure posterior maximum   
 +
|-
 +
|EM_MEAN || Real*4 || cm^-6 pc || Emission measure posterior mean
 +
|-
 +
|EM_RMS || Real*4 || cm^-6 pc || Emission measure posterior rms
 
|-
 
|-
−
|I_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation of intensity
+
|TEMP_ML || Real*4 || K || Electron temperature posterior maximum   
 
|-
 
|-
−
|Beta || Real*4 || || effective spectral index
+
|TEMP_MEAN || Real*4 || K || Electron temperature posterior mean
 
|-
 
|-
−
|B_stdev || Real*4 || || standard deviation on the effective spectral index
+
|TEMP_RMS || Real*4 || K || Electron temperature posterior rms
 
|}
 
|}
  
−
; Notes:
 
−
: Comment: The Intensity is normalized at 30 GHz
 
−
: Comment: The intensity was estimated during mixing matrix estimation
 
−
 
−
Below an example of the header.
 
−
<!--pre>
 
−
XTENSION= 'BINTABLE'          / binary table extension
 
−
BITPIX  =                    8 / 8-bit bytes
 
−
NAXIS  =                    2 / 2-dimensional binary table
 
−
NAXIS1  =                  16 / width of table in bytes
 
−
NAXIS2  =              786432 / number of rows in table
 
−
PCOUNT  =                    0 / size of special data area
 
−
GCOUNT  =                    1 / one data group (required keyword)
 
−
TFIELDS =                    4 / number of fields in each row
 
−
TTYPE1  = 'I      '          / label for field  1
 
−
TFORM1  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT1  = 'uK_CMB  '          / physical unit of field
 
−
TTYPE2  = 'I_stdev '          / label for field  2
 
−
TFORM2  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT2  = 'uK_CMB  '          / physical unit of field
 
−
TTYPE3  = 'Beta    '          / label for field  3
 
−
TFORM3  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT3  = 'none    '          / physical unit of field
 
−
TTYPE4  = 'B_stdev '          / label for field  4
 
−
TFORM4  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT4  = 'none    '          / physical unit of field
 
−
EXTNAME = 'COMP-MAP'
 
−
DATE    = '2013-02-13T13:26:14' / file creation date (YYYY-MM-DDThh:mm:ss UT)
 
−
CHECKSUM= 'QXaaRVZTQVaZQVYZ'  / HDU checksum updated 2013-02-13T13:26:14
 
−
DATASUM = '2752450756'        / data unit checksum updated 2013-02-13T13:26:14
 
−
COMMENT
 
−
COMMENT *** Planck params ***
 
−
COMMENT
 
−
PIXTYPE = 'HEALPIX '          / HEALPIX pixelisation
 
−
ORDERING= 'NESTED  '          / Pixel ordering scheme, either RING or NESTED
 
−
NSIDE  =                  256 / Resolution parameter for HEALPIX
 
−
FIRSTPIX=                    0 / First pixel # (0 based)
 
−
LASTPIX =              786431 / Last pixel # (0 based)
 
−
INDXSCHM= 'IMPLICIT'          / Indexing: IMPLICIT or EXPLICIT
 
−
COORDSYS= 'GALACTIC'
 
−
FILENAME= 'COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits'
 
−
COMMENT ---------------------------------------------------------------------
 
−
COMMENT The intensity is normalized at 30GHz
 
−
COMMENT The intensity was estimated during mixing matrix estimation
 
−
COMMENT Object:
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_mean.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_stddev.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_mean.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_stddev.fits
 
−
COMMENT ---------------------------------------------------------------------
 
−
END
 
−
</pre -->
 
−
 
−
=====Low frequency component at Nside 2048=====
 
  
−
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits
+
=====Spinning dust emission=====
  
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}}
 +
: Nside = 256
 +
: Angular resolution = 60 arcmin
  
−
: '''Name HDU -- COMP-MAP'''
+
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. 
  
−
The Fits extension is composed by the columns described below:
+
: Reference frequency: 22.8 GHz
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ FITS header
+
|+ HDU -- COMP-MAP-AME1
 
|-
 
|-
 +
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I || Real*8 || uK<math>_{CMB}</math>|| Intensity
+
|I_ML || Real*4 || uK_RJ || Primary amplitude posterior maximum   
 
|-
 
|-
−
|I_stdev || Real*8 || uK<math>_{CMB}</math> || standard deviation of intensity
+
|I_MEAN || Real*4 || uK_RJ || Primary amplitude posterior mean
 
|-
 
|-
−
|I_hr1 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 1
+
|I_RMS || Real*4 || uK_RJ || Primary amplitude posterior rms
 
|-
 
|-
−
|I_hr2 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 2
+
|FREQ_ML || Real*4 || GHz || Primary peak frequency posterior maximum   
 +
|-
 +
|FREQ_MEAN || Real*4 || GHz || Primary peak frequency posterior mean
 +
|-
 +
|FREQ_RMS || Real*4 || GHz || Primary peak frequency posterior rms
 
|}
 
|}
  
−
; Notes:
+
: Reference frequency: 41.0 GHz
−
: Comment: The intensity was computed after mixing matrix application
+
: Peak frequency: 33.35 GHz
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ Extension 1 -- COMP-MAP-AME2
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|I_ML || Real*4 || uK_RJ || Secondary amplitude posterior maximum   
 +
|-
 +
|I_MEAN || Real*4 || uK_RJ || Secondary amplitude posterior mean
 +
|-
 +
|I_RMS || Real*4 || uK_RJ || Secondary amplitude posterior rms
 +
|}
  
  
−
: '''Name HDU -- BeamWF'''
 
−
 
−
The Fits second extension is composed by the columns described below:
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ FITS header
+
|+ Extension 2 -- SPINNING-DUST-TEMP
 
|-
 
|-
 +
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|BeamWF || Real*4 || || beam profile
+
|nu  || Real*4 || GHz || Frequency   
 +
|-
 +
|j_nu/nH || Real*4 || Jy sr-1 cm2/H || spdust2 spectrum   
 
|}
 
|}
  
−
; Notes:
+
=====CO line emission=====
−
: Comment: Beam window function used in the Component separation process
 
  
−
Below an example of the header of the first and second extension respectively.
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}}
−
<!-- pre>
+
: Nside = 256
−
XTENSION= 'BINTABLE'          / binary table extension
+
: Angular resolution = 60 arcmin
−
BITPIX  =                    8 / 8-bit bytes
 
−
NAXIS  =                    2 / 2-dimensional binary table
 
−
NAXIS1  =                  32 / width of table in bytes
 
−
NAXIS2  =            50331648 / number of rows in table
 
−
PCOUNT  =                    0 / size of special data area
 
−
GCOUNT  =                    1 / one data group (required keyword)
 
−
TFIELDS =                    4 / number of fields in each row
 
−
TTYPE1  = 'I      '          / label for field  1
 
−
TFORM1  = 'D      '          / data format of field: 8-byte DOUBLE
 
−
TUNIT1  = 'uK_CMB  '          / physical unit of field
 
−
TTYPE2  = 'I_stdev '          / label for field  2
 
−
TFORM2  = 'D      '          / data format of field: 8-byte DOUBLE
 
−
TUNIT2  = 'uK_CMB  '          / physical unit of field
 
−
TTYPE3  = 'I_hr1  '          / label for field  3
 
−
TFORM3  = 'D      '          / data format of field: 8-byte DOUBLE
 
−
TUNIT3  = 'uK_CMB  '          / physical unit of field
 
−
TTYPE4  = 'I_hr2  '          / label for field  4
 
−
TFORM4  = 'D      '          / data format of field: 8-byte DOUBLE
 
−
TUNIT4  = 'uK_CMB  '          / physical unit of field
 
−
EXTNAME = 'COMP-MAP'
 
−
DATE    = '2013-02-15T17:12:04' / file creation date (YYYY-MM-DDThh:mm:ss UT)
 
−
CHECKSUM= 'dlA5ei24di94di94'  / HDU checksum updated 2013-02-15T17:12:13
 
−
DATASUM = '3117718572'        / data unit checksum updated 2013-02-15T17:12:13
 
−
COMMENT
 
−
COMMENT *** Planck params ***
 
−
COMMENT
 
−
PIXTYPE = 'HEALPIX '          / HEALPIX pixelisation
 
−
ORDERING= 'NESTED  '          / Pixel ordering scheme, either RING or NESTED
 
−
NSIDE  =                2048 / Resolution parameter for HEALPIX
 
−
FIRSTPIX=                    0 / First pixel # (0 based)
 
−
LASTPIX =            50331647 / Last pixel # (0 based)
 
−
INDXSCHM= 'IMPLICIT'          / Indexing: IMPLICIT or EXPLICIT
 
−
BAD_DATA=          -1.6375E+30
 
−
COORDSYS= 'GALACTIC'
 
−
FILENAME= 'COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits'
 
−
COMMENT ---------------------------------------------------------------------
 
−
COMMENT The intensity was computed after mixibg matrix application
 
−
COMMENT Objects used:
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_lowfreq.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary
 
−
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_lowfreq_stddev.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_lowfreq.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_lowfreq.fits
 
−
COMMENT ---------------------------------------------------------------------
 
−
END
 
−
</pre>
 
  
−
<pre>
+
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.  
−
XTENSION= 'BINTABLE'          / binary table extension
 
−
BITPIX  =                    8 / 8-bit bytes
 
−
NAXIS  =                    2 / 2-dimensional binary table
 
−
NAXIS1  =                    4 / width of table in bytes
 
−
NAXIS2  =                1501 / number of rows in table
 
−
PCOUNT  =                    0 / size of special data area
 
−
GCOUNT  =                    1 / one data group (required keyword)
 
−
TFIELDS =                    1 / number of fields in each row
 
−
TTYPE1  = 'BeamWF  '          / label for field  1
 
−
TFORM1  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT1  = 'none    '          / physical unit of field
 
−
EXTNAME = 'BeamWF  '
 
−
DATE    = '2013-02-15T17:12:17' / file creation date (YYYY-MM-DDThh:mm:ss UT)
 
−
CHECKSUM= '74GA849274E97499'  / HDU checksum updated 2013-02-15T17:12:17
 
−
DATASUM = '3098248385'        / data unit checksum updated 2013-02-15T17:12:17
 
−
COMMENT
 
−
COMMENT *** Planck params ***
 
−
COMMENT
 
−
MAX-LPOL=                1500 / Maximum L multipole
 
−
POLAR  =                    T / Polarization included (True/False)
 
−
BCROSS =                    T / Magnetic cross terms included (True/False)
 
−
COMMENT ---------------------------------------------------------------------
 
−
COMMENT The intensity was computed after mixing matrix application
 
−
COMMENT
 
−
COMMENT Objects used:
 
−
COMMENT
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary
 
−
COMMENT /dx9delta_beams/dx9_delta_v1_7b_lowfreq_beam.fits
 
−
COMMENT
 
−
COMMENT ---------------------------------------------------------------------
 
−
END
 
−
</pre -->
 
  
−
====Thermal dust====
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-co10
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|I_ML || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior maximum   
 +
|-
 +
|I_MEAN || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior mean
 +
|-
 +
|I_RMS || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior rms
 +
|}
  
−
=====Thermal dust component at Nside=256=====
 
−
 
−
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits
 
−
 
−
: '''Name HDU -- COMP-MAP'''
 
−
 
−
The Fits extension is composed by the columns described below:
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ FITS header
+
|+ Extension 1 -- COMP-MAP-co21
 
|-
 
|-
 +
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I || Real*4 || MJy/sr || Intensity
+
|I_ML || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior maximum   
 
|-
 
|-
−
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity
+
|I_MEAN || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior mean
 
|-
 
|-
−
|Em || Real*4 || || emissivity
+
|I_RMS || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior rms
 +
|}
 +
 
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ Extension 2 -- COMP-MAP-co32
 
|-
 
|-
−
|Em_stdev || Real*4 || || standard deviation on emissivity
+
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|T || Real*4 || uK<math>_{CMB}</math> || temperature
+
|I_ML || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior maximum   
 
|-
 
|-
−
|T_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation on temerature
+
|I_MEAN || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior mean
 +
|-
 +
|I_RMS || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior rms
 
|}
 
|}
  
−
; Notes:
+
=====94/100 GHz line emission=====
−
: Comment: The intensity is normalized at 353 GHz
 
  
−
Below an example of the header.
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-commander_0256_R2.00.fits}}
−
<!-- pre>
+
: Nside = 256
−
XTENSION= 'BINTABLE'          / binary table extension
+
: Angular resolution = 60 arcmin
−
BITPIX  =                    8 / 8-bit bytes
 
−
NAXIS  =                    2 / 2-dimensional binary table
 
−
NAXIS1  =                  24 / width of table in bytes
 
−
NAXIS2  =              786432 / number of rows in table
 
−
PCOUNT  =                    0 / size of special data area
 
−
GCOUNT  =                    1 / one data group (required keyword)
 
−
TFIELDS =                    6 / number of fields in each row
 
−
TTYPE1  = 'I      '          / label for field  1
 
−
TFORM1  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT1  = 'MJy/sr  '          / physical unit of field
 
−
TTYPE2  = 'I_stdev '          / label for field  2
 
−
TFORM2  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT2  = 'MJy/sr  '          / physical unit of field
 
−
TTYPE3  = 'Em      '          / label for field  3
 
−
TFORM3  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT3  = 'uK_CMB  '          / physical unit of field
 
−
TTYPE4  = 'Em_stdev'          / label for field  4
 
−
TFORM4  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT4  = 'none    '          / physical unit of field
 
−
TTYPE5  = 'T      '          / label for field  5
 
−
TFORM5  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT5  = 'uK_CMB  '          / physical unit of field
 
−
TTYPE6  = 'T_stdev '          / label for field  6
 
−
TFORM6  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT6  = 'uK_CMB  '          / physical unit of field
 
−
EXTNAME = 'COMP-MAP'
 
−
DATE    = '2013-02-13T13:31:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)
 
−
CHECKSUM= '9OAOJO7N9OANGO7N'  / HDU checksum updated 2013-02-13T13:31:15
 
−
DATASUM = '4139938263'        / data unit checksum updated 2013-02-13T13:31:15
 
−
COMMENT
 
−
COMMENT *** Planck params ***
 
−
COMMENT
 
−
PIXTYPE = 'HEALPIX '          / HEALPIX pixelisation
 
−
ORDERING= 'NESTED  '          / Pixel ordering scheme, either RING or NESTED
 
−
NSIDE  =                  256 / Resolution parameter for HEALPIX
 
−
FIRSTPIX=                    0 / First pixel # (0 based)
 
−
LASTPIX =              786431 / Last pixel # (0 based)
 
−
INDXSCHM= 'IMPLICIT'          / Indexing: IMPLICIT or EXPLICIT
 
−
COORDSYS= 'GALACTIC'
 
−
FILENAME= 'COM_CompMap_dust-commrul_0256_R1.00.fits'
 
−
COMMENT ---------------------------------------------------------------------
 
−
COMMENT The intensity is normalized at 353 GHz
 
−
COMMENT Object:
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_mean.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_stddev.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_mean.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_stddev.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_mean.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_stddev.fits
 
−
COMMENT ---------------------------------------------------------------------
 
−
END
 
−
</pre -->
 
  
−
=====Thermal dust component at Nside=2048=====
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-xline
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|I_ML || Real*4 || uK_cmb || Amplitude posterior maximum   
 +
|-
 +
|I_MEAN || Real*4 || uK_cmb || Amplitude posterior mean
 +
|-
 +
|I_RMS || Real*4 || uK_cmb || Amplitude posterior rms
 +
|}
  
−
File name: COM_CompMap_dust-commrul_2048_R1.00.fits
+
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.
  
 +
=====Thermal dust emission=====
  
−
: '''Name HDU -- COMP-MAP'''
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}}
 +
: Nside = 256
 +
: Angular resolution = 60 arcmin
  
−
The Fits extension is composed by the columns described below:
+
: Reference frequency: 545 GHz
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ FITS header
+
|+ HDU -- COMP-MAP-dust
 
|-
 
|-
 +
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I || Real*8 || MJy/sr || Intensity
+
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum   
 +
|-
 +
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean
 
|-
 
|-
−
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity
+
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms
 
|-
 
|-
−
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1
+
|TEMP_ML || Real*4 || K || Dust temperature posterior maximum   
 
|-
 
|-
−
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2
+
|TEMP_MEAN || Real*4 || K || Dust temperature posterior mean
 +
|-
 +
|TEMP_RMS || Real*4 || K || Dust temperature posterior rms
 +
|-
 +
|BETA_ML || Real*4 || NA || Emissivity index posterior maximum   
 +
|-
 +
|BETA_MEAN || Real*4 || NA || Emissivity index posterior mean
 +
|-
 +
|BETA_RMS || Real*4 || NA || Emissivity index posterior rms
 
|}
 
|}
  
 +
=====Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters=====
  
−
: '''Name HDU -- BeamWF'''
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SZ-commander_0256_R2.00.fits|link=COM_CompMap_SZ-commander_0256_R2.00.fits}}
 +
: Nside = 256
 +
: Angular resolution = 60 arcmin
  
−
The Fits second extension is composed by the columns described below:
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ FITS header
+
|+ HDU -- COMP-MAP-SZ
 
|-
 
|-
 +
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|BeamWF || Real*4 || || beam profile 
+
|Y_ML || Real*4 || y_SZ || Y parameter posterior maximum   
 +
|-
 +
|Y_MEAN || Real*4 || y_SZ || Y parameter posterior mean
 +
|-
 +
|Y_RMS || Real*4 || y_SZ || Y parameter posterior rms
 
|}
 
|}
  
−
; Notes:
+
===High-resolution temperature products===
−
: Comment: Beam window function used in the Component separation process
 
  
−
Below an example of the header of the first and second extension respectively.
+
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.
−
<!--  pre>
+
 
−
XTENSION= 'BINTABLE'          / binary table extension
+
====Inputs====
−
BITPIX  =                    8 / 8-bit bytes
 
−
NAXIS  =                    2 / 2-dimensional binary table
 
−
NAXIS1  =                  32 / width of table in bytes
 
−
NAXIS2  =            50331648 / number of rows in table
 
−
PCOUNT  =                    0 / size of special data area
 
−
GCOUNT  =                    1 / one data group (required keyword)
 
−
TFIELDS =                    4 / number of fields in each row
 
−
TTYPE1  = 'I      '          / label for field  1
 
−
TFORM1  = 'D      '          / data format of field: 8-byte DOUBLE
 
−
TUNIT1  = 'MJy/sr  '          / physical unit of field
 
−
TTYPE2  = 'I_stdev '          / label for field  2
 
−
TFORM2  = 'D      '          / data format of field: 8-byte DOUBLE
 
−
TUNIT2  = 'MJy/sr  '          / physical unit of field
 
−
TTYPE3  = 'I_hr1  '          / label for field  3
 
−
TFORM3  = 'D      '          / data format of field: 8-byte DOUBLE
 
−
TUNIT3  = 'MJy/sr  '          / physical unit of field
 
−
TTYPE4  = 'I_hr2  '          / label for field  4
 
−
TFORM4  = 'D      '          / data format of field: 8-byte DOUBLE
 
−
TUNIT4  = 'MJy/sr  '          / physical unit of field
 
−
EXTNAME = 'COMP-MAP'
 
−
DATE    = '2013-02-16T10:23:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)
 
−
CHECKSUM= '6k8A7i826i896i89'  / HDU checksum updated 2013-02-16T10:23:32
 
−
DATASUM = '3817117839'        / data unit checksum updated 2013-02-16T10:23:32
 
−
COMMENT
 
−
COMMENT *** Planck params ***
 
−
COMMENT
 
−
PIXTYPE = 'HEALPIX '          / HEALPIX pixelisation
 
−
ORDERING= 'NESTED  '          / Pixel ordering scheme, either RING or NESTED
 
−
NSIDE  =                2048 / Resolution parameter for HEALPIX
 
−
FIRSTPIX=                    0 / First pixel # (0 based)
 
−
LASTPIX =             50331647 / Last pixel # (0 based)
 
−
INDXSCHM= 'IMPLICIT'          / Indexing: IMPLICIT or EXPLICIT
 
−
BAD_DATA=         -1.6375E+30
 
−
COORDSYS= 'GALACTIC'
 
−
FILENAME= 'COM_CompMap_dust-commrul_2048_R1.00.fits'
 
−
COMMENT ---------------------------------------------------------------------
 
−
COMMENT Objects used:
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_dust_flux.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary
 
−
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_dust_stddev.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_dust_flux.fits
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru
 
−
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_dust_flux.fits
 
−
COMMENT ---------------------------------------------------------------------
 
−
END
 
−
</pre>
 
  
−
<pre>
+
The following data products are used for the low-resolution analysis:
−
XTENSION= 'BINTABLE'          / binary table extension
+
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
−
BITPIX  =                    8 / 8-bit bytes
+
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps
−
NAXIS  =                    2 / 2-dimensional binary table
+
* Full-mission 353 GHz detector set ds2 and detector 1 maps
−
NAXIS1  =                    4 / width of table in bytes
+
* Full-mission 545 GHz detector 2 and 4 maps
−
NAXIS2  =                3001 / number of rows in table
+
* Full-mission 857 GHz detector 2 map
−
PCOUNT  =                    0 / size of special data area
+
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.
−
GCOUNT  =                    1 / one data group (required keyword)
 
−
TFIELDS =                    1 / number of fields in each row
 
−
TTYPE1  = 'BeamWF  '          / label for field  1
 
−
TFORM1  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT1  = 'none    '          / physical unit of field
 
−
EXTNAME = 'BeamWF  '
 
−
DATE    = '2013-02-16T10:23:34' / file creation date (YYYY-MM-DDThh:mm:ss UT)
 
−
CHECKSUM= 'FBGWI9EWFAEWF7EW'  / HDU checksum updated 2013-02-16T10:23:34
 
−
DATASUM = '4096860189'        / data unit checksum updated 2013-02-16T10:23:34
 
−
COMMENT
 
−
COMMENT *** Planck params ***
 
−
COMMENT
 
−
MAX-LPOL=                3000 / Maximum L multipole
 
−
COMMENT ---------------------------------------------------------------------
 
−
COMMENT Beam window function used in the Component separation process
 
−
COMMENT
 
−
COMMENT Objects used:
 
−
COMMENT
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary
 
−
COMMENT /dx9delta_beams/dx9_delta_v1_7b_dust_beam.fits
 
−
COMMENT
 
−
COMMENT ---------------------------------------------------------------------
 
−
END
 
−
</pre -->
 
  
−
====Sky mask====
+
====Outputs====
  
−
File name: COM_CompMap_Mask-rulerminimal_2048.fits
+
=====CO J2->1 emission=====
  
−
; '''Name HDU -- COMP-MASK'''
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO21-commander_2048_R2.00.fits|link=COM_CompMap_CO21-commander_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 7.5 arcmin
  
−
The Fits extension is composed by the columns described below:
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ FITS header
+
|+ HDU -- COMP-MAP-CO21
 
|-
 
|-
 +
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|Mask || Real*4 || || Mask
+
|I_ML_FULL || Real*4 || K_RJ km/s || Full-mission amplitude posterior maximum   
 +
|-
 +
|I_ML_HM1 || Real*4 || K_RJ km/s || First half-mission amplitude posterior maximum   
 +
|-
 +
|I_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission amplitude posterior maximum   
 +
|-
 +
|I_ML_HR1 || Real*4 || K_RJ km/s || First half-ring amplitude posterior maximum   
 +
|-
 +
|I_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring amplitude posterior maximum   
 +
|-
 +
|I_ML_YR1 || Real*4 || K_RJ km/s || "First year" amplitude posterior maximum   
 +
|-
 +
|I_ML_YR2 || Real*4 || K_RJ km/s || "Second year" amplitude posterior maximum   
 
|}
 
|}
  
−
Below an example of the header.
 
−
<!-- pre>
 
−
XTENSION= 'BINTABLE'          / binary table extension
 
−
BITPIX  =                    8 / 8-bit bytes
 
−
NAXIS  =                    2 / 2-dimensional binary table
 
−
NAXIS1  =                    4 / width of table in bytes
 
−
NAXIS2  =            50331648 / number of rows in table
 
−
PCOUNT  =                    0 / size of special data area
 
−
GCOUNT  =                    1 / one data group (required keyword)
 
−
TFIELDS =                    1 / number of fields in each row
 
−
TTYPE1  = 'Mask    '          / label for field  1
 
−
TFORM1  = 'E      '          / data format of field: 4-byte REAL
 
−
TUNIT1  = 'none    '          / physical unit of field
 
−
EXTNAME = 'COMP-MAP'
 
−
DATE    = '2013-02-16T21:07:43' / file creation date (YYYY-MM-DDThh:mm:ss UT)
 
−
CHECKSUM= '5fQAAeQ45eQAAeQ3'  / HDU checksum updated 2013-02-16T21:07:44
 
−
DATASUM = '1075621420'        / data unit checksum updated 2013-02-16T21:07:44
 
−
COMMENT
 
−
COMMENT *** Planck params ***
 
−
COMMENT
 
−
PIXTYPE = 'HEALPIX '          / HEALPIX pixelisation
 
−
ORDERING= 'NESTED  '          / Pixel ordering scheme, either RING or NESTED
 
−
NSIDE  =                2048 / Resolution parameter for HEALPIX
 
−
FIRSTPIX=                    0 / First pixel # (0 based)
 
−
LASTPIX =            50331647 / Last pixel # (0 based)
 
−
INDXSCHM= 'IMPLICIT'          / Indexing: IMPLICIT or EXPLICIT
 
−
OBJECT  = 'FULLSKY '          / Sky coverage, either FULLSKY or PARTIAL
 
−
BAD_DATA=          -1.6375E+30
 
−
COORDSYS= 'GALACTIC'
 
−
FILENAME= 'COM_CompMap_Mask-rulerminimal_2048.fits'
 
−
COMMENT ---------------------------------------------------------------------
 
−
COMMENT Objects used:
 
−
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary
 
−
COMMENT /dx9delta_masks/deltadx9_ruler_mask_total_minimal.fits
 
−
COMMENT ---------------------------------------------------------------------
 
−
END
 
−
</pre -->
 
  
−
== Dust optical depth map and model ==
+
=====Thermal dust emission=====
  
−
Thermal emission from interstellar dust is captured by Planck-HFI over the whole sky, at all frequencies from 100 to 857 GHz. This emission is well modelled by a modified black body in the far-infrared to millimeter range. It is produced by the biggest interstellar dust grain that are in thermal equilibrium with the radiation field from stars. The grains emission properties in the sub-millimeter are therefore directly linked to their absorption properties in the UV-visible range. By modelling the thermal dust emission in the sub-millimeter, a map of dust reddening in the visible can then be constructed.  
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_ThermalDust-commander_2048_R2.00.fits|link=COM_CompMap_ThermalDust-commander_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 7.5 arcmin
  
−
; Model of thermal dust emission
+
: Reference frequency: 545 GHz
−
 
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
The model of the thermal dust emission is based on a modify black body fit to the data $I_\nu$
+
|+ HDU -- COMP-MAP-dust
−
 
+
|-
−
$I_\nu = A\, B_\nu(T)\, \nu^\beta$
 
−
 
 
−
where B_nu(T) is the Planck function for dust equilibirum temperature T, A is the amplitude of the MBB and beta the dust spectral index. The dust optical depth at frequency nu is
 
−
 
 
−
$\tau_\nu = I_\nu / B_\nu(T) = A\, \nu^\beta$
 
−
 
 
−
The dust parameters provided are $T$, beta and $\tau_{353}$. They were obtained by fitting the Planck data at 353, 545 and 857 GHz together with the IRAS (IRIS) 100 micron data. All maps (in Healpix nside=2048) were smoothed to a common resolution of 5 arcmin. The CMB anisotropies, clearly visible at 353 GHz, were removed from all the HFI maps using the SMICA map.  An offset was removed from each map to obtained a meaningful Galactic zero level, using a correlation with the LAB 21 cm data in diffuse areas of the sky ($N_{HI} < 2\times10^{20} cm^{-2}$). Because the dust emission is so well correlated between frequencies in the Rayleigh-Jeans part of the dust spectrum, the zero level of the 545 and 353 GHz were improved by correlating with the 857 GHz over a larger mask ($N_{HI} < 3\times10^{20} cm^{-2}$). Faint residual dipole structures, identified in the 353 and 545 GHz maps, were removed prior to the fit.
 
−
 
 
−
The MBB fit was performed using a chi-square minimization, assuming errors for each data point that include instrumental noise, calibration uncertainties (on both the dust emission and the CMB anisotropies) and uncertainties on the zero level. Because of the known degeneracy between $T$ and $\beta$ in the presence of noise, we produced a model of dust emission using data smoothed to 35 arcmin; at such resolution no systematic bias of the parameters is observed. The map of the spectral index $\beta$ at 35 arcmin was than used to fit the data for $T$ and $\tau_{353}$ at 5 arcmin.
 
−
 
 
−
; The $E(B-V)$ map
 
−
For the production of the $E(B-V)$ map, we used Planck and IRAS data from which point sources in diffuse areas were removed to avoid contamination by galaxies.  In the hypothesis of constant dust emission cross-section, the optical depth map $\tau_{353}$ is proportional to dust column density. It can then be used to estimate E(B-V), also proportional to dust column density in the hypothesis of a constant differential absorption cross-section between the B and V bands. Given those assumptions, $ E(B-V) = q\, \tau_{353}$.
 
−
 
 
−
To estimate the calibration factor q, we followed a method similar to <cite>#mortsell2013</cite> based on SDSS reddening measurements ($E(g-r)$ which corresponds closely to $E(B-V)$) of 77 429 Quasars <cite>#schneider2007</cite>. The interstellar HI column densities covered on the lines of sight of this sample ranges from $0.5$ to $10\times10^{20}\,cm^{-2}$. Therefore this sample allows to estimate q in the diffuse ISM where dust properties are expected to vary less than in denser clouds where coagulation and grain growth might modify dust emission and absorption cross sections.
 
−
 
 
−
; Dust optical depth products
 
−
 
 
−
The characteristics of the dust model maps are the following.
 
−
* Dust optical depth at 353 GHz : nside=2048, fwhm=5 arcmin, no units
 
−
* Dust reddening E(B-V) : Nside=2048, fwhm=5 arcmin, units=magnitude, obtained with data from which point sources were removed.
 
−
* Dust temperature : nside 2048, fwhm=5 arcmin, units=Kelvin
 
−
* Dust spectral index : Nside=2048, fwhm=35 arcmin, no units
 
−
 
 
−
 
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 
−
|+ '''Dust opacity file data structure'''
 
−
|- bgcolor="ffdead" 
 
−
! colspan="4" | 1. EXTNAME = 'COMP-MAP'
 
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
| TAU353 || Real*4 || none || The opacity at 353GHz
+
|I_ML_FULL || Real*4 || uK_RJ || Full-mission amplitude posterior maximum   
−
|-
 
−
| TAU353ERR || Real*4 || none || Error in the opacity
 
 
|-
 
|-
−
| EBV || Real*4 || mag || E(B-V)
+
|I_ML_HM1 || Real*4 || uK_RJ || First half-mission amplitude posterior maximum   
 
|-
 
|-
−
| EBV_ERR || Real*4 || mag || Error in E(B-V)
+
|I_ML_HM2 || Real*4 || uK_RJ || Second half-mission amplitude posterior maximum   
 
|-
 
|-
−
|T_HF || Real*4 || K || Temperature for the high frequency correction
+
|I_ML_HR1 || Real*4 || uK_RJ || First half-ring amplitude posterior maximum   
 
|-
 
|-
−
|T_HF_ERR || Real*4 || K || Error on the temperature
+
|I_ML_HR2 || Real*4 || uK_RJ || Second half-ring amplitude posterior maximum   
 
|-
 
|-
−
| BETAHF || Real*4 || none || Beta for the high frequency correction
+
|I_ML_YR1 || Real*4 || uK_RJ || "First year" amplitude posterior maximum   
 
|-
 
|-
−
| BETAHFERR || Real*4 || none || Error on beta
+
|I_ML_YR2 || Real*4 || uK_RJ || "Second year" amplitude posterior maximum   
 
|-
 
|-
−
|- bgcolor="ffdead" 
+
|BETA_ML_FULL || Real*4 || NA || Full-mission emissivity index posterior maximum   
−
! Keyword || Data Type || Value || Description
 
 
|-
 
|-
−
| AST-COMP || String || DUST-OPA|| Astrophysical compoment name
+
|BETA_ML_HM1 || Real*4 || NA || First half-mission emissivity index posterior maximum   
 
|-
 
|-
−
| PIXTYPE || String || HEALPIX ||
+
|BETA_ML_HM2 || Real*4 || NA || Second half-mission emissivity index posterior maximum   
 
|-
 
|-
−
| COORDSYS || String || GALACTIC ||Coordinate system
+
|BETA_ML_HR1 || Real*4 || NA || First half-ring emissivity index posterior maximum   
 
|-
 
|-
−
| ORDERING || String || NESTED  || Healpix ordering
+
|BETA_ML_HR2 || Real*4 || NA || Second half-ring emissivity index posterior maximum   
 
|-
 
|-
−
| NSIDE  ||   Int || 2048 || Healpix Nside for LFI and HFI, respectively
+
|BETA_ML_YR1 || Real*4 || NA || "First year" emissivity index posterior maximum   
 
|-
 
|-
−
| FIRSTPIX ||   Int*4 ||           0 || First pixel number
+
|BETA_ML_YR2 || Real*4 || NA || "Second year" emissivity index posterior maximum   
 
|-
 
|-
−
| LASTPIX ||  Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively
 
 
|}
 
|}
  
−
== CO emission maps ==
+
===Polarization products===
  
−
CO rotational transition line emission is present in all HFI bands but for the 143 GHz channel. It is especially significant in the 100, 217 and 353 GHz channels (due to the 115 (1-0), 230 (2-1) and 345 GHz (3-2) CO transitions). This emission comes essentially from the Galactic interstellar medium and is mainly located at low and intermediate Galactic latitudes. Three approaches (summarised below) have been used to extract CO velocity-integrated emission maps from HFI maps and to make three types of CO products. An introduction is given in [[Science#CO_maps|Section]] and a full description of these products is given in <cite>#planck2013-p03a</cite>.
+
Two polarization foreground products are provided, namely synchrotron and thermal dust emission. The spectral models are assumed identical to the corresponding temperature spectral models.
−
* Type 1 product: it is based on a single channel approach using the fact that each CO line has a slightly different transmission in each bolometer at a given frequency channel. These transmissions can be evaluated from bandpass measurements that were performed on the ground or empirically determined from the sky using existing ground-based CO surveys. From these, the J=1-0, J=2-1 and J=3-2 CO lines can be extracted independently. As this approach is based on individual bolometer maps of a single channel, the resulting Signal-to-Noise ratio (SNR) is relatively low. The benefit, however, is that these maps do not suffer from contamination from other HFI channels (as is the case for the other approaches) and are more reliable, especially in the Galactic Plane.
 
  
−
* Type 2 product: this product is obtained using a multi frequency approach. Three frequency channel maps are combined to extract the J=1-0 (using the 100, 143 and 353 GHz channels) and J=2-1 (using the 143, 217 and 353 GHz channels) CO maps. Because frequency channels are combined, the spectral behaviour of other foregrounds influences the result. The two type 2 CO maps produced in this way have a higher SNR than the type 1 maps at the cost of a larger possible residual contamination from other diffuse foregrounds.
+
====Inputs====
  
−
* Type 3 product: using prior information on CO line ratios and a multi-frequency component separation method, we construct a combined CO emission map with the largest possible SNR. This type 3 product can be used as a sensitive finder chart for low-intensity diffuse CO emission over the whole sky.
+
The following data products are used for the polarization analysis:
 +
* (Only low-resolution analysis) Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}
 +
* (Only low-resolution analysis) Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}
 +
* (Only low-resolution analysis) Full-mission 70 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=70|period=Full|link=LFI 70 GHz frequency maps}}
 +
* Full-mission 100 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=100|period=Full|link=HFI 100 GHz frequency maps}}
 +
* Full-mission 143 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=143|period=Full|link=HFI 143 GHz frequency maps}}
 +
* Full-mission 217 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=217|period=Full|link=HFI 217 GHz frequency maps}}
 +
* Full-mission 353 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=353|period=Full|link=HFI 353 GHz frequency maps}}
 +
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.
  
−
The released Type 1 CO maps have been produced using the MILCA-b algorithm, Type 2 maps using a specific implementation of the Commander algorithm, and the Type 3 map using the full Commander-Ruler component separation pipeline (see [[Astrophysical_component_maps#Maps_of_astrophysical_foregrounds|above]]).
+
====Outputs====
 +
=====Synchrotron emission=====
  
−
Characteristics of the released maps are the following. We provide Healpix maps with Nside=2048. For one transition, the CO velocity-integrated line signal map is given in K_RJ.km/s units. A conversion factor from this unit to the native unit of HFI maps (K_CMB) is provided in the header of the data files and in the RIMO. Four maps are given per transition and per type:
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits|link=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits}}
−
* The signal map
+
: Nside = 256
−
* The standard deviation map (same unit as the signal),
+
: Angular resolution = 40 arcmin
−
* A null test noise map (same unit as the signal) with similar statistical properties. It is made out of half the difference of half-ring maps.
 
−
* A mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.
 
  
−
All products of a given type belong to a single file.
+
: Reference frequency: 30 GHz
−
Type 1 products have the native HFI resolution i.e. approximately 10, 5 and 5 arcminutes for the CO 1-0, 2-1, 3-2 transitions respectively.
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
Type 2 products have a 15 arcminute resolution
+
|+ HDU -- COMP-MAP-SynchrotronPol
−
The Type 3 product has a 5.5 arcminute resolution.
+
|-
−
 
 
−
 
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 
−
|+ '''Type-1 CO map file data structure'''
 
−
|- bgcolor="ffdead" 
 
−
!colspan="4" | 1. EXTNAME = 'COMP-MAP'
 
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map
+
|Q_ML_FULL || Real*4 || &mu;K_RJ || Full-mission Stokes Q posterior maximum   
 +
|-
 +
|U_ML_FULL || Real*4 || &mu;K_RJ || Full-mission Stokes U posterior maximum   
 
|-
 
|-
−
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity
+
|Q_ML_HM1 || Real*4 || &mu;K_RJ || First half-mission Stokes Q posterior maximum   
 
|-
 
|-
−
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|U_ML_HM1 || Real*4 || &mu;K_RJ || First half-mission Stokes U posterior maximum   
 
|-
 
|-
−
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable
+
|Q_ML_HM2 || Real*4 || &mu;K_RJ || Second half-mission Stokes Q posterior maximum   
 
|-
 
|-
−
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map
+
|U_ML_HM2 || Real*4 || &mu;K_RJ || Second half-mission Stokes U posterior maximum   
 
|-
 
|-
−
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity
+
|Q_ML_HR1 || Real*4 || &mu;K_RJ || First half-ring Stokes Q posterior maximum   
 
|-
 
|-
−
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|U_ML_HR1 || Real*4 || &mu;K_RJ || First half-ring Stokes U posterior maximum   
 
|-
 
|-
−
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable
+
|Q_ML_HR2 || Real*4 || &mu;K_RJ || Second half-ring Stokes Q posterior maximum   
 
|-
 
|-
−
|I32 || Real*4 || K_RJ km/sec || The CO(3-2) intensity map
+
|U_ML_HR2 || Real*4 || &mu;K_RJ || Second half-ring Stokes U posterior maximum   
 
|-
 
|-
−
|E32 || Real*4 || K_RJ km/sec || Uncertainty in the CO(3-2) intensity
+
|Q_ML_YR1 || Real*4 || &mu;K_RJ || "First year" Stokes Q posterior maximum   
 
|-
 
|-
−
|N32 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|U_ML_YR1 || Real*4 || &mu;K_RJ || "First year" Stokes U posterior maximum   
 
|-
 
|-
−
|M32 || Byte || none || Region over which the CO(3-2) intensity is considered reliable
+
|Q_ML_YR2 || Real*4 || &mu;K_RJ || "Second year" Stokes Q posterior maximum
 +
|-
 +
|U_ML_YR2 || Real*4 || &mu;K_RJ || "Second year" Stokes U posterior maximum     
 +
|}
 +
 
 +
=====Thermal dust emission=====
 +
 
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_DustPol-commander_1024_R2.00.fits|link=COM_CompMap_DustPol-commander_1024_R2.00.fits}}
 +
: Nside = 1024
 +
: Angular resolution = 10 arcmin
 +
 
 +
: Reference frequency: 353 GHz
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-DustPol
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
! Keyword || Data Type || Value || Description
+
! Column Name || Data Type || Units || Description
 +
|-
 +
|Q_ML_FULL || Real*4 || uK_RJ || Full-mission Stokes Q posterior maximum   
 +
|-
 +
|U_ML_FULL || Real*4 || uK_RJ || Full-mission Stokes U posterior maximum   
 +
|-
 +
|Q_ML_HM1 || Real*4 || uK_RJ || First half-mission Stokes Q posterior maximum   
 +
|-
 +
|U_ML_HM1 || Real*4 || uK_RJ || First half-mission Stokes U posterior maximum   
 
|-
 
|-
−
|AST-COMP || string || CO-TYPE2 || Astrophysical compoment name
+
|Q_ML_HM2 || Real*4 || uK_RJ || Second half-mission Stokes Q posterior maximum   
 
|-
 
|-
−
|PIXTYPE || String || HEALPIX ||
+
|U_ML_HM2 || Real*4 || uK_RJ || Second half-mission Stokes U posterior maximum   
 
|-
 
|-
−
|COORDSYS || String || GALACTIC ||Coordinate system
+
|Q_ML_HR1 || Real*4 || uK_RJ || First half-ring Stokes Q posterior maximum   
 
|-
 
|-
−
|ORDERING || String || NESTED  || Healpix ordering
+
|U_ML_HR1 || Real*4 || uK_RJ || First half-ring Stokes U posterior maximum   
 
|-
 
|-
−
|NSIDE  ||   Int || 2048 || Healpix Nside for LFI and HFI, respectively
+
|Q_ML_HR2 || Real*4 || uK_RJ || Second half-ring Stokes Q posterior maximum   
 
|-
 
|-
−
|FIRSTPIX ||   Int*4 ||                 0 || First pixel number
+
|U_ML_HR2 || Real*4 || uK_RJ || Second half-ring Stokes U posterior maximum   
 
|-
 
|-
−
|LASTPIX ||   Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively
+
|Q_ML_YR1 || Real*4 || uK_RJ || "First year" Stokes Q posterior maximum   
 
|-
 
|-
−
|CNV 1-0      || Real*4 ||     value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) 
+
|U_ML_YR1 || Real*4 || uK_RJ || "First year" Stokes U posterior maximum   
 
|-
 
|-
−
|CNV 2-1      || Real*4 ||     value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) 
+
|Q_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes Q posterior maximum
 
|-
 
|-
−
|CNV 3-2      || Real*4 ||     value || Factor to convert CO(3-2) intensityto Kcmb (units Kcmb/(Krj*km/s)) 
+
|U_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes U posterior maximum     
 
|}
 
|}
  
 +
=== Modelling of the thermal dust emission with the Draine and Li dust model ===
 +
 +
The Planck, IRAS, and WISE infrared observations were fit with the dust model presented by Draine & Li in 2007 (DL07).
 +
The input maps, the DL07 model, and the fitting procedure and results are presented in {{PlanckPapers|planck2014-XXIX}}.
 +
Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.
 +
 +
====Inputs====
 +
 +
The following data have been fit:
 +
 +
* WISE 12 micron map
 +
* IRAS 60 micron map
 +
* IRAS 100 micron map
 +
* Full-mission 353 GHz PR2 map
 +
* Full-mission 545 GHz PR2 map
 +
* Full-mission 857 GHz PR2 map
 +
 +
The CIB monopole, the CMB anisotropries and the zodiacal light were subtracted to obtain dust emission maps from the sky emission maps.
 +
All maps were smoothed to a common angular resolution of 5'.
 +
 +
====Model Parameters====
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
For each pixel of the inputs maps, we have fitted four parameters of the DL07 model:
−
|+ '''Type-2 CO map file data structure'''
+
 
−
|- bgcolor="ffdead" 
+
* the dust mass surface density, Sigma_Mdust,
−
!colspan="4" | 1. EXTNAME = 'COMP-MAP'
+
* the dust mass fraction in small PAH grains, q_PAH,
 +
* the fraction of the total luminosity from dust heated by intense radiation fields, f_PDR,
 +
* the starlight intensity heating the bulk of the dust, U_min.
 +
 
 +
The parameter maps and their uncertainties are gathered in one file. This file also includes the
 +
chi2 of the fit per degree of freedom.
 +
 
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 5 arcmin
 +
 
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-Dust-DL07-Parameters
 +
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map
+
|Sigma_Mdust || Real*4 || Solar masses/kpc^2 || Dust mass surface density
 
|-
 
|-
−
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity
+
|Sigma_Mdust_unc || Real*4 || Solar masses/kpc^2 || Uncertainty (1 sigma) on Sigma_Mdust
 
|-
 
|-
−
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|q_PAH || Real*4 || dimensionless || Dust mass fraction in small PAH grains   
 
|-
 
|-
−
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable
+
|q_PAH_unc || Real*4 || dimensionless || Uncertainty (1 sigma) on q_PAH
 
|-
 
|-
 +
|f_PDR || Real*4 || dimensionless || Fraction of the total luminosity from dust heated by intense radiation fields
 
|-
 
|-
−
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map
+
|f_PDR_unc || Real*4 || dimensionless || Uncertainty (1 sigma) on f_PDR
 
|-
 
|-
−
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity
+
|U_min || Real*4 || dimensionless || Starlight intensity heating the bulk of the dust   
 
|-
 
|-
−
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|U_min_unc || Real*4 || dimensionless || Uncertainty (1 sigma) on U_min
 
|-
 
|-
−
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable
+
|Chi2_DOF || Real*4 || dimensionless || Chi2 of the fit per degree of freedom
 +
|}
 +
 
 +
====Visible extinction maps====
 +
 
 +
We provide two exinctions maps at the visible V band: the value from the model (Av_DL) and the 
 +
renormalized one (Av_RQ) that matches extinction estimates for quasars (QSOs) derived from the Sloan digital sky survey (SDSS) data.
 +
 
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 5 arcmin
 +
 
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-Dust-DL07-AvMaps
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
! Keyword || Data Type || Value || Description
+
! Column Name || Data Type || Units || Description
 +
|-
 +
|Av_DL || Real*4 || magnitude || Extinction in the V band from the DL model
 +
|-
 +
|Av_DL_unc || Real*4 || magnitude || Uncertainty (1 sigma) on Av_DL
 
|-
 
|-
−
|AST-COMP || String || CO-TYPE2 || Astrophysical compoment name
+
|Av_RQ || Real*4 || magnitude || Extinction in the V band renormalized to match estimates from QSO SDSS observations 
 
|-
 
|-
−
|PIXTYPE || String || HEALPIX ||
+
|Av_RQ_unc || Real*4 || magnitude || Uncertainty (1 sigma) on Av_RQ
 +
|}
 +
 
 +
====Model Fluxes====
 +
 
 +
We provide the model predicted fluxes in the following file.
 +
 
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 5 arcmin
 +
 
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-Dust-DL07-ModelFluxes
 
|-
 
|-
−
|COORDSYS || String || GALACTIC ||Coordinate system
+
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|ORDERING || String || NESTED  || Healpix ordering
+
|Planck_857 || Real*4 || MJy/sr || Model flux in the Planck 857 GHz band
 
|-
 
|-
−
|NSIDE  ||   Int || 2048 || Healpix Nside for LFI and HFI, respectively
+
|Planck_545 || Real*4 || MJy/sr || Model flux in the Planck 545 GHz band   
 
|-
 
|-
−
|FIRSTPIX ||   Int*4 ||                 0 || First pixel number
+
|Planck_353 || Real*4 || MJy/sr || Model flux in the Planck 353 GHz band
 
|-
 
|-
−
|LASTPIX ||   Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively
+
|WISE_12 || Real*4 || MJy/sr || Model flux in the WISE 12 micron band   
 
|-
 
|-
−
|CNV 1-0      || Real*4 ||     value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) 
+
|IRAS_60 || Real*4 || MJy/sr || Model flux in the IRAS 60 micron band   
 
|-
 
|-
−
|CNV 2-1      || Real*4 ||     value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) 
+
|IRAS_100 || Real*4 || MJy/sr || Model flux in the IRAS 100 micron band   
 
|}
 
|}
  
 +
=== Thermal dust and CIB all-sky maps from GNILC component separation ===
 +
We describe diffuse foreground products for the Planck 2015 release produced with the GNILC component separation method. See the Planck paper {{PlanckPapers|planck2016-XLVIII}} for a detailed discussion on these products.
 +
 +
====Method====
 +
 +
: The basic idea behind the Generalized Needlet Internal Linear Combination (GNILC) component-separation method ([http://adsabs.harvard.edu/abs/2011MNRAS.418..467R  Remazeilles et al, MNRAS 2011]) is to disentangle specific components of emission not on the sole basis of the spectral (frequency) information but also on the basis of their distinct spatial information (angular power spectrum). The GNILC method has been applied to Planck data in order to disentangle Galactic dust emission and Cosmic Infrared Background (CIB) anisotropies. Both components have a similar spectral signature but a distinct angular power spectrum (spatial signature). The spatial information used by GNILC is under the form of priors for the angular power spectra of the CIB, the CMB, and the instrumental noise. No assumption is made on the Galactic signal, neither spectral or spatial. In that sense, GNILC is a blind component-separation method. GNILC operates on a needlet (spherical wavelet) frame, therefore adapting the component separation to the local conditions of contamination both over the sky and over the angular scales.
 +
 +
====Data====
 +
 +
: The data used by GNILC for the analysis are the Planck data release 2 (PR2) frequency maps from 30 to 857 GHz, and a 100 micron hybrid map combined from the SFD map ([http://adsabs.harvard.edu/abs/1998ApJ...500..525S  Schlegel et al, ApJ 1998]) at large angular scales (> 30') and the IRIS map ([http://adsabs.harvard.edu/abs/2005ApJS..157..302M  Miville-Deschênes et al, ApJS 2005]) at small angular scales (< 30'). This special 100 micron map can be obtained in the External Maps section of the PLA.
 +
 +
====Pre-processing====
 +
 +
: The point-sources with a signal-to-noise ratio, S/N > 5, in each individual frequency map (30 to 857 GHz, and 100 micron) have been pre-processed by a minimum curvature surface inpainting technique ([http://adsabs.harvard.edu/abs/2015MNRAS.451.4311R  Remazeilles et al, MNRAS 2015]) prior to performing component separation with GNILC.
 +
 +
====GNILC thermal dust and CIB products====
 +
 +
The result of GNILC component separation are thermal dust and CIB maps at 353, 545, and 857 GHz. In addition, by fitting a modified blackbody model to the GNILC thermal dust products at 353, 545, 857, and 100 micron, we have created all-sky maps of the dust optical depth, dust temperature, and dust emmissivity index. Note that the thermal dust maps have a variable angular resolution over the sky with an effective beam FWHM varying from 21.8' to 5'. The dust beam FWHM map is also released as a product.
 +
 +
=====Thermal dust maps=====
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ '''Type-3 CO map file data structure'''
+
|+ HDU -- COMP-MAP-DUST
−
|- bgcolor="ffdead" 
+
|-
−
!colspan="4" | 1. EXTNAME = 'COMP-MAP'
 
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
! Column Name || Data Type || Units || Description
+
! File Name || Nside || Units || Reference frequency || Angular resolution || Description
 
|-
 
|-
−
|INTEN || Real*4 || K_RJ km/sec || The CO intensity map
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F353_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F353_2048_R2.00.fits}} || 2048 || MJy/sr || 353 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}}  || Thermal dust amplitude at 353 GHz
 
|-
 
|-
−
|ERR || Real*4 || K_RJ km/sec || Uncertainty in the intensity
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F545_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F545_2048_R2.00.fits}} || 2048 || MJy/sr || 545 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}}  || Thermal dust amplitude at 545 GHz
 
|-
 
|-
−
|NUL || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F857_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F857_2048_R2.00.fits}} || 2048 || MJy/sr || 857 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}}  || Thermal dust amplitude at 857 GHz
 
|-
 
|-
−
|MASK || Byte || none || Region over which the intensity is considered reliable
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.00.fits}} || 2048 || NA || 353 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}}  || Thermal dust optical depth at 353 GHz
 
|-
 
|-
−
|- bgcolor="ffdead" 
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.00.fits}} || 2048 || NA || NA || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}}  || Thermal dust emissivity index
−
! Keyword || Data Type || Value || Description
 
 
|-
 
|-
−
|AST-COMP || String || CO-TYPE1 || Astrophysical compoment name
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.00.fits}} || 2048 || K || NA || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}}  || Thermal dust temperature
 
|-
 
|-
−
|PIXTYPE || String || HEALPIX ||
+
|[http://pla.esac.esa.int/pla/aio/product-action?DOCUMENT_MAP.DOCUMENT_ID=COM_DocMap_Dust-GNILC-Beam-FWHM_R2.00.fits COM_DocMap_Dust-GNILC-Beam-FWHM_R2.00.fits] || 128 || Arcminute || NA || NA || Effective dust beam FWHM
 
|-
 
|-
−
|COORDSYS || String || GALACTIC ||Coordinate system
+
|}
 +
 
 +
=====CIB maps=====
 +
 
 +
 
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-CIB
 
|-
 
|-
−
|ORDERING || String || NESTED  || Healpix ordering
+
|- bgcolor="ffdead" 
 +
! File Name || Nside || Units || Reference frequency || Angular resolution || Description
 
|-
 
|-
−
|NSIDE  ||   Int || 2048 || Healpix Nside for LFI and HFI, respectively
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F353_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F353_2048_R2.00.fits}} || 2048 || MJy/sr || 353 GHz || 5 arcmin || CIB amplitude at 353 GHz
 
|-
 
|-
−
|FIRSTPIX ||   Int*4 ||                 0 || First pixel number
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F545_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F545_2048_R2.00.fits}} || 2048 || MJy/sr || 545 GHz || 5 arcmin || CIB amplitude at 545 GHz
 
|-
 
|-
−
|LASTPIX ||   Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F857_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F857_2048_R2.00.fits}} || 2048 || MJy/sr || 857 GHz || 5 arcmin || CIB amplitude at 857 GHz
 
|-
 
|-
−
|CNV      ||  Real*4 ||    value || Factor to convert to Kcmb (units Kcmb/(Krj*km/s)) 
 
 
|}
 
|}
  
 +
 +
== References ==
 +
<References />
 +
 +
  
  
−
== References ==
+
 
−
<biblio force=false>
+
 
−
#[[References]]
+
[[Category:Mission products|007]]
−
</biblio>
 
−
[[Category:Mission science products|007]]
 

Latest revision as of 08:15, 21 August 2016


Overview[edit]

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 each product and how it is obtained, followed by a description of the FITS file containing the data and associated information. All the details can be found in Planck-2015-A09[1] and Planck-2015-A10[2].

CMB maps[edit]

CMB maps have been produced using four different methods: COMMANDER, NILC, SEVEM, and SMICA, as described in the CMB and foreground separation section and also in Appendices A-D of Planck-2015-A09[1] and references therein.

As discussed extensively in Planck-2015-A01[3], Planck-2015-A06[4], Planck-2015-A08[5], and Planck-2015-A09[1], the residual systematics in the Planck 2015 polarization maps have been dramatically reduced compared to 2013, by as much as two orders of magnitude on large angular scales. Nevertheless, on angular scales greater than 10 degrees, correponding to l < 20, systematics are still non-negligible compared to the expected cosmological signal.

It was not possible, for this data release, to fully characterize the large-scale residuals from the data or from simulations. Therefore all results published by the Planck Collaboration in 2015 which are based on CMB polarization have used maps which have been high-pass filtered to remove the large angular scales. We warn all users of the CMB polarization maps that they cannot yet be used for cosmological studies at large angular scales.

For convenience, we provide as default polarized CMB maps from which all angular scales at l < 30 have been filtered out.

For each method we provide the following:

  • Full-mission CMB intensity map, confidence mask and beam transfer function.
  • Full-mission CMB polarisation map,
  • A confidence mask.
  • A beam transfer function.

In addition, and for characterisation purposes, we include six other sets of maps from three data splits: first/second half-ring, odd/even years and first/second half-mission. For the year-1,2 and half-mission-1,2 data splits we provide half-sum and half-difference maps which are produced by running the corresponding sums and differences inputs through the pipelines. The half-difference maps can be used to provide an approximate noise estimates 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 Kcmb.

In addition, for each method we provide three sets of files, each categorized by the "R2.0X" label as follows:

R2.02
 This set of intensity and polarisation maps are provided at a resolution of Nside=1024. The Stokes Q and U maps are high-pass filtered to contain only modes above l > 30, as explained above and as used for analysis by the Planck Collaboration; THESE ARE THE POLARISATION MAPS WHICH SHOULD BE USED FOR COSMOLOGICAL ANALYSIS. Each type of map is packaged into a separate fits file (as for "R2.01"), resulting in file sizes which are easier to download (as opposed to the "R2.00" files), and more convenient to use with commonly used analysis software.
R2.01
This is the most complete set of 2015 CMB maps, containing Intensity products at a resolution of Nside=2048, and both Intensity and Polarisation at resolution of Nside=1024. For polarisation (Q and U), they contain all angular resolution modes. WE CAUTION USERS ONCE AGAIN THAT THE STOKES Q AND U MAPS ARE NOT CONSIDERED USEABLE FOR COSMOLOGICAL ANALYSIS AT l < 30. The structure of these files is the same as for "R2.02".
R2.00
 This set of files is equivalent to the "R2.01" set, but are packaged into only two large files. Warning: downloading these files could be very lengthy...

For a complete description of the above data structures, see below; the content of the first extensions is illustrated and commented in the table below.


The gallery below shows the Intensity, noise from half-mission, half-difference, and confidence mask for the four pipelines, in the order COMMANDER, NILC, SEVEM and SMICA, from top to bottom. The Intensity maps' scale is [–500.+500] μK, and the noise spans [–25,+25] μK. We do not show the Q and U maps since they have no significant visible structure to contemplate.

  • commander temperature

  • commander noise

  • commander mask

  • nilc temperature

  • nilc noise

  • nilc mask

  • sevem temperature

  • sevem noise

  • sevem mask

  • smica temperature

  • smica noise

  • smica mask

Product description[edit]

COMMANDER[edit]

Principle
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 Planck-2015-A10[2].
Resolution (effective beam)
The Commander sky maps have different angular resolutions depending on data products:
  • 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 Nside=256. The corresponding CMB map defines the input map for the low-l Planck 2015 temperature likelihood.
  • The Commander CMB temperature map derived from Planck-only observations has an angular resolution of ~5 arcmin and is pixelized at Nside=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.
  • The Commander CMB polarization map has an angular resolution of 10 arcmin and is pixelized at Nside=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.
Confidence mask
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 Planck-2015-A10[2]. 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.

NILC[edit]

Principle
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.
Resolution (effective beam)
The spectral analysis, and estimation of the NILC coefficients, is performed up to a maximum [math]\ell=4000[/math]. The effective beam is equivalent to a Gaussian circular beam with FWHM=5 arcminutes.
Confidence mask
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.


SEVEM[edit]

Principle
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.
Resolution
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).
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].
Confidence masks
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.
Foregrounds-subtracted maps[edit]

In addition to the regular CMB maps, SEVEM provides maps cleaned of the foregrounds for selected frequency channels (categorized as fgsub-sevem in the archive). In particular, for intensity there are clean CMB maps available at 100, 143 and 217 GHz, provided at the original resolution of the uncleaned channel and at Nside=2048. For polarization, there are Q/U clean CMB maps for the 70, 100 and 143 GHz (at Nside=1024). The 70 GHz clean map is provided at its original resolution, whereas the 100 and 143 GHz maps have a resolution given by a Gaussian beam with fwhm=10 arcminutes.

SMICA[edit]

Principle
SMICA produces CMB maps 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.
Resolution (effective beam)
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 [math]N_{side}[/math]=2048.
The SMICA Q and U maps are obtained similarly but are produced at [math]N_{side}[/math]=1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).
Confidence mask
A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel. See section below detailing the production process.


Common Masks[edit]

A number of common masks have been defined for analysis of the CMB temperature and polarization maps. They are based on the confidence masks provided by the component separation methods. One mask for temperature and one mask for polarization have been chosen as the preferred masks based on subsequent analyses.

The common masks for the CMB temperature maps are:

  • UT78: union of the Commander, SEVEM, and SMICA temperature confidence masks (the NILC mask was not included since it masks much less of the sky). It has fsky = 77.6%. This is the preferred mask for temperature.
  • UTA76: in addition to the UT78 mask, it masks pixels where standard deviation between the four CMB maps is greater than 10 μK. It has fsky = 76.1%.

The common masks for the CMB polarization maps are:

  • UP78: the union of the Commander, SEVEM and SMICA polarization confidence masks (the NILC mask was not included since it masks much less of the sky). It has fsky = 77.6%.
  • UPA77: In addition to the UP78 mask, it masks pixels where the standard deviation between the four CMB maps, averaged in Q and U, is greater than 4 μK. It has fsky = 76.7%.
  • UPB77: in addition to the UP78 mask, it masks polarized point sources detected in the frequency channel maps. It has fsky = 77.4%. This is the preferred mask for polarization.

CMB-subtracted frequency maps ("Foreground maps")[edit]

These are the full-sky, full-mission frequency maps in intensity from which the CMB has been subtracted. The maps contain foregrounds and noise. They are provided for each frequency channel and for each component separation method. They are grouped into 8 files, two for each method of which there is one for each instrument. The maps are are at Nside = 1024 for the three LFI channels and at Nside = 2048 for the six HFI channels. The filenames are:

  • LFI_Foregrounds-{method}_1024_Rn.nn.fits (145 MB each)
  • HFI_Foregrounds-{method}_2048_Rn.nn.fits (1.2 GB each)

To remove the CMB, the respective CMB map was first deconvolved with the 5 arcmin beam, then convolved with the beam of the frequency channel, and finally subtracted from the frequency map. This was done using the [math]B_\rm{l}[/math] in harmonic space, assuming a symmetric beam.

The CMB-subtracted maps have complicated noise properties. The CMB maps contain a noise contribution from each of the frequency maps, depending on the weights with which they were combined. Therefore subtracting the CMB map from a frequency channel contributes additional noise from the other frequency channels.

Quadrupole Residual Maps[edit]

The second-order (kinematic) quadrupole is a frequency-dependent effect. During the production of the frequency maps the frequency-independent part was subtracted, which leaves a frequency-dependent residual quadrupole. The residuals in the component-separated CMB temperature maps have been estimated by simulating the effect in the frequency maps and propagating it through the component separation pipelines. The residuals have an amplitude of around 2 μK peak-to-peak. The maps of the estimated residuals can be used to remove the effect by subtracting them from the CMB maps.

Production process[edit]

COMMANDER[edit]

Pre-processing
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.
Priors
The following priors are enforced in the Commander analysis:
  • 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
  • Monopoles and dipoles are fixed to nominal values for a small set of reference frequencies
  • Gaussian priors are enforced on spectral parameters, with values informed by the values derived in the high signal-to-noise areas of the sky
  • The Jeffreys ignorance prior is enforced on spectral parameters in addition to the informative Gaussian priors
Fitting procedure
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.

NILC[edit]

Pre-processing
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
Linear combination
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.
Post-processing
E and B maps are re-combined into Q and U products using standard HEALPix tools.

SEVEM[edit]

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] 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).

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, and these intermediate products (clean maps at individual frequencies for intensity and polarization) are also provided in the archive. 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.

Intensity

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.

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.

In addition, the clean CMB maps produced at 100, 143 and 217 GHz frequencies are also provided. The resolution of these maps is the same as that of the uncleaned frequency channels and have been constructed at Nside=2048. They have been inpainted at the position of the detected point sources. Note that these three clean maps should be close to independent, although some level of correlation will be present since the same templates have been used to clean the maps.

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.

Polarization

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 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 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 order to increase the signal-to-noise ratio of the template. 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. In this way, the 100 GHz 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.

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 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) to avoid the introduction of ringing around the Galactic centre in the filtering process.

The clean CMB maps at individual frequency channels produced as intermediate steps of SEVEM are also provided for Q and U, constructed at Nside=1024. The clean 70 GHz map is provided at its native resolution, while the clean maps at 100 and 143 GHz frequencies have a resolution of 10 arcminutes (Gaussian beam). The three maps have been inpainted in the positions of the detected point sources. Note that, due to the availability of a smaller number of templates for polarization than for intensity, these maps are less independent than for the temperature case, since, for instance, the 100 GHz map is used to clean the 143 GHz one and viceversa.

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.


SMICA[edit]

A) Production of the intensity map.

1) Pre-processing
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.
2) Linear combination
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.
3) Post-processing
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.


B) Production of the Q and U polarisation maps.

The SMICA pipeline for polarization uses all the 7 polarized Planck channels. The production of the Q and U maps is similar to the production of the intensity map. However, there is no input point source pre-processing of the input maps. The regions of very strong emission are masked out using an apodized mask before computing the E and B modes of the input maps and combining them to produce the E and B modes of the CMB map. Those 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.


Inputs[edit]

The input maps are the sky temperature maps described in the 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.

File names and structure[edit]

Three sets of files FITS files containing the CMB products are available. In the first set all maps (i.e., covering different parts of the mission) and all characterisation products for a given method and a given Stokes parameter are grouped into a single extension, and there are two files per method (smica, nilc, sevem, and commander), one for the high resolution data (I only, Nside=2048) and one for low resolution data (Q and U only, Nside=1024). Each file also contains the associated confidence mask(s) and beam transfer function. These are the R2.00 files which have names like

  • COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.00.fits

There are 7 coverage periods:full, halfyear-1,2, halfmission-1,2, or ringhalf-1,2, and 4 characterisation products: half-sum and half-difference for the year and the half-mission periods.

In the second second set the different coverages are split into different files which in most cases have a single extension with I only (Nside=1024) and I, Q, and U (Nside=1024). This second set was built in order to allow users to use standard codes like spice or anafast on them, directly. So this set contains the I maps at Nside=1024, which are not contained in the R2.00; on the other hand this set does not contain the half-sum and half-difference maps. These are the 2.01 files which have names like

  • COM_CMB_IQU-{method}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits for the regular CMB maps, and
  • COM_CMB_IQU-{fff}-{fgsub-sevem}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits for the sevem frequency-dependent, foregrounds-subtracted maps,

where field-Int|Pol is used to indicate that only Int or only Pol data are contained (at present only field-Int is used for the high-res data), and is not included in the low-res data which contains all three Stokes parameters, and coverage is one of full, halfyear-1,2, halfmission-1,2, or ringhalf-1,2. Also, the coverage=full files contain also the confidence mask(s) and beam transfer function(s) which are valid for all products of the same method (one for Int and one for Pol when both are available).

The third set has the same structure as the Nside=1024 products of R2.01, but the Q and U maps have been high-pass filtered to remove modes at l < 30 for the reasons indicated earlier. These are the default products for use in polarisation studies. They are the R2.02 files which have names like:

  • COM_CMB_IQU-{method}_1024_R2.02_{coverage}.fits

Version 2.00 files[edit]

These have names like

  • COM_CMB_IQU-{method}-field-{Int,Pol}_Nside_R2.00.fits,

as indicated above. They contain:

  • a minimal primary extension with no data;
  • 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.
  • a BINTABLE extension containing the beam transfer function (mistakenly called window function in the files).

If Nside=1024 the files contain I, Q and U maps, whereas if Nside=2048 only the I map is given.

CMB R2.00 map file data structure
Ext. 1. or 2. EXTNAME = COMP-MAP (BINTABLE)
Column Name Data Type Units Description
I or Q or U Real*4 uK_cmb I or Q or U map
HM1 Real*4 uK_cmb Half-miss 1
HM2 Real*4 uK_cmb Half-miss 2
YR1 Real*4 uK_cmb Year 1
YR2 Real*4 uK_cmb Year 2
HR1 Real*4 uK_cmb Half-ring 1
HR2 Real*4 uK_cmb Half-ring 2
HMHS Real*4 uK_cmb Half-miss, half sum
HMHD Real*4 uK_cmb Half-miss, half diff
YRHS Real*4 uK_cmb Year, half sum
YRHD Real*4 uK_cmb Year, half diff
HRHS Real*4 uK_cmb Half-ring half sum
HRHD Real*4 uK_cmb Half-ring half diff
MASK BYTE Confidence mask
Keyword Data Type Value Description
AST-COMP String CMB Astrophysical compoment name
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
POLCCONV String COSMO Polarization convention
ORDERING String NESTED Healpix ordering
NSIDE Int 1024 or 2048 Healpix Nside
METHOD String name Cleaning method (smica/nilc/sevem/commander)
Ext. 2. or 3. EXTNAME = BEAM_WF (BINTABLE) . See Note 1
Column Name Data Type Units Description
BEAMWF Real*4 none The effective beam transfer function, including the pixel window function. See Note 2.
Keyword Data Type Value Description
LMIN Int value First multipole of beam TF
LMAX Int value Last multipole of beam TF
METHOD String name Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)

Notes:

  1. Actually this is a beam transfer function, so BEAM_TF would have been more appropriate.
  2. The beam transfer 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]. The beam Window function is given by [math]W_\ell = B_\ell^2[/math]


Version 2.01 files[edit]

These files have names like:

  • COM_CMB_IQU-{method}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits for the regular CMB maps, and
  • COM_CMB_IQU-{fff}-{fgsub-sevem}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits for the sevem frequency-dependent, foregrounds-subtracted maps,

as indicated above. They contain:

  • a minimal primary extension with no data, but with a NUMEXT keyword giving the number of extensions contained.
  • one or two BINTABLE data extensions with a table of Npix lines by 1-5 columns depending on the file, as described above: the minimum begin I only, the maximum begin I, Q, U, and confidence masks for I and P.
  • a BINTABLE extension containing the beam transfer function(s): one for I, and a second one that applies to both Q and U, if Nslde=1024.

If Nside=1024 the files contain I, Q and U maps, whereas if Nside=2048 only the I map is given. The basic structure, including information on the most important keywords, is given in the table below. For full details, see the FITS header.

CMB R2.01 map file data structure
Ext. 1. or 2. EXTNAME = COMP-MAP (BINTABLE)
Column Name Data Type Units Description
I_Stokes Real*4 uK_cmb I map (Nside=1024,2048)
Q_Stokes Real*4 uK_cmb Q map (Nside=1024)
U_Stokes Real*4 uK_cmb U map (Nside=2048)
TMASK Int none optional Temperature confidence mask
PMASK Int none optional Polarisation confidence mask
Keyword Data Type Value Description
AST-COMP String CMB Astrophysical compoment name
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
POLCCONV String COSMO Polarization convention
ORDERING String NESTED Healpix ordering
NSIDE Int 1024 or 2048 Healpix Nside
METHOD String name Cleaning method (SMICA/NILC/SEVEM)
Optional Ext. 2. or 3. EXTNAME = BEAM_TF (BINTABLE)
Column Name Data Type Units Description
INT_BEAM Real*4 none Effective beam transfer function. See Note 1.
POL_BEAM Real*4 none Effective beam transfer function. See Note 1.
Keyword Data Type Value Description
LMIN Int value First multipole of beam WF
LMAX_I Int value Last multipole for Int beam TF
LMAX_P Int value Last multipole for Pol beam TF
METHOD String name Cleaning method

Notes:

  1. The beam transfer 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]. The beam Window function is given by [math]W_\ell = B_\ell^2[/math]

Version 2.02 files[edit]

For polarisation work, this is the default set of files to be used for cosmological analysis. Their content is identical to the "R2.01" files, except that angular scales above l < 30 have been filtered out of the Q and U maps.

These files have names like:

  • COM_CMB_IQU-{method}_1024_R2.02_{coverage}.fits

as indicated above. They contain: The files contain

  • a minimal primary extension with no data, but with a NUMEXT keyword giving the number of extensions contained.
  • one or two BINTABLE data extensions with a table of Npix lines by 1-5 columns depending on the file, as described above: the minimum begin I only, the maximum begin I, Q, U, and confidence masks for I and P.
  • a BINTABLE extension containing 2 beam transfer functions: one for I and one that applies to both Q and U.

If Nside=1024 the files contain I, Q and U maps, whereas if Nside=2048 only the I map is given. The basic structure, including information on the most important keywords, is given in the table below. For full details, see the FITS header.

CMB R2.02 map file data structure
Ext. 1. or 2. EXTNAME = COMP-MAP (BINTABLE)
Column Name Data Type Units Description
I_Stokes Real*4 uK_cmb I map (Nside=1024)
Q_Stokes Real*4 uK_cmb Q map (Nside=1024)
U_Stokes Real*4 uK_cmb U map (Nside=2048)
TMASK Int none optional Temperature confidence mask
PMASK Int none optional Polarisation confidence mask
Keyword Data Type Value Description
AST-COMP String CMB Astrophysical compoment name
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
POLCCONV String COSMO Polarization convention
ORDERING String NESTED Healpix ordering
NSIDE Int 1024 or 2048 Healpix Nside
METHOD String name Cleaning method (SMICA/NILC/SEVEM)
Optional Ext. 2. or 3. EXTNAME = BEAM_TF (BINTABLE)
Column Name Data Type Units Description
INT_BEAM Real*4 none Effective beam transfer function. See Note 1.
POL_BEAM Real*4 none Effective beam transfer function. See Note 1.
Keyword Data Type Value Description
LMIN Int value First multipole of beam WF
LMAX_I Int value Last multipole for Int beam TF
LMAX_P Int value Last multipole for Pol beam TF
METHOD String name Cleaning method

Notes:

  1. The beam transfer 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]. The beam Window function is given by [math]W_\ell = B_\ell^2[/math]

Common masks[edit]

The common masks are stored into two different files for Temperature and Polarisation respectively:

  • COM_CMB_IQU-common-field-MaskInt_2048_R2.nn.fits with the UT78 and UTA76 masks
  • COM_CMB_IQU-common-field-MaskPol_1024_R2.nn.fits with the UP78, UPA77, and UPB77 masks

Both files contain also a map of the missing pixels for the half mission and year coverage periods. The 2 (for Temp) or 3 (for Pol) masks and the missing pixels maps are stored in 4 or 5 column a BINTABLE extension 1 of each file, named MASK-INT and MASK-POL, respectively. See the FITS file headers for details.

Quadrupole residual maps[edit]

The quadrupole residual maps are stored in files called:

  • COM_CMB_IQU-kq-resid-{method}-field-Int_2048_R2.02.fits

They contain:

  • a minimal primary extension with no data, but with a NUMEXT keyword giving the number of extensions contained.
  • a single BINTABLE extension with a single column of Npix lines containing the HEALPIX map indicated

The basic structure of the data extension is shown below. For full details see the extension header.

Kinetic quadrupole residual map file data structure
Ext. 1. EXTNAME = COMP-MAP (BINTABLE)
Column Name Data Type Units Description
INTENSITY Real*4 K_cmb the residual map
Keyword Data Type Value Description
AST-COMP String KQ-RESID Astrophysical compoment name
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
POLCCONV String COSMO Polarization convention
ORDERING String NESTED Healpix ordering
NSIDE Int 2048 Healpix Nside
METHOD String name Cleaning method

Astrophysical foregrounds from parametric component separation[edit]

We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper Planck-2015-A10[2] for a detailed description of these products. Further scientific discussion and interpretation may be found in Planck-2015-A25[6].

Low-resolution temperature products[edit]

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.

Inputs[edit]

The following data products are used for the low-resolution analysis:

  • Full-mission 30 GHz frequency map, LFI 30 GHz frequency maps
  • Full-mission 44 GHz frequency map, LFI 44 GHz frequency maps
  • Full-mission 70 GHz ds1 (18+23), ds2 (19+22), and ds3 (20+21) detector-set maps
  • Full-mission 100 GHz ds1 and ds2 detector set maps
  • Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
  • Full-mission 217 GHz detector 1, 2, 3 and 4 maps
  • Full-mission 353 GHz detector set ds2 and detector 1 maps
  • Full-mission 545 GHz detector 2 and 4 maps
  • Full-mission 857 GHz detector 2 map
  • Beam-symmetrized 9-year WMAP K-band map (Lambda)
  • Beam-symmetrized 9-year WMAP Ka-band map (Lambda)
  • Default 9-year WMAP Q1 and Q2 differencing assembly maps (Lambda)
  • Default 9-year WMAP V1 and V2 differencing assembly maps (Lambda)
  • Default 9-year WMAP W1, W2, W3, and W4 differencing assembly maps (Lambda)
  • Re-processed 408 MHz survey map, Remazeilles et al. (2014) (Lambda)

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.

Outputs[edit]

Synchrotron emission[edit]
File name: COM_CompMap_Synchrotron-commander_0256_R2.00.fits
Reference frequency: 408 MHz
Nside = 256
Angular resolution = 60 arcmin
HDU -- COMP-MAP-Synchrotron
Column Name Data Type Units Description
I_ML Real*4 uK_RJ Amplitude posterior maximum
I_MEAN Real*4 uK_RJ Amplitude posterior mean
I_RMS Real*4 uK_RJ Amplitude posterior rms


Extension 1 -- SYNC-TEMP
Column Name Data Type Units Description
nu Real*4 Hz Frequency
intensity Real*4 W/Hz/m2/sr GALPROP z10LMPD_SUNfE spectrum
Free-free emission[edit]
File name: COM_CompMap_freefree-commander_0256_R2.00.fits
Reference frequency: NA
Nside = 256
Angular resolution = 60 arcmin
HDU -- COMP-MAP-freefree
Column Name Data Type Units Description
EM_ML Real*4 cm^-6 pc Emission measure posterior maximum
EM_MEAN Real*4 cm^-6 pc Emission measure posterior mean
EM_RMS Real*4 cm^-6 pc Emission measure posterior rms
TEMP_ML Real*4 K Electron temperature posterior maximum
TEMP_MEAN Real*4 K Electron temperature posterior mean
TEMP_RMS Real*4 K Electron temperature posterior rms


Spinning dust emission[edit]
File name: COM_CompMap_AME-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin

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.

Reference frequency: 22.8 GHz
HDU -- COMP-MAP-AME1
Column Name Data Type Units Description
I_ML Real*4 uK_RJ Primary amplitude posterior maximum
I_MEAN Real*4 uK_RJ Primary amplitude posterior mean
I_RMS Real*4 uK_RJ Primary amplitude posterior rms
FREQ_ML Real*4 GHz Primary peak frequency posterior maximum
FREQ_MEAN Real*4 GHz Primary peak frequency posterior mean
FREQ_RMS Real*4 GHz Primary peak frequency posterior rms
Reference frequency: 41.0 GHz
Peak frequency: 33.35 GHz
Extension 1 -- COMP-MAP-AME2
Column Name Data Type Units Description
I_ML Real*4 uK_RJ Secondary amplitude posterior maximum
I_MEAN Real*4 uK_RJ Secondary amplitude posterior mean
I_RMS Real*4 uK_RJ Secondary amplitude posterior rms


Extension 2 -- SPINNING-DUST-TEMP
Column Name Data Type Units Description
nu Real*4 GHz Frequency
j_nu/nH Real*4 Jy sr-1 cm2/H spdust2 spectrum
CO line emission[edit]
File name: COM_CompMap_CO-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin

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.

HDU -- COMP-MAP-co10
Column Name Data Type Units Description
I_ML Real*4 K_RJ km/s CO(1-0) amplitude posterior maximum
I_MEAN Real*4 K_RJ km/s CO(1-0) amplitude posterior mean
I_RMS Real*4 K_RJ km/s CO(1-0) amplitude posterior rms
Extension 1 -- COMP-MAP-co21
Column Name Data Type Units Description
I_ML Real*4 K_RJ km/s CO(2-1) amplitude posterior maximum
I_MEAN Real*4 K_RJ km/s CO(2-1) amplitude posterior mean
I_RMS Real*4 K_RJ km/s CO(2-1) amplitude posterior rms
Extension 2 -- COMP-MAP-co32
Column Name Data Type Units Description
I_ML Real*4 K_RJ km/s CO(3-2) amplitude posterior maximum
I_MEAN Real*4 K_RJ km/s CO(3-2) amplitude posterior mean
I_RMS Real*4 K_RJ km/s CO(3-2) amplitude posterior rms
94/100 GHz line emission[edit]
File name: COM_CompMap_xline-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin
HDU -- COMP-MAP-xline
Column Name Data Type Units Description
I_ML Real*4 uK_cmb Amplitude posterior maximum
I_MEAN Real*4 uK_cmb Amplitude posterior mean
I_RMS Real*4 uK_cmb Amplitude posterior rms

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.

Thermal dust emission[edit]
File name: COM_CompMap_dust-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin
Reference frequency: 545 GHz
HDU -- COMP-MAP-dust
Column Name Data Type Units Description
I_ML Real*4 uK_RJ Amplitude posterior maximum
I_MEAN Real*4 uK_RJ Amplitude posterior mean
I_RMS Real*4 uK_RJ Amplitude posterior rms
TEMP_ML Real*4 K Dust temperature posterior maximum
TEMP_MEAN Real*4 K Dust temperature posterior mean
TEMP_RMS Real*4 K Dust temperature posterior rms
BETA_ML Real*4 NA Emissivity index posterior maximum
BETA_MEAN Real*4 NA Emissivity index posterior mean
BETA_RMS Real*4 NA Emissivity index posterior rms
Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters[edit]
File name: COM_CompMap_SZ-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin
HDU -- COMP-MAP-SZ
Column Name Data Type Units Description
Y_ML Real*4 y_SZ Y parameter posterior maximum
Y_MEAN Real*4 y_SZ Y parameter posterior mean
Y_RMS Real*4 y_SZ Y parameter posterior rms

High-resolution temperature products[edit]

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.

Inputs[edit]

The following data products are used for the low-resolution analysis:

  • Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
  • Full-mission 217 GHz detector 1, 2, 3 and 4 maps
  • Full-mission 353 GHz detector set ds2 and detector 1 maps
  • Full-mission 545 GHz detector 2 and 4 maps
  • Full-mission 857 GHz detector 2 map

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.

Outputs[edit]

CO J2->1 emission[edit]
File name: COM_CompMap_CO21-commander_2048_R2.00.fits
Nside = 2048
Angular resolution = 7.5 arcmin
HDU -- COMP-MAP-CO21
Column Name Data Type Units Description
I_ML_FULL Real*4 K_RJ km/s Full-mission amplitude posterior maximum
I_ML_HM1 Real*4 K_RJ km/s First half-mission amplitude posterior maximum
I_ML_HM2 Real*4 K_RJ km/s Second half-mission amplitude posterior maximum
I_ML_HR1 Real*4 K_RJ km/s First half-ring amplitude posterior maximum
I_ML_HR2 Real*4 K_RJ km/s Second half-ring amplitude posterior maximum
I_ML_YR1 Real*4 K_RJ km/s "First year" amplitude posterior maximum
I_ML_YR2 Real*4 K_RJ km/s "Second year" amplitude posterior maximum


Thermal dust emission[edit]
File name: COM_CompMap_ThermalDust-commander_2048_R2.00.fits
Nside = 2048
Angular resolution = 7.5 arcmin
Reference frequency: 545 GHz
HDU -- COMP-MAP-dust
Column Name Data Type Units Description
I_ML_FULL Real*4 uK_RJ Full-mission amplitude posterior maximum
I_ML_HM1 Real*4 uK_RJ First half-mission amplitude posterior maximum
I_ML_HM2 Real*4 uK_RJ Second half-mission amplitude posterior maximum
I_ML_HR1 Real*4 uK_RJ First half-ring amplitude posterior maximum
I_ML_HR2 Real*4 uK_RJ Second half-ring amplitude posterior maximum
I_ML_YR1 Real*4 uK_RJ "First year" amplitude posterior maximum
I_ML_YR2 Real*4 uK_RJ "Second year" amplitude posterior maximum
BETA_ML_FULL Real*4 NA Full-mission emissivity index posterior maximum
BETA_ML_HM1 Real*4 NA First half-mission emissivity index posterior maximum
BETA_ML_HM2 Real*4 NA Second half-mission emissivity index posterior maximum
BETA_ML_HR1 Real*4 NA First half-ring emissivity index posterior maximum
BETA_ML_HR2 Real*4 NA Second half-ring emissivity index posterior maximum
BETA_ML_YR1 Real*4 NA "First year" emissivity index posterior maximum
BETA_ML_YR2 Real*4 NA "Second year" emissivity index posterior maximum

Polarization products[edit]

Two polarization foreground products are provided, namely synchrotron and thermal dust emission. The spectral models are assumed identical to the corresponding temperature spectral models.

Inputs[edit]

The following data products are used for the polarization analysis:

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.

Outputs[edit]

Synchrotron emission[edit]
File name: COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 40 arcmin
Reference frequency: 30 GHz
HDU -- COMP-MAP-SynchrotronPol
Column Name Data Type Units Description
Q_ML_FULL Real*4 μK_RJ Full-mission Stokes Q posterior maximum
U_ML_FULL Real*4 μK_RJ Full-mission Stokes U posterior maximum
Q_ML_HM1 Real*4 μK_RJ First half-mission Stokes Q posterior maximum
U_ML_HM1 Real*4 μK_RJ First half-mission Stokes U posterior maximum
Q_ML_HM2 Real*4 μK_RJ Second half-mission Stokes Q posterior maximum
U_ML_HM2 Real*4 μK_RJ Second half-mission Stokes U posterior maximum
Q_ML_HR1 Real*4 μK_RJ First half-ring Stokes Q posterior maximum
U_ML_HR1 Real*4 μK_RJ First half-ring Stokes U posterior maximum
Q_ML_HR2 Real*4 μK_RJ Second half-ring Stokes Q posterior maximum
U_ML_HR2 Real*4 μK_RJ Second half-ring Stokes U posterior maximum
Q_ML_YR1 Real*4 μK_RJ "First year" Stokes Q posterior maximum
U_ML_YR1 Real*4 μK_RJ "First year" Stokes U posterior maximum
Q_ML_YR2 Real*4 μK_RJ "Second year" Stokes Q posterior maximum
U_ML_YR2 Real*4 μK_RJ "Second year" Stokes U posterior maximum
Thermal dust emission[edit]
File name: COM_CompMap_DustPol-commander_1024_R2.00.fits
Nside = 1024
Angular resolution = 10 arcmin
Reference frequency: 353 GHz
HDU -- COMP-MAP-DustPol
Column Name Data Type Units Description
Q_ML_FULL Real*4 uK_RJ Full-mission Stokes Q posterior maximum
U_ML_FULL Real*4 uK_RJ Full-mission Stokes U posterior maximum
Q_ML_HM1 Real*4 uK_RJ First half-mission Stokes Q posterior maximum
U_ML_HM1 Real*4 uK_RJ First half-mission Stokes U posterior maximum
Q_ML_HM2 Real*4 uK_RJ Second half-mission Stokes Q posterior maximum
U_ML_HM2 Real*4 uK_RJ Second half-mission Stokes U posterior maximum
Q_ML_HR1 Real*4 uK_RJ First half-ring Stokes Q posterior maximum
U_ML_HR1 Real*4 uK_RJ First half-ring Stokes U posterior maximum
Q_ML_HR2 Real*4 uK_RJ Second half-ring Stokes Q posterior maximum
U_ML_HR2 Real*4 uK_RJ Second half-ring Stokes U posterior maximum
Q_ML_YR1 Real*4 uK_RJ "First year" Stokes Q posterior maximum
U_ML_YR1 Real*4 uK_RJ "First year" Stokes U posterior maximum
Q_ML_YR2 Real*4 uK_RJ "Second year" Stokes Q posterior maximum
U_ML_YR2 Real*4 uK_RJ "Second year" Stokes U posterior maximum

Modelling of the thermal dust emission with the Draine and Li dust model[edit]

The Planck, IRAS, and WISE infrared observations were fit with the dust model presented by Draine & Li in 2007 (DL07). The input maps, the DL07 model, and the fitting procedure and results are presented in Planck-2014-XXIX[7]. Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.

Inputs[edit]

The following data have been fit:

  • WISE 12 micron map
  • IRAS 60 micron map
  • IRAS 100 micron map
  • Full-mission 353 GHz PR2 map
  • Full-mission 545 GHz PR2 map
  • Full-mission 857 GHz PR2 map

The CIB monopole, the CMB anisotropries and the zodiacal light were subtracted to obtain dust emission maps from the sky emission maps. All maps were smoothed to a common angular resolution of 5'.

Model Parameters[edit]

For each pixel of the inputs maps, we have fitted four parameters of the DL07 model:

  • the dust mass surface density, Sigma_Mdust,
  • the dust mass fraction in small PAH grains, q_PAH,
  • the fraction of the total luminosity from dust heated by intense radiation fields, f_PDR,
  • the starlight intensity heating the bulk of the dust, U_min.

The parameter maps and their uncertainties are gathered in one file. This file also includes the chi2 of the fit per degree of freedom.

File name: COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits
Nside = 2048
Angular resolution = 5 arcmin
HDU -- COMP-MAP-Dust-DL07-Parameters
Column Name Data Type Units Description
Sigma_Mdust Real*4 Solar masses/kpc^2 Dust mass surface density
Sigma_Mdust_unc Real*4 Solar masses/kpc^2 Uncertainty (1 sigma) on Sigma_Mdust
q_PAH Real*4 dimensionless Dust mass fraction in small PAH grains
q_PAH_unc Real*4 dimensionless Uncertainty (1 sigma) on q_PAH
f_PDR Real*4 dimensionless Fraction of the total luminosity from dust heated by intense radiation fields
f_PDR_unc Real*4 dimensionless Uncertainty (1 sigma) on f_PDR
U_min Real*4 dimensionless Starlight intensity heating the bulk of the dust
U_min_unc Real*4 dimensionless Uncertainty (1 sigma) on U_min
Chi2_DOF Real*4 dimensionless Chi2 of the fit per degree of freedom

Visible extinction maps[edit]

We provide two exinctions maps at the visible V band: the value from the model (Av_DL) and the renormalized one (Av_RQ) that matches extinction estimates for quasars (QSOs) derived from the Sloan digital sky survey (SDSS) data.

File name: COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits
Nside = 2048
Angular resolution = 5 arcmin
HDU -- COMP-MAP-Dust-DL07-AvMaps
Column Name Data Type Units Description
Av_DL Real*4 magnitude Extinction in the V band from the DL model
Av_DL_unc Real*4 magnitude Uncertainty (1 sigma) on Av_DL
Av_RQ Real*4 magnitude Extinction in the V band renormalized to match estimates from QSO SDSS observations
Av_RQ_unc Real*4 magnitude Uncertainty (1 sigma) on Av_RQ

Model Fluxes[edit]

We provide the model predicted fluxes in the following file.

File name: COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits
Nside = 2048
Angular resolution = 5 arcmin
HDU -- COMP-MAP-Dust-DL07-ModelFluxes
Column Name Data Type Units Description
Planck_857 Real*4 MJy/sr Model flux in the Planck 857 GHz band
Planck_545 Real*4 MJy/sr Model flux in the Planck 545 GHz band
Planck_353 Real*4 MJy/sr Model flux in the Planck 353 GHz band
WISE_12 Real*4 MJy/sr Model flux in the WISE 12 micron band
IRAS_60 Real*4 MJy/sr Model flux in the IRAS 60 micron band
IRAS_100 Real*4 MJy/sr Model flux in the IRAS 100 micron band

Thermal dust and CIB all-sky maps from GNILC component separation[edit]

We describe diffuse foreground products for the Planck 2015 release produced with the GNILC component separation method. See the Planck paper Planck-2016-XLVIII[8] for a detailed discussion on these products.

Method[edit]

The basic idea behind the Generalized Needlet Internal Linear Combination (GNILC) component-separation method (Remazeilles et al, MNRAS 2011) is to disentangle specific components of emission not on the sole basis of the spectral (frequency) information but also on the basis of their distinct spatial information (angular power spectrum). The GNILC method has been applied to Planck data in order to disentangle Galactic dust emission and Cosmic Infrared Background (CIB) anisotropies. Both components have a similar spectral signature but a distinct angular power spectrum (spatial signature). The spatial information used by GNILC is under the form of priors for the angular power spectra of the CIB, the CMB, and the instrumental noise. No assumption is made on the Galactic signal, neither spectral or spatial. In that sense, GNILC is a blind component-separation method. GNILC operates on a needlet (spherical wavelet) frame, therefore adapting the component separation to the local conditions of contamination both over the sky and over the angular scales.

Data[edit]

The data used by GNILC for the analysis are the Planck data release 2 (PR2) frequency maps from 30 to 857 GHz, and a 100 micron hybrid map combined from the SFD map (Schlegel et al, ApJ 1998) at large angular scales (> 30') and the IRIS map (Miville-Deschênes et al, ApJS 2005) at small angular scales (< 30'). This special 100 micron map can be obtained in the External Maps section of the PLA.

Pre-processing[edit]

The point-sources with a signal-to-noise ratio, S/N > 5, in each individual frequency map (30 to 857 GHz, and 100 micron) have been pre-processed by a minimum curvature surface inpainting technique (Remazeilles et al, MNRAS 2015) prior to performing component separation with GNILC.

GNILC thermal dust and CIB products[edit]

The result of GNILC component separation are thermal dust and CIB maps at 353, 545, and 857 GHz. In addition, by fitting a modified blackbody model to the GNILC thermal dust products at 353, 545, 857, and 100 micron, we have created all-sky maps of the dust optical depth, dust temperature, and dust emmissivity index. Note that the thermal dust maps have a variable angular resolution over the sky with an effective beam FWHM varying from 21.8' to 5'. The dust beam FWHM map is also released as a product.

Thermal dust maps[edit]
HDU -- COMP-MAP-DUST
File Name Nside Units Reference frequency Angular resolution Description
COM_CompMap_Dust-GNILC-F353_2048_R2.00.fits 2048 MJy/sr 353 GHz COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust amplitude at 353 GHz
COM_CompMap_Dust-GNILC-F545_2048_R2.00.fits 2048 MJy/sr 545 GHz COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust amplitude at 545 GHz
COM_CompMap_Dust-GNILC-F857_2048_R2.00.fits 2048 MJy/sr 857 GHz COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust amplitude at 857 GHz
COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.00.fits 2048 NA 353 GHz COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust optical depth at 353 GHz
COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.00.fits 2048 NA NA COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust emissivity index
COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.00.fits 2048 K NA COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust temperature
COM_DocMap_Dust-GNILC-Beam-FWHM_R2.00.fits 128 Arcminute NA NA Effective dust beam FWHM
CIB maps[edit]
HDU -- COMP-MAP-CIB
File Name Nside Units Reference frequency Angular resolution Description
COM_CompMap_CIB-GNILC-F353_2048_R2.00.fits 2048 MJy/sr 353 GHz 5 arcmin CIB amplitude at 353 GHz
COM_CompMap_CIB-GNILC-F545_2048_R2.00.fits 2048 MJy/sr 545 GHz 5 arcmin CIB amplitude at 545 GHz
COM_CompMap_CIB-GNILC-F857_2048_R2.00.fits 2048 MJy/sr 857 GHz 5 arcmin CIB amplitude at 857 GHz


References[edit]

  1. ↑ 1.01.11.2 Planck 2015 results. XI. Diffuse component separation: CMB maps, Planck Collaboration, 2016, A&A, 594, A9.
  2. ↑ 2.02.12.22.3 Planck 2015 results. X. Diffuse component separation: Foreground maps, Planck Collaboration, 2016, A&A, 594, A10.
  3. ↑ Planck 2015 results. I. Overview of products and results, Planck Collaboration, 2016, A&A, 594, A1.
  4. ↑ Planck 2015 results. VI. LFI mapmaking, Planck Collaboration, 2016, A&A, 594, A6.
  5. ↑ Planck 2015 results. VIII. High Frequency Instrument data processing: Calibration and maps, Planck Collaboration, 2016, A&A, 594, A8.
  6. ↑ Planck 2015 results. XXV. Diffuse low frequency Galactic foregrounds, Planck Collaboration, 2016, A&A, 594, A25.
  7. ↑ Planck intermediate results. XXIX. All-sky dust modelling with Planck, IRAS, and WISE observations', Planck Collaboration Int. XXIX, A&A, 586, A132, (2016).
  8. ↑ Planck intermediate results. XLVIII. Disentangling Galactic dust emission and cosmic infrared background anisotropies, Planck Collaboration Int. XLVIII A&A, 596, A109, (2016).

Flexible Image Transfer Specification

Cosmic Microwave background

Full-Width-at-Half-Maximum

(Planck) Low Frequency Instrument

(Planck) High Frequency Instrument

Data Processing Center

(Hierarchical Equal Area isoLatitude Pixelation of a sphere, <ref name="Template:Gorski2005">HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere, K. M. Górski, E. Hivon, A. J. Banday, B. D. Wandelt, F. K. Hansen, M. Reinecke, M. Bartelmann, ApJ, 622, 759-771, (2005).

Sunyaev-Zel'dovich

Planck Legacy Archive

Retrieved from ‘https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=CMB_and_astrophysical_component_maps&oldid=12339’