Difference between revisions of "CMB and astrophysical component maps"

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{{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.
  
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.
+
'''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.'''
All the details can be found in <cite>#planck2013-p06</cite>.
 
  
 +
'''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.'''
  
==CMB maps==
+
'''For convenience, we provide as default polarized CMB maps from which all angular scales at l < 30 have been filtered out. '''
-----------------
 
  
CMB maps have been produced by the SMICA, NILC, SEVEM and COMMANDER-Ruler pipelines. Of these, the SMICA product is considered the preferred one overall and is labelled ''Main product'' in the Planck Legacy Archive, while the other two are labeled as ''Additional product''.
+
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>.
  
SMICA and NILC also produce ''inpainted'' maps, in which the Galactic Plane, some bright regions and masked point sources are replaced with a constrained CMB realization such that the whole map has the same statistical distribution as the observed CMB. 
+
In addition, for each method we provide three sets of files, each categorized by the "R2.0X" label as follows:
  
The results of SMICA, NILC and SEVEM pipeline are distributed as a FITS file containing 4 extensions:
+
; ''R2.02''
# CMB maps and ancillary products (3 or 6 maps)
+
<pre style="white-space: pre-wrap;
# CMB-cleaned foreground maps from LFI (3 maps)
+
white-space: -moz-pre-wrap;
# CMB-cleaned foreground maps from HFI (6 maps)
+
white-space: -pre-wrap;
# Effective beam of the CMB maps (1 vector)
+
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>
  
The results of COMMANDER-Ruler are distributed as two FITS files (the high and low resolution) containing the following extensions:
+
; ''R2.01''
High resolution N$_\rm{side}$=2048 (note that we don't provide the CMB-cleaned foregrounds maps for LFI and HFI because the Ruler resolution (~7.4') is lower than the HFI highest channel and and downgrading it will introduce noise correlation).  
+
<pre style="white-space: pre-wrap;
# CMB maps and ancillary products (4 maps)
+
white-space: -moz-pre-wrap;
# Effective beam of the CMB maps (1 vector)
+
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>
  
Low resolution N$_\rm{side}$=256
+
; ''R2.00''
# CMB maps and ancillary products (3 maps)
+
<pre style="white-space: pre-wrap;
# 10 example CMB maps used in the montecarlo realization (10 maps)
+
white-space: -moz-pre-wrap;
# Effective beam of the CMB maps (1 vector)
+
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 data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.
+
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.
  
  
{| class="wikitable"  border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center" style="background:#efefef;"
+
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.
|+ style="background:#eeeeee;" | '''The maps (CMB, noise, masks) contained in the first extension'''
 
|-
 
!width=40px | Col name
 
!width=200px| SMICA
 
!width=200px| NILC
 
!width=200px| SEVEM
 
!width=200px| COMMANDER-Ruler H
 
!width=200px| COMMANDER-Ruler L
 
!width=300px| Description / notes
 
|-
 
| align="left" | 1: I
 
| [[File: CMB-smica.png|200px]]
 
| [[File: CMB-nilc.png|200px]]
 
| [[File: CMB-sevem.png|200px]]
 
| [[File: CMB-CR_h.png|200px]]
 
| [[File: CMB-CR_l.png|200px]]
 
| Raw CMB anisotropy map.  These are the maps used in the component separation paper <cite>#planck2013-p06</cite> {{P2013|12}}.
 
|-
 
| 2: NOISE
 
| [[File: CMBnoise-smica.png|200px]]
 
| [[File: CMBnoise-nilc.png|200px]]
 
| [[File: CMBnoise-sevem.png|200px]]
 
| [[File: CMBnoise-CR_h.png|200px]]
 
| align='center' | not applicable
 
| Noise map.  Obtained by propagating the half-ring noise through the CMB cleaning pipelines.
 
|-
 
| 3: VALMASK
 
| [[File: valmask-smica.png|200px]]
 
| [[File: valmask-nilc.png|200px]]
 
| [[File: valmask-sevem.png|200px]]
 
| [[File: valmask-cr_h.png|200px]]
 
| [[File: valmask-cr_l.png|200px]]
 
| Confidence map. Pixels with an expected low level of foreground contamination.  These maps are only indicative and obtained by different ad hoc methods.  They cannot be used to rank the CMB maps.
 
|-
 
| 4: I_MASK
 
| [[File: cmbmask-smica.png|200px]]
 
| [[File: cmbmask-nilc.png|200px]]
 
| align='center' | not applicable
 
| align='center' | not applicable
 
| align='center' | not applicable
 
| Some areas are masked for the production of the raw CMB maps (for NILC: point sources from 44 GHz to 857 GHz; for SMICA: point sources from 30 GHz to 857 GHz, Galatic region and additional bright regions).
 
|-
 
| 5: INP_CMB
 
| [[File: CMBinp-smica.png|200px]]
 
| [[File: CMBinp-nilc.png|200px]]
 
| align='center' | not applicable
 
| align='center' | not applicable
 
| align='center' | not applicable
 
| Inpainted CMB map.  The raw CMB maps with some regions (as indicated by INP_MASK) replaced by a constrained Gaussian realization.  The inpainted SMICA map was used for PR.
 
|-
 
| 6: INP_MASK
 
| [[File: inpmask-smica.png|200px]]
 
| [[File: inpmask-nilc.png|200px]]
 
| align='center' | not applicable
 
| align='center' | not applicable
 
| align='center' | not applicable
 
| Mask of the inpainted regions.  For SMICA, this is identical to I_MASK.  For NILC, it is not.
 
|}
 
  
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>
  
The union (or common) mask is defined as the union of the confidence masks from the four component separation pipelines, the three listed above and Commander-Ruler. It leaves 73% of the sky available, and so it is denoted as U73.
+
===Product description ===
  
 +
====COMMANDER====
  
===Product description ===
+
;Principle
  
====SMICA====
+
: 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}}.
  
; Principle
 
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole.  It includes multipoles up to <math>\ell = 4000</math>.
 
 
; Resolution (effective beam)
 
; Resolution (effective beam)
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''.  It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function.  Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function.   Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.
+
 
 +
: 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
 
; Confidence mask
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources.  This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel.
+
 
; Masks and inpainting
+
: 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.  
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions.  Those invalid pixels are indicated with the mask named 'I_MASK'.   The raw SMICA map has been inpainted, producing the map named "INP_CMB".  Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.
 
  
 
====NILC====
 
====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
 
; Principle
: The Needlet-ILC (hereafter NILC) CMB map is constructed from all Planck channels from 44 to 857 GHz and includes multipoles up to <math>\ell = 3200</math>. It 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.
+
: 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)
 
; Resolution (effective beam)
: As in the SMICA product except that there is no abrupt truncation at <math>\ell_{max}= 3200</math> but a smooth transition to <math>0</math> over the range <math>2700\leq\ell\leq 3200</math>.
+
: 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
 
; Confidence mask
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources.  This mask provides a qualitative indication of the cleanliness of a pixel.   The threshold is somewhat arbitrary.
+
: 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.
; Masks and inpainting
 
: The raw NILC map has valid pixels except at the location of masked point sources.  This is indicated with the mask named 'I_MASK'.  The raw NILC map has been inpainted, producing the map named "INP_CMB".  The inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.
 
  
====SEVEM====
 
  
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 robustNote that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB ma (''I_MASK'') nor an inpainted version of the map and its associated mask.  On the other hand, it provides ''channel maps'' and 100, 143, and 217 GHz which are used as the building blocks of the final map.
+
====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:
 +
 
 +
* 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.
 +
 
 +
* 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%.
 +
 
 +
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 f<sub>sky</sub> = 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 &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.
 +
 
 +
====CMB-subtracted frequency maps ("Foreground maps")====
 +
 
 +
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 methodThey 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:
 +
 
 +
* ''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.
  
====COMMANDER-Ruler====
+
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.
  
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at $N_\rm{side}$=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which
+
====Quadrupole Residual Maps====
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper <cite>#planck2013-p06</cite> {{p2013|12}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of:
 
  
* Maps of the Amplitudes of the CMB at low resolution, $N_\rm{side}$=256, along with the standard deviations of the outputs, beam profiles derived from the production process.  
+
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.
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, $N_\rm{side}$=2048, beam profiles derived from the production process.  
 
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see <cite>#planck2013-p06</cite>.  
 
  
 
===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.
  
; 1) Pre-processing
+
; Priors
: All input maps undergo a pre-processing step to deal with point sources.  The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz,  here all point sources with SNR > 7.5 are masked and filled-in similarly.
 
; 2) Linear combination
 
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.
 
; 3) Post-processing
 
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.
 
  
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.
+
: 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
  
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]
+
: 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====
 
====NILC====
  
; 1) Pre-processing
+
; Pre-processing
: Same pre-processing as SMICA (except the 30 GHz channel is not used).
+
 
; 2) Linear combination
+
: 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
: The pre-processed Planck frequency channels from 44 to 857 GHz are linearly combined with weights which depend on location on the sky and on the multipole range up to <math>\ell = 3200</math>.   This is achieved using a needlet (redundant spherical wavelet) decomposition.  For more details, see <cite>#planck2013-p06</cite>.
+
 
; 3) Post-processing
+
; Linear combination
: The areas masked in the pre-processing plus other bright regions step are replaced by a constrained Gaussian realization as in the SMICA post-processing step.
+
 
 +
: 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====
 
====SEVEM====
  
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 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).
  
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math>
+
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.
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).
 
  
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.
+
;Intensity
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.
 
  
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.
+
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.
  
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 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.
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>.
+
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 method has been successfully applied to Planck simulations <cite>#leach2008</cite> and to WMAP polarisation data <cite>#Fernandez-Cobos2012</cite>.
+
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.
  
====COMMANDER-Ruler====
+
;Polarization
  
The production process consist in low and high resolution runs according to the description above.  
+
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
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA.  
+
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
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA.  
+
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====
 +
 
 +
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.
 +
 
 +
<!--[[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.''']]-->
 +
 
 +
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.
 +
 
 +
<!--[[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.''']]-->
  
 
===Inputs===
 
===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.  
 
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_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.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_R1.12.fits|link=COM_CompMap_CMB-sevem_2048_R1.12.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_R1.20.fits|link=COM_CompMap_CMB-smica_2048_R1.20.fits}}
+
*''COM_CMB_IQU-{fff}-{fgsub-sevem}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits'' for the sevem frequency-dependent, foregrounds-subtracted maps,
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_2048_R1.00.fits|link=COM_CompMap_CMB-commrul_2048_R1.00.fits}}
+
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).
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_0256_R1.00.fits|link=COM_CompMap_CMB-commrul_0256_R1.00.fits}}
 
  
 +
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''
  
The files contain a minimal primary extension with no data and four ''BINTABLE'' data extensions. Each column of the ''BINTABLE'' is a (Healpix) map; the column names and the most important keywords of each extension are described in the table below; for the remaining keywords, please see the FITS files directly.
+
====Version 2.00 files====
  
 +
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.
  
 
{| 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 || 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                                   
 
|-
 
|-
|NOISE || Real*4 || uK_cmb || Estimated noise map (note 1)
+
|HM2 || Real*4 || uK_cmb || Half-miss 2                                   
 
|-
 
|-
|I_STDEV|| Real*4 || uK_cmb || Standard deviation, ONLY on COMMANDER-Ruler products
+
|YR1  || Real*4 || uK_cmb || Year 1                                       
 
|-
 
|-
|VALMASK|| Byte || none || Confidence mask (note 2)
+
|YR2  || Real*4 || uK_cmb || Year 2                                        
 
|-
 
|-
|I_MASK|| Byte || none || Mask of regions over which CMB map is not built (Optional - see note 3)
+
|HR1  || Real*4 || uK_cmb || Half-ring 1                                   
 
|-
 
|-
|INP_CMB || Real*4 || uK_cmb || Inpainted CMB temperature map (Optional - see note 3)
+
|HR2  || Real*4 || uK_cmb || Half-ring 2                                   
 
|-
 
|-
|INP_MASK || Byte || none || mask of inpainted pixels (Optional - see note 3)
+
|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                               
 +
|-
 +
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Keyword || Data Type || Value || Description
 
! Keyword || Data Type || Value || Description
Line 231: 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-Ruler)
+
|METHOD  || String ||name || Cleaning method (smica/nilc/sevem/commander)
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
!colspan="4" | Ext. 2. EXTNAME = ''FGDS-LFI'' (BINTABLE) - Note 4
+
!colspan="4" | Ext. 2. or 3. EXTNAME = ''BEAM_WF'' (BINTABLE) .  See Note 1
 
|- 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
+
|BEAMWF          || Real*4 || none || The effective beam transfer function, including the pixel window function.  See Note 2.
|-
 
|LFI_044  || Real*4 || K_cmb || 44 GHz foregrounds
 
|-
 
|LFI_070  || Real*4 || K_cmb || 70 GHz foregrounds
 
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Keyword || Data Type || Value || Description
 
! Keyword || Data Type || Value || Description
 
|-
 
|-
|PIXTYPE ||  String || HEALPIX ||
+
|LMIN ||  Int || value || First multipole of beam TF
 
|-
 
|-
|COORDSYS ||  String || GALACTIC ||Coordinate system
+
|LMAX ||  Int || value || Last multipole of beam TF
 
|-
 
|-
|ORDERING || String || NESTED  || Healpix ordering
+
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
|-
 
|NSIDE  ||  Int || 1024 || Healpix Nside
 
|-
 
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM)
 
 
|-
 
|-
 +
|}
 +
 +
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. 3. EXTNAME = ''FGDS-HFI'' (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
 
|-
 
|-
|HFI_100  || Real*4 || K_cmb || 100 GHz foregrounds
+
|I_Stokes    || Real*4 || uK_cmb || I map (Nside=1024,2048)
|-
+
|-
|HFI_143   || Real*4 || K_cmb || 143 GHz foregrounds
+
|Q_Stokes   || Real*4 || uK_cmb || Q map (Nside=1024)                                 
 
|-
 
|-
|HFI_217   || Real*4 || K_cmb || 217 GHz foregrounds
+
|U_Stokes   || Real*4 || uK_cmb || U map (Nside=2048)                                   
 
|-
 
|-
|HFI_353  || Real*4 || K_cmb || 353 GHz foregrounds
+
|TMASK    || Int || none  || optional Temperature confidence mask                                 
 
|-
 
|-
|HFI_545   || Real*4 || MJy/sr || 545 GHz foregrounds
+
|PMASK   || Int || none  || optional Polarisation confidence mask                                   
|-
 
|HFI_857    || Real*4 || MJy/sr || 857 GHz foregrounds
 
 
|-
 
|-
 
|- 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/COMMANDER-Ruler)
 
 
|- 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 || none || The effective beam window function, including the pixel window function. See Note 5.
+
|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 303: Line 419:
 
|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
 
|-
 
|-
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
+
|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====
  
Notes:
+
'''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. '''
# 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 confidence mask indicates where the CMB map is considered valid.  
+
These files have names like:
# This column is not present in the SEVEM and COMMANDER-Ruler product file.  For SEVEM these three columns give the CMB channel maps at 100, 143, and 217 GHz (columns ''C100'', ''C143'', and ''C217'', in units of uK_cmb.
+
*''COM_CMB_IQU-{method}_1024_R2.02_{coverage}.fits''
# 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. Those columns are not present in the COMMANDER-Ruler product file.
+
as indicated above. They contain:
# The beam window function <math>B_\ell</math> given here includes the  pixel window function <math>p_\ell</math> for the Nside=2048  pixelizationIt means that, ideally, <math>C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2</math>.
+
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 belowFor full details, see the FITS header.
  
The low resolution COMMANDER-Ruler CMB product is organized in the following way:
 
 
{| 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 low resolution COMMANDER-Ruler map file data structure'''
+
|+ '''CMB R2.02 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 || CMB temperature map obtained as average over 1000 samples
+
|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)                           
 
|-
 
|-
|I_stdev  || Real*4 || uK_cmb || Corresponding Standard deviation amongst the 1000 samples
+
|TMASK    || Int || none  || optional Temperature confidence mask                                 
 
|-
 
|-
|VALMASK|| Byte || none || 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 || 2048 || Healpix Nside
+
|NSIDE  ||  Int || 1024 or 2048 || Healpix Nside
 
|-
 
|-
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
+
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM)
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
!colspan="4" | Ext. 2. EXTNAME = ''CMB-Sample'' (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
 
|-
 
|-
|I_SIM01  || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|INT_BEAM          || Real*4 || none || Effective beam transfer function. See Note 1.
 
|-
 
|-
|I_SIM02  || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|POL_BEAM        || Real*4 || none || Effective beam transfer function. See Note 1.
 
|-
 
|-
|I_SIM03   || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|- bgcolor="ffdead"    
 +
! Keyword || Data Type || Value || Description
 
|-
 
|-
|I_SIM04  || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|LMIN || Int || value || First multipole of beam WF
 
|-
 
|-
|I_SIM05  || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|LMAX_I || Int || value || Last multipole for Int beam TF
 
|-
 
|-
|I_SIM06  || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|LMAX_P || Int || value || Last multipole for Pol beam TF
 
|-
 
|-
|I_SIM07  || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|METHOD  || String ||name || Cleaning method
 
|-
 
|-
|I_SIM08   || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|}
 +
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>
 +
 
 +
====Common masks====
 +
 
 +
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====
 +
 
 +
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.
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|+ '''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
 
|-
 
|-
|I_SIM09  || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
+
|INTENSITY    || Real*4 || K_cmb || the residual map                           
|-
 
|I_SIM10  || Real*4 || K_cmb || CMB Sample, smoothed to 40 arcmin
 
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Keyword || Data Type || Value || Description
 
! Keyword || Data Type || Value || Description
 +
|-
 +
|AST-COMP ||  String || KQ-RESID || 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 || 2048 || Healpix Nside
 
|-
 
|-
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
+
|METHOD  || String ||name || Cleaning method
|- bgcolor="ffdead" 
 
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)
 
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
|-
 
|BEAM_WF          || Real*4 || none || The effective beam window function, including the pixel window function.
 
|-
 
|- bgcolor="ffdead" 
 
! Keyword || Data Type || Value || Description
 
|-
 
|LMIN ||  Int || value || First multipole of beam WF
 
|-
 
|LMAX ||  Int || value || Lsst multipole of beam WF
 
|-
 
|METHOD  || String ||name || Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
 
 
|-
 
|-
 
|}
 
|}
 
 
The FITS files containing the ''union'' (or common) maks is:
 
* {{PLASingleFile|fileType=map|name=COM_Mask_CMB-union_2048_R1.10.fits|link=COM_Mask_CMB-common}}
 
which contains a single ''BINTABLE'' extension with a single column (named ''U73'') for the mask, which is boolean (FITS ''TFORM = B''), in GALACTIC coordinates, NESTED ordering, and Nside=2048.
 
 
For the benefit of users who are only looking for files that can easily be converted to pretty pictures we also provide a fits file containing the SMICA cmb map with no additional information (noise or masks). This file contains a single extension with a single column containing the SMICA cmb temperature map and it can be found {{PLASingleFile|fileType=map|name=this|link=here}}.
 
 
===Cautionary notes===
 
 
# 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 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.
 
# The beam transfer functions do not account for uncertainties in the beams of the frequency channel maps.
 
  
 
== Astrophysical foregrounds from parametric component separation ==
 
== Astrophysical foregrounds from parametric component separation ==
--------------------------
+
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}}.
  
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper <cite>#planck2013-p06</cite> {{P2013|12}} for a detailed description and astrophysical discussion of those.
+
===Low-resolution temperature products===
  
===Product description===
+
: 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.
  
; Low frequency foreground component
+
====Inputs====
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.
 
  
; Thermal dust
+
The following data products are used for the low-resolution analysis:
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided.  
+
* 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.
  
; Sky mask
+
====Outputs====
: 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.
 
  
===Production process===
+
=====Synchrotron emission=====
  
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input
+
<!--<center>
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution  
+
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px>
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is
+
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper <cite>#planck2013-p06</cite> {{p2013|12}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.
+
</gallery>
 +
</center>-->
  
===Inputs===
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}
 +
: Reference frequency: 408 MHz
 +
: Nside = 256
 +
: Angular resolution = 60 arcmin
  
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix.
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].
+
|+ 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
 +
|}
  
===Related products===
 
  
None.
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
+
|+ Extension 1 -- SYNC-TEMP
===File names===
+
|-
 
+
|- bgcolor="ffdead" 
* Low frequency component at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}
+
! Column Name || Data Type || Units || Description
* Low frequency component at N$_\rm{side}$ 2048: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}
+
|-
* Thermal dust at N$_\rm{side}$ 256: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}
+
|nu  || Real*4 || Hz || Frequency   
* Thermal dust at N$_\rm{side}$ 2048:  {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}
+
|-
* Mask: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}
+
|intensity || Real*4 || W/Hz/m2/sr || GALPROP z10LMPD_SUNfE spectrum   
 
+
|}
===Meta Data===
 
 
 
====Low frequency foreground component====
 
  
=====Low frequency component at N$_\rm{side}$ = 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"   
 
|- 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
 
|-
 
|-
|I_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation of intensity
+
|EM_RMS || Real*4 || cm^-6 pc || Emission measure posterior rms
 
|-
 
|-
|Beta || Real*4 || || effective spectral index
+
|TEMP_ML || Real*4 || K || Electron temperature posterior maximum   
 
|-
 
|-
|B_stdev || Real*4 || || standard deviation on the effective spectral index
+
|TEMP_MEAN || Real*4 || K || Electron temperature posterior mean
 +
|-
 +
|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
 
 
=====Low frequency component at N$_\rm{side}$ = 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"   
 
|- 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_MEAN || Real*4 || uK_RJ || Primary amplitude posterior mean
 
|-
 
|-
|I_stdev || Real*8 || uK<math>_{CMB}</math> || standard deviation of intensity
+
|I_RMS || Real*4 || uK_RJ || Primary amplitude posterior rms
 
|-
 
|-
|I_hr1 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 1
+
|FREQ_ML || Real*4 || GHz || Primary peak frequency posterior maximum   
 
|-
 
|-
|I_hr2 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 2
+
|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"   
 
|- 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
 
  
====Thermal dust====
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}}
 +
: Nside = 256
 +
: Angular resolution = 60 arcmin
  
=====Thermal dust component at N$_\rm{side}$=256=====
+
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. 
  
: 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
+
|+ HDU -- COMP-MAP-co10
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- 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(1-0) amplitude posterior maximum   
 
|-
 
|-
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity
+
|I_MEAN || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior mean
 
|-
 
|-
|Em || Real*4 || || emissivity
+
|I_RMS || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior rms
 +
|}
 +
 
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ Extension 1 -- COMP-MAP-co21
 
|-
 
|-
|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(2-1) amplitude posterior maximum   
 
|-
 
|-
|T_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation on temerature
+
|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
 
|}
 
|}
  
; Notes:
 
: Comment: The intensity is normalized at 353 GHz
 
 
=====Thermal dust component at N$_\rm{side}$=2048=====
 
 
File name: COM_CompMap_dust-commrul_2048_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 2 -- COMP-MAP-co32
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
|I || Real*8 || MJy/sr || Intensity
+
|I_ML || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior maximum   
 
|-
 
|-
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity
+
|I_MEAN || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior mean
 
|-
 
|-
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1
+
|I_RMS || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior rms
|-
 
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2  
 
 
|}
 
|}
  
 +
=====94/100 GHz line emission=====
  
: '''Name HDU -- BeamWF'''
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-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-xline
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
|BeamWF || Real*4 || || beam profile 
+
|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
 
|}
 
|}
  
; Notes:
+
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.
: Comment: Beam window function used in the Component separation process
 
  
====Sky mask====
+
=====Thermal dust emission=====
  
File name: COM_CompMap_Mask-rulerminimal_2048.fits
+
: 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
  
; '''Name HDU -- COMP-MASK'''
+
: Reference frequency: 545 GHz
 
 
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-dust
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
|Mask || Real*4 || || Mask
+
|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 dust emission ==
+
=====Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters=====
-------------------------------------
 
  
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. The details of the model can be found here <cite>#dustModelXXXI</cite>.
+
: 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
  
=== Model of all-sky thermal dust emission ===
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-SZ
 +
|-
 +
|- bgcolor="ffdead" 
 +
! 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
 +
|}
  
The model of the thermal dust emission is based on a modified black body (MBB) fit to the data <math>I_\nu</math>
+
===High-resolution temperature products===
  
: <math>I_\nu = A\, B_\nu(T)\, \nu^\beta</math>
+
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.
  
where <math>B_\nu(T)</math> is the Planck function for dust equilibirum temperature <math>T</math>, <math>A</math> is the amplitude of the MBB and <math>\beta</math> the dust spectral index. The dust optical depth at frequency <math>\nu</math> is
+
====Inputs====
  
: <math>\tau_\nu = I_\nu / B_\nu(T) = A\, \nu^\beta</math>
+
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.
  
The dust parameters provided are <math>T</math>, <math>\beta</math> and <math>\tau_{353}</math>. They were obtained by fitting the Planck data at 353, 545 and 857 GHz (from which the Planck zodiacal light model was removed) together with the IRAS 100 micron data. The latter is a combination of the 100 micron maps from IRIS (Miville-Deschenes & Lagache, 2005) and from Schlegel et al. (1998), SFD1998. The IRIS (SFD1998) map is used at scales smaller (larger) than 30 arcmin; this combination allows to take advantage of the higher angular resolution and better control of gain variations of the IRIS map and of the better removal of the zodiacal light emission of the SFD1998 map.
+
====Outputs====
  
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 set a Galactic zero level, using a correlation with the LAB 21 cm data in diffuse areas of the sky (<math>N_{HI} < 2\times10^{20} cm^{-2}</math>). 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 (<math>N_{HI} < 3\times10^{20} cm^{-2}</math>). Faint residual dipole structures, identified in the 353 and 545 GHz maps, were removed prior to the fit.
+
=====CO J2->1 emission=====
  
The MBB fit was performed using a <math>\chi^2</math> minimization method, 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 levels. Because of the known degeneracy between <math>T</math> and <math>\beta</math> in the presence of noise, we performed tge fit in two steps. First we produced a model of dust emission using data smoothed to 30 arcmin; at such resolution no systematic bias of the parameters is observed. In a second step the map of the spectral index <math>\beta</math> at 30 arcmin was used to fit the data for <math>T</math> and <math>\tau_{353}</math> at 5 arcmin.
+
: 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 <math>E(B-V)</math> map for extra-galactic studies===
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
For the production of the <math>E(B-V)</math> map, we used a MBB fit to Planck and IRAS data from which point sources were removed to avoid contamination by galaxies.  In the hypothesis of constant dust emission cross-section, the optical depth map <math>\tau_{353}</math> is proportional to dust column density and therefore often used to estimate E(B-V). The analysis of Planck data revealed that the ratio <math>\tau_{353}/N_{HI}</math> and <math>\tau_{353}/E(B-V)</math> are not constant, even in the diffuse ISM, but that they depend on <math>T</math> revealing possible spatial variations of the dust emission cross-section. It appears that the dust radiance, <math>R</math>, i.e. the dust emission integrated in frequency, is a better tracer of column density in the diffuse ISM, implying small spatial variations of the radiation field strength at high Galactic latitude.
+
|+ HDU -- COMP-MAP-CO21
Given those results, we also deliver the map of <math>R</math> as a dust product and we propose to use it as an estimator of Galactic dust reddening for extra-galactic studies: <math>E(B-V) = q\, R</math>.
+
|-
 +
|- bgcolor="ffdead" 
 +
! 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   
 +
|}
  
To estimate the calibration factor q, we followed a method similar to <cite>#mortsell2013</cite> based on SDSS reddening measurements of quasars in the u, g, r, i and z bands <cite>#schneider2007</cite>. We used a sample of 53 399 quasars, selecting objects at redshifts for which Ly<math>\alpha</math> does not enter the SDSS filters. The interstellar HI column densities covered on the lines of sight of this sample ranges from <math>0.5</math> to <math>10\times10^{20}\,cm^{-2}</math>. Therefore this sample allows us to estimate q in the diffuse ISM where this map of E(B-V) is intended to be used.
 
  
=== Dust optical depth products ===
+
=====Thermal dust emission=====
The dust model maps are found in the file {{PLASingleFile|fileType=map|name=HFI_CompMap_ThermalDustModel_2048_R1.20.fits|link=HFI_CompMap_ThermalDustModel_2048_R1.20.fits}} (see the note [[#noteOnDust|below]] for an important clarification regarding the thermal dust model); its characteristics are:
 
* Dust optical depth at 353 GHz: Nside=2048, fwhm=5', no units
 
* Dust temperature: Nside 2048, fwhm=5', units=Kelvin
 
* Dust spectral index: Nside=2048, fwhm=30', no units
 
* Dust radiance: Nside=2048, fwhm=5', units=Wm<sup>-2</sup>sr<sup>-1</sup>
 
* E(B-V) for extragalactic studies: Nside=2048, fwhm=5', units=magnitude, obtained with data from which point sources were removed.
 
  
 +
: 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
  
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
: Reference frequency: 545 GHz
|+ '''Dust opacity file data structure'''
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
|- bgcolor="ffdead" 
+
|+ HDU -- COMP-MAP-dust
! 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 optical depth at 353GHz
+
|I_ML_FULL || Real*4 || uK_RJ || Full-mission amplitude posterior maximum   
 
|-
 
|-
| ERR_TAU || Real*4 || none || Error on the optical depth
+
|I_ML_HM1 || Real*4 || uK_RJ || First half-mission amplitude posterior maximum   
 
|-
 
|-
| EBV || Real*4 || mag || E(B-V) for extra-galactic studies
+
|I_ML_HM2 || Real*4 || uK_RJ || Second half-mission amplitude posterior maximum   
 
|-
 
|-
| RADIANCE || Real*4 || Wm<sup>-2</sup>sr<sup>-1</sup> || Integrated emission
+
|I_ML_HR1 || Real*4 || uK_RJ || First half-ring amplitude posterior maximum   
 
|-
 
|-
|TEMP || Real*4 || K || Dust temperature
+
|I_ML_HR2 || Real*4 || uK_RJ || Second half-ring amplitude posterior maximum   
 
|-
 
|-
|ERR_TEMP || Real*4 || K || Error on the temperature
+
|I_ML_YR1 || Real*4 || uK_RJ || "First year" amplitude posterior maximum   
 
|-
 
|-
| BETA || Real*4 || none || Dust spectral index
+
|I_ML_YR2 || Real*4 || uK_RJ || "Second year" amplitude posterior maximum   
 
|-
 
|-
| ERR_BETA || Real*4 || none || Error on Beta
+
|BETA_ML_FULL || Real*4 || NA || Full-mission emissivity index posterior maximum   
 
|-
 
|-
|- bgcolor="ffdead" 
+
|BETA_ML_HM1 || Real*4 || NA || First half-mission emissivity index posterior maximum   
! Keyword || Data Type || Value || Description
 
 
|-
 
|-
| AST-COMP || String || DUST|| Astrophysical compoment name
+
|BETA_ML_HM2 || Real*4 || NA || Second half-mission emissivity index posterior maximum   
 
|-
 
|-
| PIXTYPE || String || HEALPIX ||
+
|BETA_ML_HR1 || Real*4 || NA || First half-ring emissivity index posterior maximum   
 
|-
 
|-
| COORDSYS || String || GALACTIC ||Coordinate system
+
|BETA_ML_HR2 || Real*4 || NA || Second half-ring emissivity index posterior maximum   
 
|-
 
|-
| ORDERING || String || NESTED  || Healpix ordering
+
|BETA_ML_YR1 || Real*4 || NA || "First year" emissivity index posterior maximum   
 
|-
 
|-
| NSIDE  ||   Int || 2048 || Healpix Nside for LFI and HFI, respectively
+
|BETA_ML_YR2 || Real*4 || NA || "Second year" emissivity index posterior maximum   
 
|-
 
|-
| FIRSTPIX ||  Int*4 ||          0 || First pixel number
 
|-
 
| LASTPIX ||  Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively
 
 
|}
 
|}
  
 +
===Polarization products===
  
 +
Two polarization foreground products are provided, namely synchrotron and thermal dust emission. The spectral models are assumed identical to the corresponding temperature spectral models.
  
<div id="noteOnDust"></div><span style="font-size:120%"> <span style="color:Red"><b>IMPORTANT NOTE:</b></span></span> The dust model has recently (4 December 2013) been updated and the new model is the one being distributed by default. A detailed description of the model can be found here <cite>#dustModelXXXI</cite>. Users interested in the old dust model map should contact the [http://www.sciops.esa.int/helpdesk_pia PLA help desk].
+
====Inputs====
  
== CO emission maps ==
+
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.
  
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. A full description of how these products were producedis given in <cite>#planck2013-p03a</cite>.
+
====Outputs====
 +
=====Synchrotron emission=====
  
* 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.
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits|link=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits}}
* 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.
+
: Nside = 256
* 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.
+
: Angular resolution = 40 arcmin
  
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 [[CMB_and _astrophysical_component_maps#Maps_of_astrophysical_foregrounds | above]]).
+
: Reference frequency: 30 GHz
 
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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:
+
|+ HDU -- COMP-MAP-SynchrotronPol
* The signal map
+
|-
* The standard deviation map (same unit as the signal),
 
* 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.
 
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.
 
Type 2 products have a 15 arcminute resolution
 
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   
 +
|-
 +
|Q_ML_HM1 || Real*4 || &mu;K_RJ || First half-mission Stokes Q posterior maximum   
 
|-
 
|-
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity
+
|U_ML_HM1 || Real*4 || &mu;K_RJ || First half-mission Stokes U posterior maximum   
 
|-
 
|-
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|Q_ML_HM2 || Real*4 || &mu;K_RJ || Second half-mission Stokes Q posterior maximum   
 
|-
 
|-
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable
+
|U_ML_HM2 || Real*4 || &mu;K_RJ || Second half-mission Stokes U posterior maximum   
 
|-
 
|-
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map
+
|Q_ML_HR1 || Real*4 || &mu;K_RJ || First half-ring Stokes Q posterior maximum   
 
|-
 
|-
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity
+
|U_ML_HR1 || Real*4 || &mu;K_RJ || First half-ring Stokes U posterior maximum   
 
|-
 
|-
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|Q_ML_HR2 || Real*4 || &mu;K_RJ || Second half-ring Stokes Q posterior maximum   
 
|-
 
|-
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable
+
|U_ML_HR2 || Real*4 || &mu;K_RJ || Second half-ring Stokes U posterior maximum   
 
|-
 
|-
|I32 || Real*4 || K_RJ km/sec || The CO(3-2) intensity map
+
|Q_ML_YR1 || Real*4 || &mu;K_RJ || "First year" Stokes Q posterior maximum   
 
|-
 
|-
|E32 || Real*4 || K_RJ km/sec || Uncertainty in the CO(3-2) intensity
+
|U_ML_YR1 || Real*4 || &mu;K_RJ || "First year" Stokes U posterior maximum   
 
|-
 
|-
|N32 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
+
|Q_ML_YR2 || Real*4 || &mu;K_RJ || "Second year" Stokes Q posterior maximum
 
|-
 
|-
|M32 || Byte || none || Region over which the CO(3-2) intensity is considered reliable
+
|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 ===
  
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
The Planck, IRAS, and WISE infrared observations were fit with the dust model presented by Draine & Li in 2007 (DL07).
|+ '''Type-2 CO map file data structure'''
+
The input maps, the DL07 model, and the fitting procedure and results are presented in {{PlanckPapers|planck2014-XXIX}}.
|- bgcolor="ffdead" 
+
Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.
!colspan="4" | 1. EXTNAME = 'COMP-MAP'
+
 
 +
====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====
 +
 
 +
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: {{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.
  
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
====Method====
|+ '''Type-3 CO map file data structure'''
+
 
 +
: 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="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-DUST
 +
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
!colspan="4" | 1. EXTNAME = 'COMP-MAP'
+
! File Name || Nside || Units || Reference frequency || Angular resolution || Description
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || 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]]
 
#[[References2]]
 
</biblio>
 
  
  
  
 
[[Category:Mission products|007]]
 
[[Category:Mission 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.

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]

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