# Difference between revisions of "CMB and astrophysical component maps"

## 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 FITSFlexible Image Transfer Specification file containing the data and associated information. All the details can be found in Planck-2015-A09[1] and Planck-2015-A10[2].

## CMBCosmic Microwave background maps

CMBCosmic Microwave background 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 CMBCosmic Microwave background polarization have used maps which have been high-pass filtered to remove the large angular scales. We warn all users of the CMBCosmic Microwave background polarization maps that they cannot yet be used for cosmological studies at large angular scales.

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

For each method we provide the following:

• Full-mission CMBCosmic Microwave background intensity map, confidence mask and beam transfer function.
• Full-mission CMBCosmic Microwave background polarisation map,
• 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 CMBCosmic Microwave background 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

#### COMMANDER

Principle
COMMANDER is a Planck software code implementing pixel based Bayesian parametric component separation. Each astrophysical signal component is modelled in terms of a small number of free parameters per pixel, typically in terms of an amplitude at a given reference frequency and a small set of spectral parameters, and these are fitted to the data with an MCMC Gibbs sampling algorithm. Instrumental parameters, including calibration[LFI meaning]: absolute calibration refers to the 0th order calibration for each channel, 1 single number, while the relative calibration refers to the component of the calibration that varies pointing period by pointing period., 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 FWHMFull-Width-at-Half-Maximum resolution, and are pixelized at Nside=256. The corresponding CMBCosmic Microwave background map defines the input map for the low-l Planck 2015 temperature likelihood.
• The Commander CMBCosmic Microwave background 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 CMBCosmic Microwave background 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.
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

Principle
The Needlet-ILC (hereafter NILC) CMBCosmic Microwave background 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 . The effective beam is equivalent to a Gaussian circular beam with FWHMFull-Width-at-Half-Maximum=5 arcminutes.
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 CMBCosmic Microwave background 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 CMBCosmic Microwave background-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 CMBCosmic Microwave background map.
Resolution
For intensity the clean CMBCosmic Microwave background map is constructed up to a maximum at Nside=2048 and at the standard resolution of 5 arcminutes (Gaussian beam).
For polarization the clean CMBCosmic Microwave background map is produced at Nside=1024 with a resolution of 10 arcminutes (Gaussian beam) and a maximum .
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 CMBCosmic Microwave background 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 CMBCosmic Microwave background 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 CMBCosmic Microwave background maps for the 70, 100 and 143 GHz (at Nside=1024). The 70 GHz clean map is provided at its original resolution, whereas the 100 and 143 GHz maps have a resolution given by a Gaussian beam with fwhm=10 arcminutes.

#### SMICA

Principle
SMICA produces CMBCosmic Microwave background maps by linearly combining all Planck input channels with multipole-dependent weights. It includes multipoles up to . 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 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 =2048.
The SMICA Q and U maps are obtained similarly but are produced at =1024 with an effective beam of 10 arc-minutes (to be multiplied by the pixel window function, as for the intensity map).
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.

A number of common masks have been defined for analysis of the CMBCosmic Microwave background 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 CMBCosmic Microwave background 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 CMBCosmic Microwave background maps is greater than 10 μK. It has fsky = 76.1%.

The common masks for the CMBCosmic Microwave background 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 CMBCosmic Microwave background 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.

#### CMBCosmic Microwave background-subtracted frequency maps ("Foreground maps")

These are the full-sky, full-mission frequency maps in intensity from which the CMBCosmic Microwave background 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(Planck) Low Frequency Instrument channels and at Nside = 2048 for the six HFI(Planck) High Frequency Instrument channels. The filenames are:

• LFI(Planck) Low Frequency Instrument_Foregrounds-{method}_1024_Rn.nn.fits (145 MB each)
• HFI(Planck) High Frequency Instrument_Foregrounds-{method}_2048_Rn.nn.fits (1.2 GB each)

To remove the CMBCosmic Microwave background, the respective CMBCosmic Microwave background 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 in harmonic space, assuming a symmetric beam.

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

The frequency maps from which the CMBCosmic Microwave background have been subtracted are:

• LFI(Planck) Low Frequency Instrument_SkyMap_0nn_1024_R2.01_full.fits
• HFI(Planck) High Frequency Instrument_SkyMap_nnn_2048_R2.0n_full.fits

Note that the temperature column in the HFI(Planck) High Frequency Instrument R2.00, R2.01 and R2.02 is the same, since the changes in these maps involved the polarization columns only. Also note that the zodiacal light correction described here was applied to the HFI(Planck) High Frequency Instrument temperature maps before the CMBCosmic Microwave background subtraction.

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 CMBCosmic Microwave background 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 CMBCosmic Microwave background maps.

### Production process

#### 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 FWHMFull-Width-at-Half-Maximum; for the Planck-only, all-frequency analysis it is 40 arcmin FWHMFull-Width-at-Half-Maximum; 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

Pre-processing
All sky frequency maps are deconvolved using the DPCData Processing Center beam transfer function provided, and re-convolved with a 5 arcminutes FWHMFull-Width-at-Half-Maximum 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([http://healpix.sourceforge.net Hierarchical Equal Area isoLatitude Pixelation of a sphere], <ref name="[[:Template:Gorski2005]]">[http://iopscience.iop.org/0004-637X/622/2/759/pdf/0004-637X_622_2_759.pdf '''HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere'''], K. M. G&oacute;rski, E. Hivon, A. J. Banday, B. D. Wandelt, F. K. Hansen, M. Reinecke, M. Bartelmann, ApJ, '''622''', 759-771, (2005). 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([http://healpix.sourceforge.net Hierarchical Equal Area isoLatitude Pixelation of a sphere], <ref name="[[:Template:Gorski2005]]">[http://iopscience.iop.org/0004-637X/622/2/759/pdf/0004-637X_622_2_759.pdf '''HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere'''], K. M. G&oacute;rski, E. Hivon, A. J. Banday, B. D. Wandelt, F. K. Hansen, M. Reinecke, M. Bartelmann, ApJ, '''622''', 759-771, (2005). tools.

#### 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 CMBCosmic Microwave background signal is properly removed. A linear combination of the templates is then subtracted from (hitherto unused) map d to produce a clean CMBCosmic Microwave background map at that frequency. This is done in real space at each position on the sky: where is the number of templates. The coefficients are obtained by minimising the variance of the clean map 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 CMBCosmic Microwave background 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 CMBCosmic Microwave background 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 CMBCosmic Microwave background 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 CMBCosmic Microwave background 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 CMBCosmic Microwave background maps for the Q and U components at a resolution of 10' (Gaussian beam) for a HEALPix([http://healpix.sourceforge.net Hierarchical Equal Area isoLatitude Pixelation of a sphere], <ref name="[[:Template:Gorski2005]]">[http://iopscience.iop.org/0004-637X/622/2/759/pdf/0004-637X_622_2_759.pdf '''HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere'''], K. M. G&oacute;rski, E. Hivon, A. J. Banday, B. D. Wandelt, F. K. Hansen, M. Reinecke, M. Bartelmann, ApJ, '''622''', 759-771, (2005). 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 CMBCosmic Microwave background 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 CMBCosmic Microwave background 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 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 CMBCosmic Microwave background map. Those modes are then used to synthesize the U and Q CMBCosmic Microwave background 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 CMBCosmic Microwave background 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.

Summary table with the different masks that have been used by the component separation methods to pre-process and to process the frequency maps and the CMBCosmic Microwave background maps.

Commander 2015 (PR2) Used for diffuse inpainting of input frequency maps Used for constrained Gaussian realization inpaiting of CMBCosmic Microwave background map Description
TMASK NO NO TMASK (the equivalent to PR1 VALMASK) is the confidence mask in temperature that defines the region where the reconstructed CMBCosmic Microwave background is trusted. It can be found inside COM_CMB_IQU-commander-field-Int_2048_R2.01_full.fits.
PMASK NO NO PMASK is the confidence mask in polarization that defines the region where the reconstructed CMBCosmic Microwave background is trusted. It can be found inside COM_CMB_IQU-commander_1024_R2.02_full.fits.
INP_MASK_T NO YES Three masks have been used for inpaiting of CMBCosmic Microwave background maps for specific ranges: three different angular resolution maps (40 arcmin, 7.5 arcmin and full resolution), are produced using different data combinations and foreground models. Each of these are inpainted with their own masks with a constrained Gaussian realization before coadding the three maps in harmonic space.
INP_MASK_P NO YES Mask used for inpainting of the CMBCosmic Microwave background map in polarization.
SEVEM 2015 (PR2) Used for Diffuse Inpainting of foregorund subtracted CMBCosmic Microwave background maps (fgsub-sevem) Used for constrained Gaussian realization inpaiting of CMBCosmic Microwave background map Description
TMASK NO NO TMASK (the equivalent to PR1 VALMASK) is the confidence mask in temperature that defines the region where the reconstructed CMBCosmic Microwave background is trusted. It can be found inside COM_CMB_IQU-sevem-field-Int_2048_R2.01_full.fits.
PMASK NO NO PMASK is the confidence mask in polarization that defines the region where the reconstructed CMBCosmic Microwave background is trusted. It can be found inside COM_CMB_IQU-sevem_1024_R2.02_full.fits.
INP_MASK_T YES NO Point source mask for temperature. This mask is the combination of the 143 and 217 T point source masks used for the inpainting of the foreground subtracted CMBCosmic Microwave background maps at those two frequencies. These two maps have been combined to produce the final CMBCosmic Microwave background map.
INP_MASK_P YES NO Point source mask for polarization. This mask is the combination of the 100 and 143 point source masks used for the inpainting of the foreground subtracted CMBCosmic Microwave background maps at those two frequencies. These two maps have been combined to produce the final CMBCosmic Microwave background map.
INP_MASK_T for the cleaned 100, 143 and 217 GHz CMBCosmic Microwave background YES NO Three temperature point source masks used for the inpainting of the foreground subtracted CMBCosmic Microwave background maps at the considered frequencies:
INP_MASK_P for the cleaned 70, 100 and 143 GHz CMBCosmic Microwave background YES NO Three polarization point source masks used for the inpainting of the foreground subtracted CMBCosmic Microwave background maps at the considered frequencies:
NILC 2015 (PR2) Used for diffuse inpainting of input frequency maps Used for constrained Gaussian realization inpaiting of CMBCosmic Microwave background map Description
TMASK NO NO TMASK (the equivalent to PR1 VALMASK) is the confidence mask in temperature that defines the region where the reconstructed CMBCosmic Microwave background is trusted. It can be found inside COM_CMB_IQU-nilc-field-Int_2048_R2.01_full.fits.
PMASK NO NO PMASK is the confidence mask in polarization that defines the region where the reconstructed CMBCosmic Microwave background is trusted. It can be found inside COM_CMB_IQU-nilc_1024_R2.02_full.fits.
INP_MASK YES NO The pre-processing involves inpainting of the holes in INP_MASK in the frequency maps prior to applying NILC on them. The first mask (nside 2048) has been used for the pre-processing of sky maps for HFI(Planck) High Frequency Instrument channels and second one for LFI(Planck) Low Frequency Instrument channels (nside 1024). They can downloaded here:
SMICA 2015 (PR2) Used for diffuse inpainting of input frequency maps Used for constrained Gaussian realization inpaiting of CMBCosmic Microwave background map Description
TMASK NO YES TMASK (the equivalent to PR1 VALMASK) is the confidence mask in temperature that defines the region where the reconstructed CMBCosmic Microwave background is trusted. It can be found inside COM_CMB_IQU-smica-field-Int_2048_R2.01_full.fits.
PMASK NO YES PMASK is the confidence mask in polarization that defines the region where the reconstructed CMBCosmic Microwave background is trusted. It can be found inside COM_CMB_IQU-smica_1024_R2.02_full.fits.

### Inputs

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

Three sets of files FITSFlexible Image Transfer Specification files containing the CMBCosmic Microwave background 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_CMBCosmic Microwave background_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_CMBCosmic Microwave background_IQU-{method}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits for the regular CMBCosmic Microwave background maps, and
• COM_CMBCosmic Microwave background_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_CMBCosmic Microwave background_IQU-{method}_1024_R2.02_{coverage}.fits

#### Version 2.00 files

These have names like

• COM_CMBCosmic Microwave background_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 CMBCosmic Microwave background 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.

CMBCosmic Microwave background 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
Keyword Data Type Value Description
AST-COMP String CMBCosmic Microwave background 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 given here includes the pixel window function for the Nside=2048 pixelization. It means that, ideally, . The beam Window function is given by

#### Version 2.01 files

These files have names like:

• COM_CMBCosmic Microwave background_IQU-{method}{-field-Int|Pol}_Nside_R2.01_{coverage}.fits for the regular CMBCosmic Microwave background maps, and
• COM_CMBCosmic Microwave background_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 FITSFlexible Image Transfer Specification header.

CMBCosmic Microwave background 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)
Keyword Data Type Value Description
AST-COMP String CMBCosmic Microwave background 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 given here includes the pixel window function for the Nside=2048 pixelization. It means that, ideally, . The beam Window function is given by

#### Version 2.02 files

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

These files have names like:

• COM_CMBCosmic Microwave background_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 FITSFlexible Image Transfer Specification header.

CMBCosmic Microwave background 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)
Keyword Data Type Value Description
AST-COMP String CMBCosmic Microwave background 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 given here includes the pixel window function for the Nside=2048 pixelization. It means that, ideally, . The beam Window function is given by

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

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 FITSFlexible Image Transfer Specification file headers for details.

The quadrupole residual maps are stored in files called:

• COM_CMBCosmic Microwave background_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

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

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

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 FWHMFull-Width-at-Half-Maximum by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256.

#### Outputs

##### Synchrotron emission
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
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
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 FITSFlexible Image Transfer Specification 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
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
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
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
File name: COM_CompMap_SZ-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin
HDU -- COMP-MAP-SZSunyaev-Zel'dovich
Column Name Data Type Units Description
Y_ML Real*4 y_SZSunyaev-Zel'dovich Y parameter posterior maximum
Y_MEAN Real*4 y_SZSunyaev-Zel'dovich Y parameter posterior mean
Y_RMS Real*4 y_SZSunyaev-Zel'dovich Y parameter posterior rms

### High-resolution temperature products

High-resolution foreground products at 7.5 arcmin FWHMFull-Width-at-Half-Maximum are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz.

#### Inputs

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 FWHMFull-Width-at-Half-Maximum by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=2048.

#### Outputs

##### CO J2->1 emission
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
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

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

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 FWHMFull-Width-at-Half-Maximum 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 CMBCosmic Microwave background and thermal dust emission), the corresponding resolution is 10 arcmin FWHMFull-Width-at-Half-Maximum and Nside=1024.

#### Outputs

##### Synchrotron emission
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
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

## CO emission maps

CO rotational transition line emission is present in all HFI(Planck) High Frequency Instrument bands except 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(Planck) High Frequency Instrument maps and to make three types of CO products. A full description of how these products were generated is given in Planck-2013-XIII[7] and Planck-2015-A10[2].

• 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(Planck) High Frequency Instrument channels (as is the case for the other approaches) and are more reliable, especially in the Galactic Plane. The improvement relative to the 2013 release comes from the combined effect of the ADCanalog to digital converter correction, the VLTC correction, and the improved calibration scheme. As a result, the noise level is ~30% lower in the new products, and the maps are much better behaved at high latitudes.
• 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.
• Type 3 product: to generate this product, fixed CO line ratios are assumed and a high-resolution parametric foreground model is fit. In 2013 this product was generated using the Commander-Ruler technique. In 2015, this technique is superseded by the high-resolution Commander-only, used to produce the J=2-1 map presented in [1] and described in Section 5.4 of Planck-2015-A10[2].

Type 1 and 2 maps have been produced using the MILCA algorithm. Commander has been used to produce low resolution CO J=1-0,2-1,3-2 maps (here) and high resolution CO J=2-1 maps (here).

A summary of all the 2015 CO maps can be found in Table 9 from Planck-2015-A10[2], also shown here:

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(Planck) High Frequency Instrument maps (K_CMBCosmic Microwave background) is provided in the header of the data files and in the RIMOreduced IMO. Four maps are given per transition and per type:

• 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 (0 or 1) giving the regions (1) where the CO measurement is not reliable because of some severe identified foreground contamination.

File name: HFI_CompMap_CO-Type1_2048_R2.00.fits
Nside = 2048

Type-1 CO map file data structure
1. EXTNAME = 'COMP-MAP'
Column Name Data Type Units Description
INTEN10 Real*4 K_RJ km/sec The CO(1-0) intensity map
ERR10 Real*4 K_RJ km/sec Uncertainty in the CO(1-0) intensity
NULL10 Real*4 K_RJ km/sec Map built from the half-ring difference maps
MASK10 Byte none Region over which the CO(1-0) intensity is considered reliable
INTEN21 Real*4 K_RJ km/sec The CO(2-1) intensity map
ERR21 Real*4 K_RJ km/sec Uncertainty in the CO(2-1) intensity
NULL21 Real*4 K_RJ km/sec Map built from the half-ring difference maps
MASK21 Byte none Region over which the CO(2-1) intensity is considered reliable
INTEN32 Real*4 K_RJ km/sec The CO(3-2) intensity map
ERR32 Real*4 K_RJ km/sec Uncertainty in the CO(3-2) intensity
NULL32 Real*4 K_RJ km/sec Map built from the half-ring difference maps
MASK32 Byte none Region over which the CO(3-2) intensity is considered reliable
Keyword Data Type Value Description
AST-COMP string CO-TYPE1 Astrophysical compoment name
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
ORDERING String NESTED Healpix ordering
NSIDE Int 2048 Healpix Nside for LFI(Planck) Low Frequency Instrument and HFI(Planck) High Frequency Instrument, respectively
FIRSTPIX Int*4 0 First pixel number
LASTPIX Int*4 50331647 Last pixel number, for LFI(Planck) Low Frequency Instrument and HFI(Planck) High Frequency Instrument, respectively
CNV 1-0 Real*4 value Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s))
CNV 2-1 Real*4 value Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s))
CNV 3-2 Real*4 value Factor to convert CO(3-2) intensityto Kcmb (units Kcmb/(Krj*km/s))

File name: HFI_CompMap_CO-Type2_2048_R2.00.fits
Nside = 2048

Type-2 CO map file data structure
1. EXTNAME = 'COMP-MAP'
Column Name Data Type Units Description
I10 Real*4 K_RJ km/sec The CO(1-0) intensity map
E10 Real*4 K_RJ km/sec Uncertainty in the CO(1-0) intensity
N10 Real*4 K_RJ km/sec Map built from the half-ring difference maps
M10 Byte none Region over which the CO(1-0) intensity is considered reliable
I21 Real*4 K_RJ km/sec The CO(2-1) intensity map
E21 Real*4 K_RJ km/sec Uncertainty in the CO(2-1) intensity
N21 Real*4 K_RJ km/sec Map built from the half-ring difference maps
M21 Byte none Region over which the CO(2-1) intensity is considered reliable
Keyword Data Type Value Description
AST-COMP String CO-TYPE2 Astrophysical compoment name
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
ORDERING String NESTED Healpix ordering
NSIDE Int 2048 Healpix Nside for LFI(Planck) Low Frequency Instrument and HFI(Planck) High Frequency Instrument, respectively
FIRSTPIX Int*4 0 First pixel number
LASTPIX Int*4 50331647 Last pixel number, for LFI(Planck) Low Frequency Instrument and HFI(Planck) High Frequency Instrument, respectively
CNV 1-0 Real*4 value Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s))
CNV 2-1 Real*4 value Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s))

## Modelling of the thermal dust emission with the Draine and Li dust model

The Planck, IRAS, and WISE infrared observations were fit with the dust model presented by Draine & Li in 2007 (DL07). The input maps, the DL07 model, and the fitting procedure and results are presented in Planck-2014-XXIX[8]. Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.

### Inputs

The following data have been fit:

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

The CIB monopole, the CMBCosmic Microwave background 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: 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

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

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

We describe diffuse foreground products for the Planck 2015 release produced with the GNILC component separation method. See the Planck paper Planck-2016-XLVIII[9] for a detailed discussion on these products.

### Method

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 CMBCosmic Microwave background, 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 (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 PLAPlanck Legacy Archive.

### 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 (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 FWHMFull-Width-at-Half-Maximum varying from 21.8' to 5'. The dust beam FWHMFull-Width-at-Half-Maximum map is also released as a product.

#### Thermal dust maps

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_R2.01.fits (version 2.01 includes the error map)
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_R2.01.fits (version 2.01 includes the error map)
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_R2.01.fits (version 2.01 includes the error map)
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 FWHMFull-Width-at-Half-Maximum

#### CIB maps

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

1. Planck 2015 results. XI. Diffuse component separation: CMB maps, Planck Collaboration, 2016, A&A, 594, A9.
2. Planck 2015 results. X. Diffuse component separation: Foreground maps, Planck Collaboration, 2016, A&A, 594, A10.
3. Planck 2015 results. I. Overview of products and results, Planck Collaboration, 2016, A&A, 594, A1.
4. Planck 2015 results. VI. LFI mapmaking, Planck Collaboration, 2016, A&A, 594, A6.
5. Planck 2015 results. VIII. High Frequency Instrument data processing: Calibration and maps, Planck Collaboration, 2016, A&A, 594, A8.
6. Planck 2015 results. XXV. Diffuse low frequency Galactic foregrounds, Planck Collaboration, 2016, A&A, 594, A25.
7. Planck 2013 results. XIII. Galactic CO emission, Planck Collaboration, 2014, A&A, 571, A13
8. Planck intermediate results. XXIX. All-sky dust modelling with Planck, IRAS, and WISE observations', Planck Collaboration Int. XXIX, A&A, 586, A132, (2016).
9. Planck intermediate results. XLVIII. Disentangling Galactic dust emission and cosmic infrared background anisotropies, Planck Collaboration Int. XLVIII A&A, 596, A109, (2016).