Difference between revisions of "Foreground maps"

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= Astrophysical Components=
+
= 2018 Astrophysical Components=
  
 
== 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.
 
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|planck2016-l04}} and {{PlanckPapers|planck20}}.
+
All the details can be found in {{PlanckPapers|planck2016-l04}} and {{PlanckPapers|planck2016-l08}}.
  
 
== Commander-derived astrophysical foreground maps ==
 
== Commander-derived astrophysical foreground maps ==
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=====Thermal dust emission=====
 
=====Thermal dust emission=====
  
−
: Full-mission file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_full.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_full.fits}}
+
: Full-mission file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_full.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_full.fits}}
−
: First half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm1.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_hm1.fits}}
+
: First half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm1.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm1.fits}}
−
: Second half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm2.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_hm2.fits}}
+
: Second half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm2.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm2.fits}}
−
: Odd ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe1.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_oe1.fits}}
+
: Odd ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe1.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe1.fits}}
−
: Even ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe2.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_oe2.fits}}
+
: Even ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe2.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe2.fits}}
 
: Nside = 2048
 
: Nside = 2048
 
: Angular resolution = 5 arcmin
 
: Angular resolution = 5 arcmin
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|Q_STOKES || Real*4 || uK_RJ || Full-mission Stokes Q posterior maximum     
 
|Q_STOKES || Real*4 || uK_RJ || Full-mission Stokes Q posterior maximum     
 
|-
 
|-
−
|U_STOKES || Real*4 || uK_RJ || Full-mission Stokes U posterior maximum      
+
|U_STOKES || Real*4 || uK_RJ || Full-mission Stokes U posterior maximum
 +
|-
 +
|BETA || Real*4 ||  || Spectral index (full mission only)   
 
|}
 
|}
  
 
== SMICA-derived astrophysical foreground maps ==
 
== SMICA-derived astrophysical foreground maps ==
  
−
Two SMICA-based polarization foreground products are provided, namely synchrotron and thermal dust emission. These are derived using the usual SMICA spectral matching method, tuned specifically for the reconstruction of two polarized foregrounds.  Specifically, three coherent components (plus noise) are fitted at the spectral level with the first one constrained to have CMB emissivity.  No assumptions are made regarding the other two components: they are not assumed to have a specific emissivity or angular spectrum, nor are they assumed to be uncorrelated.  This leaves a degenerate model but that degeneracy can be entirely fixed after the fit by assuming that synchrotron emission is negligible at 353 GHz and that thermal dust emission is negligible at 30 GHz. For both synchrotron and thermal dust emission, we provide results derived from both the full-mission data set, and from the half-mission and odd-even splits.
+
Two SMICA-based polarization foreground products are provided, namely synchrotron and thermal dust emission. These are derived using the usual SMICA spectral matching method, tuned specifically for the reconstruction of two polarized foregrounds.  Specifically, three coherent components (plus noise) are fitted at the spectral level with the first one constrained to have CMB emissivity.  No assumptions are made regarding the other two components: they are not assumed to have a specific emissivity or angular spectrum, nor are they assumed to be uncorrelated.  This leaves a degenerate model but that degeneracy can be entirely fixed after the spectral fit by assuming that synchrotron emission is negligible at 353 GHz and that thermal dust emission is negligible at 30 GHz. For both synchrotron and thermal dust emission, we provide results derived from both the full-mission data set, and from the half-mission and odd-even splits.
  
 
In addition to the real observations, we also provide 300 end-to-end noise simulations processed through the algorithm with the same spectral parameters as derived from the data for each of the data splits. The filenames of these simulations have the following format:
 
In addition to the real observations, we also provide 300 end-to-end noise simulations processed through the algorithm with the same spectral parameters as derived from the data for each of the data splits. The filenames of these simulations have the following format:
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=====Thermal dust emission=====
 
=====Thermal dust emission=====
  
−
: Full-mission file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_full.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_full.fits}}
+
: Full-mission file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_full.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_full.fits}}
−
: First half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm1.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_hm1.fits}}
+
: First half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm1.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm1.fits}}
−
: Second half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm2.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_hm2.fits}}
+
: Second half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm2.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm2.fits}}
−
: Odd ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe1.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_oe1.fits}}
+
: Odd ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe1.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe1.fits}}
−
: Even ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe2.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_oe2.fits}}
+
: Even ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe2.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe2.fits}}
 
: Nside = 2048
 
: Nside = 2048
 
: Angular resolution = 12 arcmin
 
: Angular resolution = 12 arcmin
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|}
 
|}
  
−
====GNILC thermal dust maps====
+
==GNILC thermal dust maps==
  
 
The 2018 GNILC thermal dust products are provided as single files that include both intensity and polarization, 3x3 IQU noise covariance matrices per pixel, and as well as local smoothing scale for the variable resolution map. The structure of the data files is the following:
 
The 2018 GNILC thermal dust products are provided as single files that include both intensity and polarization, 3x3 IQU noise covariance matrices per pixel, and as well as local smoothing scale for the variable resolution map. The structure of the data files is the following:
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|-
 
|-
 
|}
 
|}
−
 
−
= Other maps that require special processing =
 
−
 
−
== 2015 Lensing map ==
 
−
 
−
We distribute the minimum-variance (MV) lensing potential estimate presented in {{PlanckPapers|planck2014-a17}} as part of the 2014 data release. This map represents an estimate of the CMB lensing potential on approximately 70% of the sky, and also forms the basis for the Planck 2014 lensing likelihood. It is produced using filtered temperature and polarization data from the SMICA DX11 CMB map; its construction is discussed in detail in {{PlanckPapers|planck2014-a11}}.
 
−
 
−
 
−
The estimate is contained in a single gzipped tarball named  ''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R2.00.tgz|link=COM_CompMap_Lensing_2048_R2.00.tgz}}''. Its contents are described below. The convergence map "dat_klm.fits" that can be found in the tarball, has been categorized as COM_Lensing-Convergence-dat-klm_2048_R2.00.fits in the Lensing Products section of the archive.
 
−
 
−
 
−
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of Lensing package '''
 
−
|-  bgcolor="ffdead" 
 
−
! Filename ||  Format ||  Description
 
−
|-
 
−
| dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Contains the estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math>.
 
−
|-
 
−
| mask.fits.gz || HEALPix FITS format map, with <math>N_{\rm  side}=2048</math> || Contains the lens reconstruction analysis mask.
 
−
|-
 
−
| nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>N_L </math>, <math>C_L+N_L</math>) || The approximate noise <math>N_L</math> (and signal+noise, <math>C_L+N_L</math>) power spectrum of <math> \hat{\kappa}_{LM} </math>, for the fiducial cosmology used in {{PlanckPapers|planck2014-a15}}.
 
−
|}
 
−
 
−
=== Previous Releases: (2013) Lensing Maps ===
 
−
 
−
<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #EEE8AA;width:80%">
 
−
'''2013 Release of the lensing map'''
 
−
<div class="mw-collapsible-content">
 
−
 
−
''' Description '''
 
−
 
−
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of {{PlanckPapers|planck2013-p12}}. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.
 
−
 
−
We distribute:
 
−
 
−
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate <math>\hat{\phi}</math> with the lensing response function <math>R_L^{\phi\phi}</math>. This map has been band-limited between multipoles <math>10 \le L \le 2048</math>.
 
−
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. ''Note'': the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.
 
−
; RLPP : This column contains the response function <math>R_L^{\phi\phi}</math>.
 
−
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, <math>N_L^{\phi\phi}</math>. The noise is highly coloured. There is a dependence of the noise power spectrum on the local noise level of the map, discussed in Appendix A of {{PlanckPapers|planck2013-p12}}. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.
 
−
 
−
Also, the table below gives the lensing curl-mode power spectrum data used to produce Figure A2 of {{PlanckPapers|planck2013-p12}}:
 
−
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center"
 
−
|+ ''''MV' curl reconstruction bandpowers from Fig A2 of {{PlanckPapers|planck2013-p12}} '''
 
−
|-  bgcolor="ffdead" 
 
−
! <math>L</math><sub>min</sub> ||  <math>L</math><sub>max</sub> ||  <math>{\hat{C}_L}^{\psi\psi} (L(L+1))^2/(2\pi)</math> || <math> std({\hat{C}_L}^{\psi\psi})  (L(L+1))^2 /(2\pi)</math>
 
−
|-
 
−
|    2 ||    7 || -13.6379  || 15.3409
 
−
|-
 
−
|    8 ||  20 ||  6.0184  ||  4.8881
 
−
|-
 
−
|    21 ||  39 ||  -1.0675  ||  3.0940
 
−
|-
 
−
|    40 ||  65 ||  0.6135  ||  1.8474
 
−
|-
 
−
|    66 ||  100 ||  1.5030  ||  1.2696
 
−
|-
 
−
|  101 ||  144 ||  1.3760  ||  0.9950
 
−
|-
 
−
|  145 ||  198 ||  -1.2289  ||  0.8286
 
−
|-
 
−
|  199 ||  263 ||  1.1910  ||  0.7001
 
−
|-
 
−
|  264 ||  338 ||  -0.6567  ||  0.6197
 
−
|-
 
−
|  339 ||  425 ||  -0.8201  ||  0.5235
 
−
|-
 
−
|  426 ||  525 ||  -0.7581  ||  0.4850
 
−
|-
 
−
|  526 ||  637 ||  -0.3201  ||  0.5134
 
−
|-
 
−
|  638 ||  762 ||  -0.1589  ||  0.4073
 
−
|-
 
−
|  763 ||  901 ||  -0.6451  ||  0.4044
 
−
|-
 
−
|  902 || 1054 ||  0.4910  ||  0.3718
 
−
|-
 
−
|  1055 || 1221 ||  -0.2186  ||  0.3702
 
−
|-
 
−
|  1222 || 1404 ||  -0.3295  ||  0.4146
 
−
|-
 
−
|  1405 || 1602 ||  -0.3647  ||  0.4703
 
−
|-
 
−
|  1603 || 1816 ||  -0.1060  ||  0.5904
 
−
|-
 
−
|  1817 || 2020 ||  -0.7887  ||  0.8507
 
−
|}
 
−
 
−
 
−
''' Production process '''
 
−
 
−
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of {{PlanckPapers|planck2013-p12}}. The response function <math>R_L^{\phi\phi}</math> here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.
 
−
 
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'''Inputs'''
 
−
 
−
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.
 
−
The analysis mask is constructed from a combination of thresholding in the 857GHz map (to remove the regions which are most contaminated by Galactic dust) and the [[CMB_and_astrophysical_component_maps#CO_emission_maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is joined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs are given in {{PlanckPapers|planck2013-p12}}.
 
−
 
−
'''File names and format'''
 
−
 
−
A single file named
 
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*''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R1.10.fits|link=COM_CompMap_Lensing_2048_R1.10.fits}}''
 
−
with two BINTABLE extensions containing the items described below.
 
−
 
−
For illustration, we show in the figures below the maps of the Wiener-filtered CMB lensing potential in Galactic coordinates using orthographic projection. The reconstruction was bandpass filtered to <math>L \in [10, 2048]</math>. Note that the lensing reconstruction, while highly statistically significant, is still noise dominated for every individual mode, and is at best <math>S/N \simeq 0.7</math> around <math>L = 30</math>.
 
−
 
−
<center>
 
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<gallery perrow=3 widths=260px heights=170px>
 
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File: analysis_lens_pub_map_orth_north_dat_p.png | Galactic north
 
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File: analysis_lens_pub_map_orth_south_dat_p.png | Galactic south
 
−
</gallery></center>
 
−
 
−
 
−
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ '''FITS file structure'''
 
−
|- bgcolor="ffdead" 
 
−
!colspan="4" | 1. EXTNAME = ''LENS-MAP''
 
−
|-  bgcolor="ffdead" 
 
−
! Column Name || Data Type || Units || Description
 
−
|-
 
−
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP
 
−
|-
 
−
|MASK || Int || none || Region over which the lensing potential is reconstructed
 
−
|- bgcolor="ffdead" 
 
−
! Keyword || Data Type || Value || Description
 
−
|-
 
−
|PIXTYPE  ||  string || HEALPIX || colspan="2"|
 
−
|-
 
−
|COORDSYS  ||  string || GALACTIC || Coordinate system
 
−
|-
 
−
|ORDERING  ||  string || NESTED  || Healpix ordering
 
−
|-
 
−
|NSIDE  || Int*4  ||  2048 ||colspan="2"| Healpix Nside
 
−
|-
 
−
|FIRSTPIX || Int*4  ||          0 ||
 
−
|-
 
−
|LASTPIX || Int*4  || 50331647 ||
 
−
|- bgcolor="ffdead" 
 
−
!colspan="4"| 2. EXTNAME = ''TransFun''
 
−
|-  bgcolor="ffdead" 
 
−
! Column Name || Data Type || Units || Description
 
−
|-
 
−
|RLPP || Real*4 || none || Response function
 
−
|-
 
−
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate
 
−
|- bgcolor="ffdead" 
 
−
! Keyword || Data Type || Value || Description
 
−
|-
 
−
|L_MIN || Int*4  ||          0 || First multipole
 
−
|-
 
−
|L_MAX || Int*4  ||  2048 || Last multipole
 
−
|}
 
−
 
−
</div>
 
−
</div>
 
−
 
−
== 2015 Lensing-induced <i>B</i>-mode map ==
 
−
 
−
We distribute the Planck map of the lensing-induced <i>B</i>-modes presented in {{PlanckPapers|planck2015-XLI}}. The Stokes parameter maps of the lensing <i>B</i>-modes are produced by combining the lensing potential map extracted from the SMICA CMB temperature map with <i>E</i>-mode data from the SMICA CMB polarization maps. The SMICA temperature and polarization products are described in {{PlanckPapers|planck2014-a11}}. The lensing-induced <i>B</i>-mode polarization maps are used in cross-correlation with the SMICA CMB polarization maps to obtain a lensing <i>B</i>-mode power spectrum measurement from approximately 70% of the sky.
 
−
 
−
We provide both raw products, which can be utilized to generate products adapted to one's specific needs in term of mask, filtering, etc., and "ready-to-use" products for cross-correlation study purposes.
 
−
 
−
=== Raw products ===
 
−
 
−
We deliver the non-normalized lensing-induced Stokes parameter maps, labelled <math> \bar{Q}^{\rm{lens}} </math> and <math> \bar{U}^{\rm{lens}} </math>, which form the basis of the final lensing <i>B</i>-mode estimator defined in equation (6) of the paper. They are defined as
 
−
 
−
<math> \begin{eqnarray}
 
−
\bar Q^{\rm{lens}}({\bf n}) &=& \widetilde Q^{E}({\bf n}) \cdot \nabla \widetilde \phi({\bf n}), \\
 
−
\bar U^{\rm{lens}}({\bf n}) &=& \widetilde U^{E}({\bf n}) \cdot \nabla \widetilde \phi({\bf n}),
 
−
\end{eqnarray} </math>
 
−
 
−
where <math> \widetilde Q^{E} </math> and  <math> \widetilde U^{E} </math> are the filtered pure <i>E</i>-mode polarization maps given in equation (5), and <math> \widetilde \phi</math> is the filtered lensing potential estimate. 
 
−
 
−
We also provide the normalization transfer function <math> \mathcal{B}_\ell </math> defined in equation (12), as well as the "B70" mask <math> M({\bf n}) </math> that retains 69% of the sky before
 
−
apodization, and its apodized version <math> \tilde{M}({\bf n}) </math>, which has an effective sky fraction <math> f_{\rm{sky}}^{\rm{eff}} = 65\% </math>.
 
−
 
−
As an example of the utilization of these products, the lensing <i>B</i>-mode maps that are shown in figure 4 are generated from
 
−
 
−
<math> Q^{\rm{lens}} \pm i U^{\rm{lens}} = \sum_{\ell m}  \left( G_\ell \mathcal{B}_\ell^{-1}  \int d{\bf n} {\, }_{\pm 2}Y_{\ell m}^*({\bf n}) \left(\bar{Q}^{\rm{lens}} \pm i \bar{U}^{\rm{lens}} \right)  \right)  {\, }_{\pm 2}Y_{\ell m}({\bf n}) </math>,
 
−
 
 
−
where <math>G_\ell</math> is a Gaussian filter of 60 arcmin FWHM (introduced for highlighting large angular scales, although it can be removed or replaced by any other filter). This can be practically done by ingesting <math>\bar{Q}^{\rm{lens}} </math> and <math> \bar{U}^{\rm{lens}} </math> in the HEALPix "smoothing" routine, and using the product <math> G_\ell\mathcal{B}_\ell^{-1} </math> as an input filtering function.
 
−
 
−
The lensing-induced Stokes parameter maps are provided without being masked for the user's convenience (in particular, it allows for various filtering to be tested). However, whenever they are utilized in view of obtaining scientific outcomes, they should be masked using the B70 mask, which is also provided.
 
−
 
−
=== Specific products ===
 
−
 
−
We provide the lensing <i>B</i>-mode spherical harmonic coefficient estimate <math> B_{\ell m}^{\rm{lens}} </math> over approximately 70% of the sky.
 
−
 
−
It can also be constructed using the raw products described above from
 
−
 
−
<math> B_{\ell m}^{\rm{lens}} = f_{10 \rightarrow 2000} \,  \mathcal{B}_\ell^{-1} \, \, {\, }_{\pm 2}\mathcal{Y} \left[ \tilde{M}({\bf n}) \left( \bar{Q}^{\rm{lens}}({\bf n}) \pm i \bar{U}^{\rm{lens}}({\bf n}) \right) \right] </math>,
 
−
 
−
where <math> f_{10 \rightarrow 2000} </math> is a band-pass filter that retain the multipole range <math> 10 \le \ell \le 2000 </math>, and <math> {\, }_{\pm2}\mathcal{Y} </math> is a short-hand notation for transforming a map into spin-weighted spherical harmonic coefficients <math> {\, }_{+2}a_{\ell m}</math>, <math>{\, }_{-2}a_{\ell m} </math> and forming <math>1/(2i)\left({\, }_{+2}a_{\ell m} - {\, }_{-2}a_{\ell m}\right)</math>. This can be done using, e.g., the HEALPix "anafast" tool.
 
−
 
−
The lensing <i>B</i>-mode power spectrum estimate <math> \hat{C}_\ell^{BB^{\rm{lens}}} </math> is obtained by forming the cross-correlation power spectrum of <math> B_{\ell m}^{\rm{lens}} </math> and the <i>B</i>-mode data from the SMICA polarization maps <math> B_{\ell m} </math>:
 
−
 
−
<math> \hat{C}_\ell^{BB^{\rm{lens}}} = \frac{\left(f_{\rm{sky}}^{\rm{eff}}\right)^{-1}}{2 \ell +1} G_\ell^{-2} \sum_m B_{\ell m}^* B_{\ell m}^{\rm{lens}}</math>,
 
−
 
−
where <math> G_\ell </math> is the 5 arcmin Gaussian beam that convolves the SMICA CMB maps.
 
−
 
−
 
−
The products are contained in a single gzipped tarball named [http://pla.esac.esa.int/pla/aio/product-action?COSMOLOGY.FILE_ID=COM_Lensing-Bmode_R2.01.tgz COM_Lensing-Bmode_R2.01.tgz]. Its contents are described below.
 
−
 
−
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of Lensing B-mode package '''
 
−
|-  bgcolor="ffdead" 
 
−
! Filename ||  Format ||  Description
 
−
|-
 
−
| bar_q_lens_map.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math>  || Contains the non-normalized lensing-induced <i>Q</i> Stokes parameter map <math> \bar Q^{\rm{lens}}({\bf n}) </math>.
 
−
|-
 
−
| bar_u_lens_map.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math>  || Contains the non-normalized lensing-induced <i>U</i> Stokes parameter map <math> \bar U^{\rm{lens}}({\bf n}) </math>.
 
−
|-
 
−
| mask.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || The B70 mask (apodized version).
 
−
|-
 
−
| mask_noapo.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || The B70 mask without apodization.
 
−
|-
 
−
| transfer_function_b_l.dat || ASCII text file, with columns = (<math>\ell</math>, <math> \mathcal{B}_\ell </math>) || The transfer function of the lensing B-mode estimator.
 
−
|-
 
−
| lensing_bmode_b_lm.fits || HEALPix FITS format alm, with <math> \ell_{\rm  max} = 2000 </math>  || Contains the lensing <i>B</i>-mode harmonic coefficients <math> B_{\ell m}^{\rm{lens}} </math>.
 
−
|-
 
−
| lensing_bmode_bandpowers.dat || ASCII text file, with columns = (<math>\ell_{\rm  min}</math>, <math>\ell_{\rm  b} </math>,  <math>\ell_{\rm  max} </math>, <math> \hat{C}_{\ell_{\rm b}}^{BB^{\rm{lens}}} </math>, <math> \Delta \hat{C}_{\ell_{\rm b}}^{BB^{\rm{lens}}} </math> )  || The lensing <i>B</i>-mode bandpower estimate on approximativily 70% of the sky and over the multipole range from 10 to 2000 shown in figure 10 of {{PlanckPapers|planck2015-XLI}} (for plotting purposes only).
 
−
|}
 
−
 
−
 
−
== 2015 Compton <i>y</i> parameter map ==
 
−
 
−
We distribute here the Planck full mission Compton parameter maps (<i>y</i>-maps hereafter) obtained using the NILC and MILCA component-separation algorithms as described in {{PlanckPapers|planck2014-a28}}. We also provide the ILC weights per scale and per frequency that were used to produce these <i>y</i>-maps. IDL routines are also provided to allow the user to apply those weights. Compton parameters produced by keeping either the first or the second half of stable pointing periods are also provided; we call these the FIRST and LAST <i>y</i>-maps. Additionally we construct noise estimates of full mission Planck <i>y</i>-maps from the half difference of the FIRST and LAST <i>y</i>-maps. These estimates are used to construct standard deviation maps of the noise in the full mission Planck <i>y</i>-maps, which are also provided. To complement this we also provide the power spectra of the noise estimate maps after correcting for inhomogeneities using the standard deviation maps. We also deliver foreground masks including point-source and Galactic masks.
 
−
 
−
<span style="color:#ff0000"> Update 04 Aug 2017:</span> The file containing the masks named ''COM_CompMap_Compton-SZMap-masks_2048_R2.00.fits'' has been updated with the file ''COM_CompMap_Compton-SZMap-masks_2048_R2.01.fits''. The difference between the two is that in the R2.00 version a region around the Galactic pole had been masked, while only the Galactic plane should be masked. This has been fixed in version R2.01. The full updated data set is contained in a single gzipped tarball named ''COM_CompMap_YSZ_R2.01.fits.tgz''. The R2.00 version of the mask is not available in the PLA anymore, but can be requested via the PLA Helpdesk.
 
−
 
−
The contents of the full data set are described below.
 
−
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of COM_CompMap_YSZ_R2.01.fits.tgz '''
 
−
|-  bgcolor="ffdead" 
 
−
! Filename ||  Format ||  Description
 
−
|-
 
−
| nilc_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math>N_{\rm  side}=2048 </math>|| Contains the NILC full mission, FIRST and LAST <i>y</i>-maps.
 
−
|-
 
−
| milca_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the MILCA full mission, FIRST and LAST <i>y</i>-maps.
 
−
|-
 
−
| nilc_weights_BAND.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 128 </math>|| Contains the NILC ILC weights for the full mission <i>y</i>-map for band BAND 0 to 9. For each band we provide a weight map per frequency.
 
−
|-
 
−
| milca_FREQ_Csz.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the MILCA ILC weights for the full mission <i>y</i>-map for frequency FREQ (100, 143, 217, 353, 545, 857). For each frequency we provide a weight map per filter band.
 
−
|-
 
−
| nilc_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math>|| Contains the stddev map for the NILC full mission <i>y</i>-map.
 
−
|-
 
−
| milca_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the stddev maps for the MILCA full mission <i>y</i>-map.
 
−
|-
 
−
| nilc_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the NILC full mission <i>y</i>-map.
 
−
|-
 
−
| milca_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the MILCA full mission <i>y</i>-map.
 
−
|-
 
−
| masks.fits || HEALPix FITS format map, with <math> N_{\rm  side} = 2048 </math> || Contains foreground masks.
 
−
|-
 
−
| nilc_bands.fits || ASCII table FITS format || Contains NILC wavelet bands in multipole space
 
−
|}
 
−
 
−
== 2015 Integrated Sachs-Wolfe effect map ==
 
−
 
−
We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in {{PlanckPapers|planck2014-a26}} as part of the 2015 data release. These map represents an estimate of the ISW anisotropies using different data sets:
 
−
 
−
* SEVEM DX11 CMB map, together with all the large-scale structure tracers considered in the ISW paper, namely: NVSS, SDSS, WISE, and the Planck lensing map
 
−
* Using only the large-scale structure tracers mentioned above
 
−
* SEVEM DX11 CMB map, together with NVSS and the Planck lensing maps (since these two tracers capture most of the information, as compared to SDSS and WISE)
 
−
 
−
 
−
For all the three cases, the reconstruction is provided on approximately 85% of the sky, and they are produced using the LCB filter described in the Planck ISW paper (Section 5), described in detail in [http://cdsads.u-strasbg.fr/abs/2008ISTSP...2..747B| Barreiro et al. 2008] and [http://cdsads.u-strasbg.fr/doi/10.1093/mnras/stw415| Bonavera et al. 2016].
 
−
 
−
These ISW maps, together with their corresponding uncertainties maps and masks, are given in a file named  ''{{PLASingleFile|fileType=map|name=COM_CompMap_ISW_0064_R2.00.fits|link=COM_CompMap_ISW_0064_R2.00.fits}}''. Its contents are described below.
 
−
 
−
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of the ISW maps file: COM_CompMap_ISW_0064_R2.00.fits '''
 
−
|-  bgcolor="ffdead"
 
−
! Extension ||  Format ||  Description || Used data sets
 
−
|-
 
−
| 0 || HEALPix FITS format map with three components, <math>N_{\rm  side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map ||  SEVEM DX11 CMB + NVSS + SDSS + WISE + Planck lensing.
 
−
|-
 
−
| 1 || HEALPix FITS format map with three components, <math>N_{\rm  side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map ||  NVSS + SDSS + WISE + Planck lensing.
 
−
|-
 
−
| 2 || HEALPix FITS format map with three components, <math>N_{\rm  side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map ||  SEVEM DX11 CMB + NVSS + Planck lensing.
 
−
|}
 
−
 
−
== 2015 Low-frequency foregrounds maps (Planck only & Planck+WMAP) ==
 
−
1) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck only)
 
−
 
−
Linear combination of Planck 28.4, 44.1, 143 and 353 GHz maps (all at 1 degree resolution), with weights listed in column w_2 of Table 1 in {{PlanckPapers|planck2014-a31}}. These weights exactly null the CMB, almost exactly null free-free emission, and null thermal dust emission to high accuracy except along the inner Galactic plane,where the brightness is uncertain by around 20% due to variation in the dust spectrum. The normalisation leaves a beta = -3 power law at the same amplitude as in the Planck 28.4 GHz map. (As presented in Fig. 3a of Planck 2015 Results XXV.)
 
−
 
−
2) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck + WMAP)
 
−
Linear combination of WMAP K, Ka, and Q band, and Planck 28.4, 44.1, 143 and 353 GHz maps (all at 1 degree resolution), with weights listed in column w_3 of Table 1 in {{PlanckPapers|planck2014-a31}}. These weights exactly null the CMB, almost exactly null free-free emission, and null thermal dust emission to high accuracy except along the inner Galactic plane, where the brightness is uncertain by around 20% due to variation in the dust spectrum. The normalisation leaves a beta = -3 power law at the same amplitude as in the Planck 28.4 GHz map. (As presented in Fig. 3b of {{PlanckPapers|planck2014-a31}}.)
 
  
 
= Previous Releases: (2015) and (2013) Foreground Maps =
 
= Previous Releases: (2015) and (2013) Foreground Maps =
Line 472: Line 180:
 
<div class="mw-collapsible-content">
 
<div class="mw-collapsible-content">
  
−
''' 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.
 
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-a12}} and {PlanckPapers|planck20}}.
 
All the details can be found in {{PlanckPapers|planck2014-a12}} and {PlanckPapers|planck20}}.
  
−
''' 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 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}}.
  
Line 505: Line 213:
 
'''Outputs'''
 
'''Outputs'''
  
−
'''Synchrotron emission'''
+
===Synchrotron emission===
  
 
<!--<center>
 
<!--<center>
Line 543: Line 251:
 
|}
 
|}
  
−
'''Free-free emission'''
+
 
 +
===Free-free emission===
  
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}}
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}}
Line 570: Line 279:
  
  
−
'''Spinning dust emission'''
+
===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}}
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}}
Line 625: Line 334:
 
|}
 
|}
  
−
'''CO line emission'''
+
===CO line emission===
  
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}}
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}}
Line 672: Line 381:
 
|}
 
|}
  
−
'''94/100 GHz line emission'''
+
===94/100 GHz line emission===
  
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-commander_0256_R2.00.fits}}
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-commander_0256_R2.00.fits}}
Line 693: Line 402:
 
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.
 
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'''
+
===Thermal dust emission===
  
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}}
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}}
Line 725: Line 434:
 
|}
 
|}
  
−
'''Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters'''
+
===Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters===
  
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SZ-commander_0256_R2.00.fits|link=COM_CompMap_SZ-commander_0256_R2.00.fits}}
 
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SZ-commander_0256_R2.00.fits|link=COM_CompMap_SZ-commander_0256_R2.00.fits}}
Line 1,046: Line 755:
  
  
−
''' Other Special maps '''
 
  
−
'''Introduction'''
 
  
−
This section describes the map-based products that required special processing.
+
== 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.  
  
−
''' 2015 lensing map '''
+
===Method===
  
−
We distribute the minimum-variance (MV) lensing potential estimate presented in {{PlanckPapers|planck2014-a17}} as part of the 2014 data release. This map represents an estimate of the CMB lensing potential on approximately 70% of the sky, and also forms the basis for the Planck 2014 lensing likelihood. It is produced using filtered temperature and polarization data from the SMICA DX11 CMB map; its construction is discussed in detail in {{PlanckPapers|planck2014-a11}}.
+
: 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 estimate is contained in a single gzipped tarball named ''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R2.00.tgz|link=COM_CompMap_Lensing_2048_R2.00.tgz}}''. Its contents are described below. The convergence map "dat_klm.fits" that can be found in the tarball, has been categorized as COM_Lensing-Convergence-dat-klm_2048_R2.00.fits in the Lensing Products section of the archive.
+
: 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.
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
+
===GNILC thermal dust and CIB products===
−
|+ ''' Contents of Lensing package '''
 
−
|-  bgcolor="ffdead" 
 
−
! Filename ||  Format ||  Description
 
−
|-
 
−
| dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Contains the estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math>.
 
−
|-
 
−
| mask.fits.gz || HEALPix FITS format map, with <math>N_{\rm  side}=2048</math> || Contains the lens reconstruction analysis mask.
 
−
|-
 
−
| nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>N_L </math>, <math>C_L+N_L</math>) || The approximate noise <math>N_L</math> (and signal+noise, <math>C_L+N_L</math>) power spectrum of <math> \hat{\kappa}_{LM} </math>, for the fiducial cosmology used in {{PlanckPapers|planck2014-a15}}.
 
−
|}
 
  
−
''' 2015 Compton <i>y</i> parameter map '''
+
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.
  
−
We distribute here the Planck full mission Compton parameter maps (<i>y</i>-maps hereafter) obtained using the NILC and MILCA component-separation algorithms as described in {{PlanckPapers|planck2014-a28}}. We also provide the ILC weights per scale and per frequency that were used to produce these <i>y</i>-maps. IDL routines are also provided to allow the user to apply those weights. Compton parameters produced by keeping either the first or the second half of stable pointing periods are also provided; we call these the FIRST and LAST <i>y</i>-maps. Additionally we construct noise estimates of full mission Planck <i>y</i>-maps from the half difference of the FIRST and LAST <i>y</i>-maps. These estimates are used to construct standard deviation maps of the noise in the full mission Planck <i>y</i>-maps, which are also provided. To complement this we also provide the power spectra of the noise estimate maps after correcting for inhomogeneities using the standard deviation maps. We also deliver foreground masks including point-source and Galactic masks.
+
====Thermal dust maps====
  
−
The full data set is contained in a single gzipped tarball named  ''COM_CompMap_YSZ_R2.00.fits.tgz''. Its contents are described below.
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
''Temporarily the tarball file can be found in the Supplement Data area of the PLA (go to pla.esac.esa.int/pla, go to Subsection Supplementary Data and type "YSZ" in the search form)''
+
|+ HDU -- COMP-MAP-DUST
−
 
 
−
 
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of COM_CompMap_YSZ_R2.00.fits.tgz} '''
 
−
|- bgcolor="ffdead" 
 
−
! Filename ||  Format ||  Description
 
 
|-
 
|-
−
| nilc_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math>N_{\rm  side}=2048 </math>|| Contains the NILC full mission, FIRST and LAST <i>y</i>-maps.
+
|- bgcolor="ffdead" 
 +
! File Name || Nside || Units || Reference frequency || Angular resolution || Description
 
|-
 
|-
−
| milca_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the MILCA full mission, FIRST and LAST <i>y</i>-maps.
+
|{{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
 
|-
 
|-
−
| nilc_weights_BAND.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 128 </math>|| Contains the NILC ILC weights for the full mission <i>y</i>-map for band BAND 0 to 9. For each band we provide a weight map per frequency.
+
|{{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
 
|-
 
|-
−
| milca_FREQ_Csz.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the MILCA ILC weights for the full mission <i>y</i>-map for frequency FREQ (100, 143, 217, 353, 545, 857). For each frequency we provide a weight map per filter band.
+
|{{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
 
|-
 
|-
−
| nilc_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math>|| Contains the stddev map for the NILC full mission <i>y</i>-map.
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{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
 
|-
 
|-
−
| milca_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the stddev maps for the MILCA full mission <i>y</i>-map.
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{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
 
|-
 
|-
−
| nilc_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the NILC full mission <i>y</i>-map.
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{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
 
|-
 
|-
−
| milca_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the MILCA full mission <i>y</i>-map.
+
|{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Radiance_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Radiance_2048_R2.00.fits}} || 2048 || W/m<sup>2</sup>/sr || 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 radiance
 
|-
 
|-
−
| masks.fits || HEALPix FITS format map, with <math> N_{\rm  side} = 2048 </math> || Contains foreground masks.
+
| {{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}} || 128 || Arcminute || NA || NA || Effective dust beam FWHM
 
|-
 
|-
−
| nilc_bands.fits || ASCII table FITS format || Contains NILC wavelet bands in multipole space
 
 
|}
 
|}
  
−
''' 2015 lensing-induced <i>B</i>-mode map '''
+
====CIB maps====
  
−
We distribute the lensing-induced <i>B</i>-mode map presented in {{PlanckPapers|planck2015-XLI}}. The lensing <i>B</i>-mode Stokes parameter maps are produced by combining the lensing potential reconstruction from the SMICA CMB temperature map with <i>E</i>-mode data from the SMICA CMB polarization maps. The SMICA temperature and polarization products are described in {{PlanckPapers|planck2014-a11}}. The lensing-induced <i>B</i>-mode polarization maps are used in cross-correlation with the SMICA CMB polarization maps to obtain a lensing <i>B</i>-mode power spectrum measurement from approximately 70% of the sky, as described in {{PlanckPapers|planck2015-XLI}}.
 
  
−
We provide both raw products, which can be utilized to generate products adapted to one's specific needs in term of mask, filtering, etc., and "ready-to-use" products for cross-correlation study purposes.  
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-CIB
 +
|-
 +
|- bgcolor="ffdead"  
 +
! File Name || Nside || Units || Reference frequency || Angular resolution || Description
 +
|-
 +
|{{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
 +
|-
 +
|{{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
 +
|-
 +
|{{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
 +
|-
 +
|}
  
−
''' Raw products '''
 
  
−
We deliver the non-normalized lensing-induced Stokes parameter maps, labelled <math> \bar{Q}^{\rm{lens}} </math> and <math> \bar{U}^{\rm{lens}} </math>, which form the basis of the final lensing <i>B</i>-mode estimator defined in equation (6) of {{PlanckPapers|planck2015-XLI}}. They are defined as
+
== Other Special maps ==
  
−
<math> \begin{eqnarray}
+
===Introduction===
−
\bar Q^{\rm{lens}}({\bf n}) &=& \widetilde Q^{E}({\bf n}) \cdot \nabla \widetilde \phi({\bf n}), \\
 
−
\bar U^{\rm{lens}}({\bf n}) &=& \widetilde U^{E}({\bf n}) \cdot \nabla \widetilde \phi({\bf n}),
 
−
\end{eqnarray} </math>
 
  
−
where <math> \widetilde Q^{E} </math> and  <math> \widetilde U^{E} </math> are the filtered pure <i>E</i>-mode polarization maps given in equation (5) of {{PlanckPapers|planck2015-XLI}}, and <math> \widetilde \phi</math> is the filtered lensing potential estimate.
+
This section describes the map-based products that required special processing.
  
−
We also provide the normalization transfer function <math> \mathcal{B}_\ell </math> defined in equation (11) of {{PlanckPapers|planck2015-XLI}}, as well as the "L70" mask <math> M({\bf n}) </math> that retains 69% of the sky before
 
−
apodization, and its apodized version <math> \tilde{M}({\bf n}) </math>, which has an effective sky fraction <math> f_{\rm{sky}}^{\rm{eff}} = 65\% </math>.
 
  
−
As an example of the utilization of these products, the lensing <i>B</i>-mode maps that are shown in figure 4 of {{PlanckPapers|planck2015-XLI}} are generated from
+
=== 2015 Compton <i>y</i> parameter map ===
−
 
−
<math> Q^{\rm{lens}} \pm i U^{\rm{lens}} = \sum_{\ell m}  \left( G_\ell \mathcal{B}_\ell^{-1}  \int d{\bf n} {\, }_{\pm 2}Y_{\ell m}^*({\bf n}) \left(\bar{Q}^{\rm{lens}} \pm i \bar{U}^{\rm{lens}} \right)  \right)  {\, }_{\pm 2}Y_{\ell m}({\bf n}) </math>,
 
−
 
 
−
where <math>G_\ell</math> is a Gaussian of 60 arcmin FWHM (introduced for highlighting large angular scales, although it can be removed or replaced by any other filter). This can be practically done by ingesting <math>\bar{Q}^{\rm{lens}} </math> and <math> \bar{U}^{\rm{lens}} </math> in the HEALPix "smoothing" routine, and using the product <math> G_\ell\mathcal{B}_\ell^{-1} </math> as an input filtering function.
 
  
−
''' Specific products '''
+
We distribute here the Planck full mission Compton parameter maps (<i>y</i>-maps hereafter) obtained using the NILC and MILCA component-separation algorithms as described in {{PlanckPapers|planck2014-a28}}. We also provide the ILC weights per scale and per frequency that were used to produce these <i>y</i>-maps. IDL routines are also provided to allow the user to apply those weights [[:File: milca_nilc_IDL_routines.zip]]. Compton parameters produced by keeping either the first or the second half of stable pointing periods are also provided; we call these the FIRST and LAST <i>y</i>-maps. Additionally we construct noise estimates of full mission Planck <i>y</i>-maps from the half difference of the FIRST and LAST <i>y</i>-maps. These estimates are used to construct standard deviation maps of the noise in the full mission Planck <i>y</i>-maps, which are also provided. To complement this we also provide the power spectra of the noise estimate maps after correcting for inhomogeneities using the standard deviation maps. We also deliver foreground masks including point-source and Galactic masks.
  
−
We provide the lensing <i>B</i>-mode spherical harmonic coefficient estimate <math> B_{\ell m}^{\rm{lens}} </math> over approximately 70% of the sky.  
+
<span style="color:#ff0000"> Update 04 Aug 2017:</span> The file containing the masks named ''COM_CompMap_Compton-SZMap-masks_2048_R2.00.fits'' has been updated with the file ''COM_CompMap_Compton-SZMap-masks_2048_R2.01.fits''. The difference between the two is that in the R2.00 version a region around the Galactic pole had been masked, while only the Galactic plane should be masked. This has been fixed in version R2.01. The full updated data set is contained in a single gzipped tarball named ''COM_CompMap_YSZ_R2.01.fits.tgz''. The R2.00 version of the mask is not available in the PLA anymore, but can be requested via the PLA Helpdesk.
  
−
It can also be constructed using the raw products described above from
+
<span style="color:#ff0000"> Update 30 July 2018:</span> The angular power spectra homogeneous noise files nilc_homnoise_spect.fits and milca_homnoise_spect.fits in COM_CompMap_YSZ_R2.01.fits.tgz have been updated. A new version of the COM_CompMap_SZ_R2.02.fits.tgz package is available in the PLA.
−
 
 
−
<math> B_{\ell m}^{\rm{lens}} = f_{10 \rightarrow 2000} \,  \mathcal{B}_\ell^{-1} \, \, {\, }_{\pm 2}\mathcal{Y} \left[ \tilde{M}({\bf n}) \left( \bar{Q}^{\rm{lens}}({\bf n}) \pm i \bar{U}^{\rm{lens}}({\bf n}) \right) \right] </math>,
 
−
 
 
−
where <math> f_{10 \rightarrow 2000} </math> is a function for producing band-powers over the range <math> 10 \le \ell \le 2000 </math>, and <math> {\, }_{\pm2}\mathcal{Y} </math> is a short-hand notation for transforming a map into spin-weighted spherical harmonic coefficients <math> {\, }_{+2}a_{\ell m}</math>, <math>{\, }_{-2}a_{\ell m} </math> and forming <math>1/(2i)\left({\, }_{+2}a_{\ell m} - {\, }_{-2}a_{\ell m}\right)</math>. This can be done using, e.g., the HEALPix "anafast" tool.
 
−
 
 
−
The lensing <i>B</i>-mode power spectrum estimate <math> \hat{C}_\ell^{BB^{\rm{lens}}} </math> discussed in {{PlanckPapers|planck2015-XLI}} is obtained by forming the cross-correlation power spectrum of <math> B_{\ell m}^{\rm{lens}} </math> and the <i>B</i>-mode data from the SMICA polarization maps <math> B_{\ell m} </math>:
 
−
 
−
<math> \hat{C}_\ell^{BB^{\rm{lens}}} = \frac{\left(f_{\rm{sky}}^{\rm{eff}}\right)^{-1}}{2 \ell +1} G_\ell^{-2} \sum_m B_{\ell m}^* B_{\ell m}^{\rm{lens}}</math>,
 
−
 
 
−
where <math> G_\ell </math> is the 5 arcmin Gaussian beam that convolves the SMICA CMB maps.  
 
−
 
 
−
 
 
−
The products are contained in a single gzipped tarball named  ''{{PLASingleFile|fileType=map|name=COM_Lensing-Bmode_R2.00.tgz|link=COM_Lensing-Bmode_R2.00.tgz}}''. Its contents are described below.
 
  
 +
The contents of the full data set are described below.
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
−
|+ ''' Contents of Lensing B-mode package '''
+
|+ ''' Contents of COM_CompMap_YSZ_R2.02.fits.tgz '''
 
|-  bgcolor="ffdead"   
 
|-  bgcolor="ffdead"   
 
! Filename ||  Format ||  Description
 
! Filename ||  Format ||  Description
 
|-
 
|-
−
| bar_q_lens_map.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the non-normalized lensing-induced <i>Q</i> Stokes parameter map <math> \bar Q^{\rm{lens}}({\bf n}) </math>.
+
| nilc_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math>N_{\rm  side}=2048 </math>|| Contains the NILC full mission, FIRST and LAST <i>y</i>-maps.
 +
|-
 +
| milca_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the MILCA full mission, FIRST and LAST <i>y</i>-maps.
 +
|-
 +
| nilc_weights_BAND.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 128 </math>|| Contains the NILC ILC weights for the full mission <i>y</i>-map for band BAND 0 to 9. For each band we provide a weight map per frequency.
 +
|-
 +
| milca_FREQ_Csz.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the MILCA ILC weights for the full mission <i>y</i>-map for frequency FREQ (100, 143, 217, 353, 545, 857). For each frequency we provide a weight map per filter band.
 
|-
 
|-
−
| bar_u_lens_map.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the non-normalized lensing-induced <i>U</i> Stokes parameter map <math> \bar U^{\rm{lens}}({\bf n}) </math>.
+
| nilc_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math>|| Contains the stddev map for the NILC full mission <i>y</i>-map.
 
|-
 
|-
−
| mask.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || The L70 mask.
+
| milca_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || Contains the stddev maps for the MILCA full mission <i>y</i>-map.
 
|-
 
|-
−
| mask_noapo.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || The L70 mask without apodization.
+
| nilc_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the NILC full mission <i>y</i>-map.
 
|-
 
|-
−
| transfer_function_b_l.dat || ASCII text file, with columns = (<math>\ell</math>, <math> \mathcal{B}_\ell </math>) || The transfer function.
+
| milca_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the MILCA full mission <i>y</i>-map.
 
|-
 
|-
−
| lensing_bmode_b_lm.fits || HEALPix FITS format alm, with <math> \ell_{\rm  max} = 2000 </math> || Contains the lensing <i>B</i>-mode harmonic coefficients <math> B_{\ell m}^{\rm{lens}} </math>.
+
| masks.fits || HEALPix FITS format map, with <math> N_{\rm  side} = 2048 </math> || Contains foreground masks.
 
|-
 
|-
−
| lensing_bmode_bandpowers.dat || ASCII text file, with columns = (<math>\ell_{\rm  min}</math>, <math>\ell_{\rm  b} </math>,  <math>\ell_{\rm  max} </math>, <math> \hat{C}_{\ell_{\rm b}}^{BB^{\rm{lens}}} </math>, <math> \Delta \hat{C}_{\ell_{\rm b}}^{BB^{\rm{lens}}} </math> )  || The lensing <i>B</i>-mode bandpower estimate on approximativily 70% of the sky and over the multipole range from 10 to 2000 shown in figure 9 of {{PlanckPapers|planck2015-XLI}} (for plotting purposes only).
+
| nilc_bands.fits || ASCII table FITS format || Contains NILC wavelet bands in multipole space
 
|}
 
|}
  
−
''' 2015 Integrated Sachs-Wolfe effect map '''
+
=== 2015 Integrated Sachs-Wolfe effect map ===
  
 
We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in {{PlanckPapers|planck2014-a26}} as part of the 2015 data release. These map represents an estimate of the ISW anisotropies using different data sets:
 
We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in {{PlanckPapers|planck2014-a26}} as part of the 2015 data release. These map represents an estimate of the ISW anisotropies using different data sets:
Line 1,180: Line 870:
 
* Using only the large-scale structure tracers mentioned above
 
* Using only the large-scale structure tracers mentioned above
 
* SEVEM DX11 CMB map, together with NVSS and the Planck lensing maps (since these two tracers capture most of the information, as compared to SDSS and WISE)
 
* SEVEM DX11 CMB map, together with NVSS and the Planck lensing maps (since these two tracers capture most of the information, as compared to SDSS and WISE)
−
 
  
 
For all the three cases, the reconstruction is provided on approximately 85% of the sky, and they are produced using the LCB filter described in the Planck ISW paper (Section 5), described in detail in [http://cdsads.u-strasbg.fr/abs/2008ISTSP...2..747B| Barreiro et al. 2008] and [http://cdsads.u-strasbg.fr/doi/10.1093/mnras/stw415| Bonavera et al. 2016].
 
For all the three cases, the reconstruction is provided on approximately 85% of the sky, and they are produced using the LCB filter described in the Planck ISW paper (Section 5), described in detail in [http://cdsads.u-strasbg.fr/abs/2008ISTSP...2..747B| Barreiro et al. 2008] and [http://cdsads.u-strasbg.fr/doi/10.1093/mnras/stw415| Bonavera et al. 2016].
Line 1,198: Line 887:
 
| 2 || HEALPix FITS format map with three components, <math>N_{\rm  side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map ||  SEVEM DX11 CMB + NVSS + Planck lensing.
 
| 2 || HEALPix FITS format map with three components, <math>N_{\rm  side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map ||  SEVEM DX11 CMB + NVSS + Planck lensing.
 
|}
 
|}
 +
 +
 +
=== 2015 Low-frequency foregrounds maps (Planck only & Planck+WMAP) ===
 +
1) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck only)
 +
 +
Linear combination of Planck 28.4, 44.1, 143 and 353 GHz maps (all at 1 degree resolution), with weights listed in column w_2 of Table 1 in {{PlanckPapers|planck2014-a31}}. These weights exactly null the CMB, almost exactly null free-free emission, and null thermal dust emission to high accuracy except along the inner Galactic plane,where the brightness is uncertain by around 20% due to variation in the dust spectrum. The normalisation leaves a beta = -3 power law at the same amplitude as in the Planck 28.4 GHz map. (As presented in Fig. 3a of Planck 2015 Results XXV.)
 +
 +
2) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck + WMAP)
 +
Linear combination of WMAP K, Ka, and Q band, and Planck 28.4, 44.1, 143 and 353 GHz maps (all at 1 degree resolution), with weights listed in column w_3 of Table 1 in {{PlanckPapers|planck2014-a31}}. These weights exactly null the CMB, almost exactly null free-free emission, and null thermal dust emission to high accuracy except along the inner Galactic plane, where the brightness is uncertain by around 20% due to variation in the dust spectrum. The normalisation leaves a beta = -3 power law at the same amplitude as in the Planck 28.4 GHz map. (As presented in Fig. 3b of {{PlanckPapers|planck2014-a31}}.)
  
 
</div>
 
</div>

Latest revision as of 17:33, 22 October 2021

2018 Astrophysical Components[edit]

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-2020-A4[1] and Planck-2020-A8[2].

Commander-derived astrophysical foreground maps[edit]

As discussed in detail in Planck-2020-A4[1], the main Planck 2018 frequency sky maps have significantly lower systematic errors than earlier versions. At the same time, these maps are also associated with a significant limitation, in that no robust single detector or detector set maps are available. As described in Planck-2020-A3[3], such maps do not contain the full signal content of the true sky. As a result, only full frequency maps are distributed and used in the 2018 analysis.

For polarization analysis, this is not a significant issue, and the 2018 polarization foreground products therefore supersede the 2015 release in all respects. However, for temperature analysis the lack of single-detector maps strongly limits the ability to extract CO line emission from the data set, and it is also not possible to exclude known detector outliers; see Planck-2015-A10[4] for details. For these reasons, we consider the parametric foreground products from 2015 to represent a more accurate description of the true sky than the corresponding 2018 version. As a result, we do not release parametric temperature foreground products from the 2018 data set, but rather recommend continued usage of the 2015 temperature model. For polarization, we recommend usage of the 2018 model.


Two Commander-based polarization foreground products are provided for the Planck 2018 releaes, namely synchrotron and thermal dust emission. For synchrotron emission, a spatially constant spectral index of β=-3.1 is adopted. For thermal dust emission, the dust temperature is fixed to that derived from the corresponding 2018 intensity analysis, while the spectral index is fitted directly from the polarization measurements, smoothed to 3 degrees FWHM. For both synchrotron and thermal dust emission, we provide results derived from both the full-mission data set, and from the half-mission and odd-even splits.

In addition to the real observations, we also provide 300 end-to-end noise simulations processed through the algorithm with the same spectral parameters as derived from the data for each of the data splits. The filenames of these simulations have the following format:

  • dx12_v3_commander_{synch,dust}_noise_{full,hm1,hm2,oe1,oe2}_00???_raw.fits

Inputs[edit]

The following data products are used for the full-mission polarization analysis (corresponding data are used for the data split products):

Outputs[edit]

Synchrotron emission[edit]
Full-mission file name: COM_CompMap_QU_synchrotron-commander_2048_R3.00_full.fits
First half-mission split file name: COM_CompMap_QU_synchrotron-commander_2048_R3.00_hm1.fits
Second half-mission split file name: COM_CompMap_QU_synchrotron-commander_2048_R3.00_hm2.fits
Odd ring split file name: COM_CompMap_QU_synchrotron-commander_2048_R3.00_oe1.fits
Even ring split file name: COM_CompMap_QU_synchrotron-commander_2048_R3.00_oe2.fits
Nside = 2048
Angular resolution = 40 arcmin
Reference frequency: 30 GHz
HDU -- COMP-MAP
Column Name Data Type Units Description
Q_STOKES Real*4 μK_RJ Stokes Q posterior maximum
U_STOKES Real*4 μK_RJ Stokes U posterior maximum
Thermal dust emission[edit]
Full-mission file name: COM_CompMap_QU_thermaldust-commander_2048_R3.00_full.fits
First half-mission split file name: COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm1.fits
Second half-mission split file name: COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm2.fits
Odd ring split file name: COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe1.fits
Even ring split file name: COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe2.fits
Nside = 2048
Angular resolution = 5 arcmin
Reference frequency: 353 GHz
HDU -- COMP-MAP
Column Name Data Type Units Description
Q_STOKES Real*4 uK_RJ Full-mission Stokes Q posterior maximum
U_STOKES Real*4 uK_RJ Full-mission Stokes U posterior maximum
BETA Real*4 Spectral index (full mission only)

SMICA-derived astrophysical foreground maps[edit]

Two SMICA-based polarization foreground products are provided, namely synchrotron and thermal dust emission. These are derived using the usual SMICA spectral matching method, tuned specifically for the reconstruction of two polarized foregrounds. Specifically, three coherent components (plus noise) are fitted at the spectral level with the first one constrained to have CMB emissivity. No assumptions are made regarding the other two components: they are not assumed to have a specific emissivity or angular spectrum, nor are they assumed to be uncorrelated. This leaves a degenerate model but that degeneracy can be entirely fixed after the spectral fit by assuming that synchrotron emission is negligible at 353 GHz and that thermal dust emission is negligible at 30 GHz. For both synchrotron and thermal dust emission, we provide results derived from both the full-mission data set, and from the half-mission and odd-even splits.

In addition to the real observations, we also provide 300 end-to-end noise simulations processed through the algorithm with the same spectral parameters as derived from the data for each of the data splits. The filenames of these simulations have the following format:

  • dx12_v3_smica_{synch,dust}_noise_{full,hm1,hm2,oe1,oe2}_00???_raw.fits

Inputs[edit]

The following data products are used for the full-mission polarization analysis (corresponding data are used for the data split products):

Outputs[edit]

Synchrotron emission[edit]
Full-mission file name: COM_CompMap_QU_synchrotron-smica_2048_R3.00_full.fits
First half-mission split file name: COM_CompMap_QU_synchrotron-smica_2048_R3.00_hm1.fits
Second half-mission split file name: COM_CompMap_QU_synchrotron-smica_2048_R3.00_hm2.fits
Odd ring split file name: COM_CompMap_QU_synchrotron-smica_2048_R3.00_oe1.fits
Even ring split file name: COM_CompMap_QU_synchrotron-smica_2048_R3.00_oe2.fits
Nside = 2048
Angular resolution = 40 arcmin
Reference frequency: Integrated 30 GHz band; no colour corrections have been applied
HDU -- COMP-MAP
Column Name Data Type Units Description
Q_STOKES Real*4 mK_RJ Stokes Q posterior maximum
U_STOKES Real*4 mK_RJ Stokes U posterior maximum
Thermal dust emission[edit]
Full-mission file name: COM_CompMap_QU_thermaldust-smica_2048_R3.00_full.fits
First half-mission split file name: COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm1.fits
Second half-mission split file name: COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm2.fits
Odd ring split file name: COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe1.fits
Even ring split file name: COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe2.fits
Nside = 2048
Angular resolution = 12 arcmin
Reference frequency: Integrated 353 GHz band; no colour corrections have been applied
HDU -- COMP-MAP
Column Name Data Type Units Description
Q_STOKES Real*4 mK_RJ Full-mission Stokes Q posterior maximum
U_STOKES Real*4 mK_RJ Full-mission Stokes U posterior maximum

GNILC thermal dust maps[edit]

The 2018 GNILC thermal dust products are provided as single files that include both intensity and polarization, 3x3 IQU noise covariance matrices per pixel, and as well as local smoothing scale for the variable resolution map. The structure of the data files is the following:

Uniform resolution file name: COM_CompMap_IQU_thermaldust-gnilc-unires_2048_R3.00.fits
Variable resolution file name: COM_CompMap_IQU_thermaldust-gnilc-varres_2048_R3.00.fits
Nside = 2048
Angular resolution = 80 arcmin FWHM, or variable
Reference frequency: Integrated 353 GHz band; no colour corrections have been applied
HDU -- COMP-MAP
Column Name Data Type Units Description
I_STOKES Real*4 K_cmb Stokes I estimate
Q_STOKES Real*4 K_cmb Stokes Q estimate
U_STOKES Real*4 K_cmb Stokes U estimate
II_COV Real*4 K_cmb^2 Covariance matrix II element
IQ_COV Real*4 K_cmb^2 Covariance matrix IQ element
IU_COV Real*4 K_cmb^2 Covariance matrix IU element
QQ_COV Real*4 K_cmb^2 Covariance matrix QQ element
QU_COV Real*4 K_cmb^2 Covariance matrix QU element
UU_COV Real*4 K_cmb^2 Covariance matrix UU element
FWHM Real*4 arcmin Local FWHM smoothing scale

Previous Releases: (2015) and (2013) Foreground Maps[edit]

Expand

Astrophysical components based on the 2015 data release

Expand

Astrophysical components based on the 2013 data release

References[edit]

  1. ↑ Jump up to: 1.01.1 Planck 2018 results. IV. Diffuse component separation, Planck Collaboration, 2020, A&A, 641, A4.
  2. Jump up ↑ Planck 2018 results. VIII. Lensing, Planck Collaboration, 2020, A&A, 641, A8.
  3. Jump up ↑ Planck 2018 results. III. High Frequency Instrument data processing and frequency maps, Planck Collaboration, 2020, A&A, 641, A3.
  4. ↑ Jump up to: 4.04.14.2 Planck 2015 results. X. Diffuse component separation: Foreground maps, Planck Collaboration, 2016, A&A, 594, A10.
  5. ↑ Jump up to: 5.05.15.25.3 Planck 2015 results. XXV. Diffuse low frequency Galactic foregrounds, Planck Collaboration, 2016, A&A, 594, A25.
  6. Jump up ↑ Planck intermediate results. XXIX. All-sky dust modelling with Planck, IRAS, and WISE observations', Planck Collaboration Int. XXIX, A&A, 586, A132, (2016).
  7. Jump up ↑ Planck intermediate results. XLVIII. Disentangling Galactic dust emission and cosmic infrared background anisotropies, Planck Collaboration Int. XLVIII A&A, 596, A109, (2016).
  8. Jump up ↑ Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect, Planck Collaboration, 2016, A&A, 594, A22.
  9. Jump up ↑ Planck 2015 results. XXI. The integrated Sachs-Wolfe effect, Planck Collaboration, 2016, A&A, 594, A21.
  10. ↑ Jump up to: 10.010.110.210.310.410.510.610.7 Planck 2013 results. XI. Component separation, Planck Collaboration, 2014, A&A, 571, A11.
  11. Jump up ↑ Component separation methods for the PLANCK mission, S. M. Leach, J.-F. Cardoso, C. Baccigalupi, R. B. Barreiro, M. Betoule, J. Bobin, A. Bonaldi, J. Delabrouille, G. de Zotti, C. Dickinson, H. K. Eriksen, J. González-Nuevo, F. K. Hansen, D. Herranz, M. Le Jeune, M. López-Caniego, E. Martínez-González, M. Massardi, J.-B. Melin, M.-A. Miville-Deschênes, G. Patanchon, S. Prunet, S. Ricciardi, E. Salerno, J. L. Sanz, J.-L. Starck, F. Stivoli, V. Stolyarov, R. Stompor, P. Vielva, A&A, 491, 597-615, (2008).
  12. Jump up ↑ Multiresolution internal template cleaning: an application to the Wilkinson Microwave Anisotropy Probe 7-yr polarization data, R. Fernández-Cobos, P. Vielva, R. B. Barreiro, E. Martínez-González, MNRAS, 420, 2162-2169, (2012).
  13. Jump up ↑ Wilkinson Microwave Anisotropy Probe 7-yr constraints on fNL with a fast wavelet estimator, B. Casaponsa, R. B. Barreiro, A. Curto, E. Martínez-González, P. Vielva, MNRAS, 411, 2019-2025, (2011).
  14. ↑ Jump up to: 14.014.1 Planck 2013 results. XXIII. Isotropy and statistics of the CMB, Planck Collaboration, 2014, A&A, 571, A23.
  15. ↑ Jump up to: 15.015.1 Planck 2013 results. XIX. The integrated Sachs-Wolfe effect, Planck Collaboration, 2014, A&A, 571, A19.
  16. ↑ Jump up to: 16.016.1 Planck 2013 results. XII. All-sky model of thermal dust emission, Planck Collaboration, 2014, A&A, 571, A12.
  17. Jump up ↑ Calibrating Milky Way dust extinction using cosmological sources, E. Mörtsell, A&A, 550, A80, (2013).
  18. Jump up ↑ The Sloan Digital Sky Survey Quasar Catalog. IV. Fifth Data Release, D. P. Schneider, P. B. Hall, G. T. Richards, M. A. Strauss, D. E. Vanden Berk, S. F. Anderson, W. N. Brandt, X. Fan, S. Jester, J. Gray, J. E. Gunn, M. U. SubbaRao, A. R. Thakar, C. Stoughton, A. S. Szalay, B. Yanny, D. G. York, N. A. Bahcall, J. Barentine, M. R. Blanton, H. Brewington, J. Brinkmann, R. J. Brunner, F. J. Castander, I. Csabai, J. A. Frieman, M. Fukugita, M. Harvanek, D. W. Hogg, Z. Ivezic, S. M. Kent, S. J. Kleinman, G. R. Knapp, R. G. Kron, J. Krzesinski, D. C. Long, R. H. Lupton, A. Nitta, J. R. Pier, D. H. Saxe, Y. Shen, S. A. Snedden, D. H. Weinberg, J. Wu, ApJ, 134, 102-117, (2007).
  19. Jump up ↑ Planck 2013 results. XIII. Galactic CO emission, Planck Collaboration, 2014, A&A, 571, A13.

Flexible Image Transfer Specification

Full-Width-at-Half-Maximum

Cosmic Microwave background

Sunyaev-Zel'dovich

Planck Legacy Archive

(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).

(Planck) Low Frequency Instrument

(Planck) High Frequency Instrument

reduced IMO

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