Difference between revisions of "Foreground maps"

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= Astrophysical Components=
+
= 2018 Astrophysical Components=
  
 
== Overview ==
 
== Overview ==
Line 52: Line 52:
 
=====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
Line 69: Line 69:
 
|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)   
 
|}
 
|}
  
Line 134: Line 136:
 
|}
 
|}
  
−
====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:
Line 172: Line 174:
 
|}
 
|}
  
−
== 2018 Lensing maps ==
+
= Previous Releases: (2015) and (2013) Foreground Maps =
  
−
We distribute several variations of lensing potential estimates presented in {{PlanckPapers|planck2016-l08}} as part of the 2018 data release, together with matching simulation packages.
+
<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #FFDAB9;width:80%">
 +
'''Astrophysical components based on the 2015 data release'''
 +
<div class="mw-collapsible-content">
  
−
There are 4 lensing data packages:
+
== Overview ==
 +
This section describes the maps of astrophysical components produced from the Planck data.  These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of each product and how it is obtained, followed by a description of the FITS file containing the data and associated information.
 +
All the details can be found in {{PlanckPapers|planck2014-a12}} and {PlanckPapers|planck20}}.
  
−
* COM_Lensing_4096_R3.00             
+
== Astrophysical foregrounds from parametric component separation ==
−
: Baseline lensing potential estimates from SMICA DX12 CMB maps. Provided are temperature-only (TT), polarization-only (PP) and minimum-variance (MV) estimates.
+
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}}.
−
* COM_Lensing_Sz_4096_R3.00         
 
−
: Variations obtained without galaxy cluster masking.
 
−
* COM_Lensing_Inhf_2048_R3.00       
 
−
: Variations obtained using inhomogeneous noise filtering.
 
−
* COM_Lensing-Szdeproj_4096_R3.00   
 
−
: Variation obtained from thermal Sunyaev-Zeldovich deprojected SMICA CMB map (TT only).
 
  
−
Each map represents an estimate of the CMB lensing potential on approximately 70% of the sky. 
+
'''Low-resolution temperature products'''
−
The lensing estimates from COM_Lensing_4096_R3.00 also forms the basis for the Planck 2018 lensing likelihood.
 
  
−
These data packages have the following common file structure:
+
: 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.
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
+
'''Inputs'''
−
|+ ''' Contents of lensing data package COM_Lensing_4096_R3.00'''
 
−
|-  bgcolor="ffdead" 
 
−
! Filename ||  Format ||  Description
 
−
|-
 
−
| mask.fits.gz || HEALPix FITS format map, with <math>N_{\rm  side}=2048</math> || Lens reconstruction analysis mask.
 
−
|-
 
−
| TT/dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (from temperature only, after mean-field subtraction).
 
−
|-
 
−
| TT/mf_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence mean-field <math> \langle \hat{\kappa}_{LM} \rangle_{\rm{MC}} </math> subtracted from the raw temperature-only data estimate.
 
−
|-
 
−
| PP/dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (from polarization only, after mean-field subtraction).
 
−
|-
 
−
| PP/mf_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence mean-field <math> \langle \hat{\kappa}_{LM} \rangle_{\rm{MC}} </math> subtracted from the raw polarization-only data estimate.
 
−
|-
 
−
| MV/dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (minimum-variance estimate from temperature and polarization, after mean-field subtraction).
 
−
|-
 
−
| MV/mf_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence mean-field <math> \langle \hat{\kappa}_{LM} \rangle_{\rm{MC}} </math> subtracted from the raw minimum variance data estimate.
 
−
|-
 
−
| TT/nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>N_L </math>, <math>C_L+N_L</math>) || Temperature-only reconstruction 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|planck2016-l08}}.
 
−
|-
 
−
| PP/nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>N_L </math>, <math>C_L+N_L</math>) || Polarization-only reconstruction 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|planck2016-l08}}..
 
−
|-
 
−
| MV/nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>N_L </math>, <math>C_L+N_L</math>) || Minimum-variance reconstruction 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|planck2016-l08}}.
 
−
|}
 
  
−
with slight variations:
+
The following data products are used for the low-resolution analysis:
−
 
+
* Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}
−
: - in COM_Lensing_Inhf_2048_R3.00, all HEALPix FITS format alm files have <math>L_{\rm  max}=2048</math>.
+
* Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}
−
: - COM_Lensing-Szdeproj_4096_R3.00 only provides the temperature-only reconstruction.
+
* Full-mission 70 GHz ds1 (18+23), ds2 (19+22), and ds3 (20+21) detector-set maps
 +
* Full-mission 100 GHz ds1 and ds2 detector set maps
 +
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
 +
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps
 +
* Full-mission 353 GHz detector set ds2 and detector 1 maps
 +
* Full-mission 545 GHz detector 2 and 4 maps
 +
* Full-mission 857 GHz detector 2 map
 +
* Beam-symmetrized 9-year WMAP K-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Beam-symmetrized 9-year WMAP Ka-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Default 9-year WMAP Q1 and Q2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Default 9-year WMAP V1 and V2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Default 9-year WMAP W1, W2, W3, and W4 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 +
* Re-processed 408 MHz survey map, Remazeilles et al. (2014) [http://lambda.gsfc.nasa.gov/product/foreground/2014_haslam_408_info.cfm (Lambda)]
 +
All maps are smoothed to a common resolution of 1 degree FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256.
  
−
The matching 4 lensing simulation packages are
+
'''Outputs'''
  
−
* COM_Lensing-SimMap_4096_R3.00             
+
===Synchrotron emission===
−
* COM_Lensing-SimMap_Sz_4096_R3.00         
 
−
* COM_Lensing-SimMap_Inhf_2048_R3.00       
 
−
* COM_Lensing-SimMap-Szdeproj_4096_R3.00   
 
  
−
with the following content:
+
<!--<center>
 +
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px>
 +
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''
 +
</gallery>
 +
</center>-->
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}
−
|+ ''' Contents of lensing simulation package COM_Lensing-SimMap_4096_R3.00'''
+
: Reference frequency: 408 MHz
−
|- bgcolor="ffdead" 
+
: Nside = 256
−
! Filenames ||  Format ||  Description
+
: Angular resolution = 60 arcmin
−
|-
+
 
−
| /inputs/mask.fits.gz || compressed HEALPix FITS format map, with <math>N_{\rm  side}=2048</math> || Lens reconstruction analysis mask.
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|-
+
|+ HDU -- COMP-MAP-Synchrotron
−
| /inputs/FFP10_wdipole_lenspotentialCls.dat || ASCII text file, with columns = (<math>L</math>, <math>C_L^{TT} </math>, <math>C_L^{EE} </math>,<math>C_L^{BB} </math>,<math>C_L^{TE} </math>,<math>C_L^{\phi\phi} </math>,<math>C_L^{T\phi} </math>,<math>C_L^{E\phi} </math>) || Input unlensed CMB spectra of the fiducial cosmology used in {{PlanckPapers|planck2016-l08}}.
 
 
|-
 
|-
−
| TT/sim_klm_{???}.fits  || 300 HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (from temperature only, no mean-field subtraction) of all 300 FFP10 simulations used in  {{PlanckPapers|planck2016-l08}}.
+
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
| PP/sim_klm_{???}.fits  || 300 HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (from polarization only, no mean-field subtraction) of all 300 FFP10 simulations used in  {{PlanckPapers|planck2016-l08}}.
+
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum   
 
|-
 
|-
−
| MV/sim_klm_{???}.fits  || 300 HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (minimum-variance estimate from temperature and polarization, no mean-field subtraction) of all 300 FFP10 simulations used in  {{PlanckPapers|planck2016-l08}}.
+
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean  
 
|-
 
|-
−
| TT/dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (from temperature only, no mean-field subtraction).
+
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms
−
|-
 
−
| PP/dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (from polarization only, no mean-field subtraction).
 
−
|-
 
−
| MV/dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> (minimum-variance estimate from temperature and polarization, no mean-field subtraction).
 
−
|-
 
−
| TT/nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>\textrm{RD-}N_L^{0} </math>, <math>\textrm{MC-}N_L^{0}</math>, <math>N_L^{1}</math>, <math>{PS}_L</math>,  <math>\langle \hat C^{\kappa\kappa}_L  - C_L^{\kappa\kappa, \rm fid}\rangle_{\rm MC}</math>, <math>1/\mathcal R^\kappa_L</math>) || Temperature-only reconstruction lensing spectrum biases and quadratic estimator normalization (inverse response), as defined in {{PlanckPapers|planck2016-l08}}.
 
−
|-
 
−
| PP/nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>\textrm{RD-}N_L^{0} </math>, <math>\textrm{MC-}N_L^{0}</math>, <math>N_L^{1}</math>, <math>{PS}_L</math>,  <math>\langle \hat C^{\kappa\kappa}_L  - C_L^{\kappa\kappa, \rm fid}\rangle_{\rm MC}</math>, <math>1/\mathcal R^\kappa_L</math>) || Polarization-only reconstruction lensing spectrum biases and quadratic estimator normalization (inverse response), as defined in {{PlanckPapers|planck2016-l08}}.
 
−
|-
 
−
| MV/nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>\textrm{RD-}N_L^{0} </math>, <math>\textrm{MC-}N_L^{0}</math>, <math>N_L^{1}</math>, <math>{PS}_L</math>,  <math>\langle \hat C^{\kappa\kappa}_L  - C_L^{\kappa\kappa, \rm fid}\rangle_{\rm MC}</math>, <math>1/\mathcal R^\kappa_L</math>) || Minimum variance reconstruction lensing spectrum biases and quadratic estimator normalization (inverse response), as defined in {{PlanckPapers|planck2016-l08}}.
 
 
|}
 
|}
  
−
with the same slight variations:
 
  
−
: - in COM_Lensing-SimMap_Inhf_2048_R3.00, all HEALPix FITS format alm files have <math>L_{\rm  max}=2048</math>.
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
: - COM_Lensing-SimMap-Szdeproj_4096_R3.00 only provides the temperature-only reconstructions.
+
|+ Extension 1 -- SYNC-TEMP
−
 
+
|-
−
We further provide the input lensing convergence realizations of all 300 FFP10 simulations in
+
|- bgcolor="ffdead"  
−
 
+
! Column Name || Data Type || Units || Description
−
* COM_Lensing-SimMap-inputs_4096_R3.00
 
−
 
 
−
with contents
 
−
 
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of lensing simulation package COM_Lensing-SimMap-inputs_4096_R3.00'''
 
−
|- bgcolor="ffdead"
 
−
! Filenames || Format || Description
 
 
|-
 
|-
−
| /inputs/clkk.dat || ASCII text file, with columns = (<math>L</math>, <math>C_L^{\kappa\kappa}</math>) || Input lensing convergence CMB spectrum of the fiducial cosmology used in {{PlanckPapers|planck2016-l08}}.
+
|nu  || Real*4 || Hz || Frequency   
 
|-
 
|-
−
| sky_klm_{???}.fits  || 300 HEALPix FITS format alm, with <math>L_{\rm  max}=4096</math> || Input lensing convergence <math> {\kappa}_{LM} = \frac{1}{2} L(L+1){\phi}_{LM} </math> realizations of all 300 FFP10 simulations used in  {{PlanckPapers|planck2016-l08}}.
+
|intensity || Real*4 || W/Hz/m2/sr || GALPROP z10LMPD_SUNfE spectrum   
 
|}
 
|}
  
−
== 2018 Lensing-induced <i>B</i>-mode maps ==
 
  
−
We distribute maps of the lensing-induced <i>B</i>-modes presented in {{PlanckPapers|planck2016-l08}}, together with a matching simulation suite. The Stokes parameter maps of the lensing <i>B</i>-modes are produced by combining tracers of lensing potential with <i>E</i>-mode data from the SMICA CMB polarization maps. These lensing-induced <i>B</i>-mode polarization maps are provided on approximately 60% of the sky. {{PlanckPapers|planck2016-l08}} details the construction of these maps.
+
===Free-free emission===
  
−
These maps come in two variations. In the first we use the <math>TT + TE + EE</math> quadratic estimator built from the DX12 SMICA CMB maps (we discard <math>TB</math> and <math>EB</math> in order to use lensing tracers that are statistically independent of the <math>B</math>-mode map). In the second we further add CIB information at 545 GHz (GNILC) to the lensing tracer.
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}}
−
 
+
: Reference frequency: NA
−
These maps are filtered template of the lensing <i>B</i>-mode (both the lensing tracer and <math>E</math>-mode used to build the <i>B</i> template are Wiener-filtered). The simulation suite may be used to assess the filter, as was done in {{PlanckPapers|planck2016-l08}} to produce the <i>B</i>-mode power spectrum (Fig. 14).
+
: Nside = 256
 +
: Angular resolution = 60 arcmin
  
−
The B-mode template package is
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
 
+
|+ HDU -- COMP-MAP-freefree
−
* COM_Lensing-Bmode_2048_R3.00
 
−
 
 
−
with contents
 
−
 
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of B-mode template data package COM_Lensing-Bmode_2048_R3.00'''
 
−
|- bgcolor="ffdead" 
 
−
! Filenames ||  Format ||  Description
 
 
|-
 
|-
−
| /inputs/mask.fits.gz || compressed HEALPix FITS format map, with <math>N_{\rm  side}=2048</math>  || <math>B</math>-mode analysis mask used in {{PlanckPapers|planck2016-l08}}.
+
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
| /inputs/clbb.dat || ASCII text file, with columns = (<math>L</math>, <math>C_L^{BB}</math>) || Input lensing <math>B</math>-mode power spectrum for the fiducial cosmology used in {{PlanckPapers|planck2016-l08}}.
+
|EM_ML || Real*4 || cm^-6 pc || Emission measure posterior maximum   
 
|-
 
|-
−
|dat_blm_TTTEETEE.fits  || HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Lensing <math>B</math>-mode template built from the <math>\hat \phi^{TT + TE + EE}</math> lensing tracer and <math>E</math>-mode map.
+
|EM_MEAN || Real*4 || cm^-6 pc || Emission measure posterior mean
 
|-
 
|-
−
|dat_blm_545_TTTEETEE.fits  || HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Lensing <math>B</math>-mode template built from the <math>\hat \phi^{TT + TE + EE} + \rm{CIB}</math> lensing tracer and <math>E</math>-mode map.
+
|EM_RMS || Real*4 || cm^-6 pc || Emission measure posterior rms
−
|}
 
−
 
 
−
The B-mode template simulation package is
 
−
 
 
−
* COM_Lensing-SimMap-Bmode_2048_R3.00
 
−
 
 
−
with contents
 
−
 
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of B-mode template simulation package COM_Lensing-SimMap-Bmode_2048_R3.00'''
 
−
|-  bgcolor="ffdead" 
 
−
! Filenames ||  Format || Description
 
 
|-
 
|-
−
| /inputs/mask.fits.gz || compressed HEALPix FITS format map, with <math>N_{\rm  side}=2048</math>  || <math>B</math>-mode analysis mask used in {{PlanckPapers|planck2016-l08}}.
+
|TEMP_ML || Real*4 || K || Electron temperature posterior maximum   
 
|-
 
|-
−
| /inputs/clbb.dat || ASCII text file, with columns = (<math>L</math>, <math>C_L^{BB}</math>) || Input lensing <math>B</math>-mode power spectrum for the fiducial cosmology used in {{PlanckPapers|planck2016-l08}}.
+
|TEMP_MEAN || Real*4 || K || Electron temperature posterior mean
 
|-
 
|-
−
|/TTTEETE/blm_{???}.fits  || 300 HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> ||Lensing <math>B</math>-mode template built from the <math>\hat \phi^{TT + TE + EE}</math> lensing tracer and <math>E</math>-mode map of all 300 FFP10 simulations used in  {{PlanckPapers|planck2016-l08}}.
+
|TEMP_RMS || Real*4 || K || Electron temperature posterior rms
−
|-
 
−
|/545_TTTEETE/blm_{???}.fits  || 300 HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> ||Lensing <math>B</math>-mode template built from the <math>\hat \phi^{TT + TE + EE} + \rm{CIB}</math>  lensing tracer and <math>E</math>-mode map of all 300 FFP10 simulations used in  {{PlanckPapers|planck2016-l08}}.
 
−
|-
 
−
|/TTTEETE/dat_blm.fits  ||  HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Lensing <math>B</math>-mode template built from the <math>\hat \phi^{TT + TE + EE}</math> lensing tracer and <math>E</math>-mode map.
 
−
|-
 
−
|/545_TTTEETE/dat_blm.fits  ||  HEALPix FITS format alm, with <math>L_{\rm  max}=2048</math> || Lensing <math>B</math>-mode template built from the <math>\hat \phi^{TT + TE + EE} + \rm{CIB}</math> lensing tracer and <math>E</math>-mode map.
 
 
|}
 
|}
  
−
== 2018 Lensing combined tracers maps ==
 
  
−
We distribute estimates of the CMB lensing convergence maps built combining the Planck 2018 quadratic estimators and CIB data at 545 GHz (GNILC), together with a matching simulation suite. The construction of these maps is decribed in details in {{PlanckPapers|planck2016-l08}}. The maps are built on about 60% of the sky.
+
===Spinning dust emission===
  
−
These maps come in two variations. In the first we use the minimum-variance (MV) quadratic estimator together with the CIB. In the second we use the <math>TT + TE + EE</math> quadratic estimator  together with the CIB, and is statistically independent from the CMB B-polarization.
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}}
−
 
+
: Nside = 256
−
The lensing combined tracer data package is
+
: Angular resolution = 60 arcmin
  
−
* COM_Lensing-CIBcomb_2000_R3.00
+
Note: The spinning dust component has two independent constituents, each corresponding to one spdust2 component, but with different peak frequencies. The two components are stored in the two first FITS extensions, and the template frequency spectrum is stored in the third extension. 
  
−
with contents
+
: Reference frequency: 22.8 GHz
−
 
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
+
|+ HDU -- COMP-MAP-AME1
−
|+ ''' Contents of lensing combined tracer data package COM_Lensing-CIBcomb_2000_R3.00'''
 
−
|- bgcolor="ffdead" 
 
−
! Filenames ||  Format ||  Description
 
 
|-
 
|-
−
| /inputs/mask.fits.gz || compressed HEALPix FITS format map, with <math>N_{\rm  side}=2048</math>  || Tracer combination analysis mask used in {{PlanckPapers|planck2016-l08}}.
+
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|dat_klm_545_MV.fits  || HEALPix FITS format alm, with <math>L_{\rm  max}=2000</math> || Lensing tracer built from the minimum-variance quadratic estimator and the CIB (GNILC 545 GHz map).
+
|I_ML || Real*4 || uK_RJ || Primary amplitude posterior maximum   
 
|-
 
|-
−
|dat_klm_545_TTTEETEE.fits  || HEALPix FITS format alm, with <math>L_{\rm  max}=2000</math> || Lensing tracer built from the <math>TT + TE + EE</math> quadratic estimator and the CIB (GNILC 545 GHz map).
+
|I_MEAN || Real*4 || uK_RJ || Primary amplitude posterior mean
−
|}
 
−
 
 
−
The lensing combined tracer simulation package is
 
−
 
 
−
* COM_Lensing-SimMap-CIBcomb_2000_R3.00
 
−
 
 
−
with contents
 
−
 
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
−
|+ ''' Contents of lensing combined tracer simulation package COM_Lensing-SimMap-CIBcomb_2000_R3.00'''
 
−
|-  bgcolor="ffdead" 
 
−
! Filenames || Format || Description
 
 
|-
 
|-
−
| /inputs/mask.fits.gz || compressed HEALPix FITS format map, with <math>N_{\rm  side}=2048</math>  || Tracer combination analysis mask used in {{PlanckPapers|planck2016-l08}}.
+
|I_RMS || Real*4 || uK_RJ || Primary amplitude posterior rms
 
|-
 
|-
−
| 545_MV/sim_klm_{???}.fits || 300 HEALPix FITS format alm, with <math>L_{\rm  max}=2000</math> ||Lensing tracer built from the minimum-variance quadratic estimator and the CIB (GNILC 545 GHz map) of all 300 FFP10 simulations used in {{PlanckPapers|planck2016-l08}}.
+
|FREQ_ML || Real*4 || GHz || Primary peak frequency posterior maximum   
 
|-
 
|-
−
| 545_TTTEETEE/sim_klm_{???}.fits || 300 HEALPix FITS format alm, with <math>L_{\rm  max}=2000</math> ||Lensing tracer built from the <math>TT + TE + EE</math> quadratic estimator and the CIB (GNILC 545 GHz map) of all 300 FFP10 simulations used in {{PlanckPapers|planck2016-l08}}.
+
|FREQ_MEAN || Real*4 || GHz || Primary peak frequency posterior mean
 
|-
 
|-
−
| 545_MV/dat_klm.fits  || HEALPix FITS format alm, with <math>L_{\rm  max}=2000</math> || Lensing tracer built from the minimum-variance quadratic estimator and the CIB (GNILC 545 GHz map).
+
|FREQ_RMS || Real*4 || GHz || Primary peak frequency posterior rms
−
|-
 
−
| 545_TTTEETEE/dat_klm.fits  ||  HEALPix FITS format alm, with <math>L_{\rm  max}=2000</math> || Lensing tracer built from the <math>TT + TE + EE</math> quadratic estimator and the CIB (GNILC 545 GHz map).
 
 
|}
 
|}
  
−
Also part of this package are high-resolution figures of the lensing deflection (similar to Fig. 3 and Fig. 13 of  {{PlanckPapers|planck2016-l08}}).
+
: Reference frequency: 41.0 GHz
−
The figures show the Wiener-filtered, gradient <math>(E)</math> mode of the displacement <math>\hat \alpha_{LM} = \sqrt{L (L + 1)} \hat \phi_{LM}</math>.
+
: Peak frequency: 33.35 GHz
−
 
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
Mollveide projection of the minimum variance quadratic estimator lensing map:
+
|+ Extension 1 -- COMP-MAP-AME2
−
* Lensing_2018_MV_alphaA0_YlGnBu_300dpi_47in_moll.png         
+
|-
−
Orthographic projection of the minimum variance quadratic estimatorlensing map:
+
|- bgcolor="ffdead" 
−
* Lensing_2018_compMV_alphaA0_YlGnBu_300dpi_47in_moll.png    
+
! Column Name || Data Type || Units || Description
−
Orthographic projection of the minimum variance quadratic estimator combined with the CIB (GNILC 545 GHz map) lensing tracer map:
+
|-
−
* Lensing_2018_compMV545_alphaA0_YlGnBu_300dpi_47in_orth.png
+
|I_ML || Real*4 || uK_RJ || Secondary amplitude posterior maximum    
−
 
+
|-
−
= Previous Releases: (2015) and (2013) Foreground Maps =
+
|I_MEAN || Real*4 || uK_RJ || Secondary amplitude posterior mean
 +
|-
 +
|I_RMS || Real*4 || uK_RJ || Secondary amplitude posterior rms
 +
|}
  
−
<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #FFDAB9;width:80%">
 
−
'''Astrophysical components based on the 2015 data release'''
 
−
<div class="mw-collapsible-content">
 
  
−
''' Overview '''
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
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.
+
|+ Extension 2 -- SPINNING-DUST-TEMP
−
All the details can be found in {{PlanckPapers|planck2014-a12}} and {PlanckPapers|planck20}}.
+
|-
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|nu  || Real*4 || GHz || Frequency   
 +
|-
 +
|j_nu/nH || Real*4 || Jy sr-1 cm2/H || spdust2 spectrum   
 +
|}
  
−
''' Astrophysical foregrounds from parametric component separation '''
+
===CO line emission===
−
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}}.
 
  
−
'''Low-resolution temperature products'''
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}}
 +
: Nside = 256
 +
: Angular resolution = 60 arcmin
  
−
: 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.  
+
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.
  
−
'''Inputs'''
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-co10
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 +
|-
 +
|I_ML || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior maximum   
 +
|-
 +
|I_MEAN || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior mean
 +
|-
 +
|I_RMS || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior rms
 +
|}
  
−
The following data products are used for the low-resolution analysis:
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
* Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}
+
|+ Extension 1 -- COMP-MAP-co21
−
* Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}
+
|-
−
* Full-mission 70 GHz ds1 (18+23), ds2 (19+22), and ds3 (20+21) detector-set maps
+
|- bgcolor="ffdead" 
−
* Full-mission 100 GHz ds1 and ds2 detector set maps
+
! Column Name || Data Type || Units || Description
−
* 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
+
|I_ML || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior maximum   
−
* Full-mission 353 GHz detector set ds2 and detector 1 maps
+
|-
−
* Full-mission 545 GHz detector 2 and 4 maps
+
|I_MEAN || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior mean
−
* Full-mission 857 GHz detector 2 map
+
|-
−
* Beam-symmetrized 9-year WMAP K-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
+
|I_RMS || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior rms
−
* Beam-symmetrized 9-year WMAP Ka-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
+
|}
−
* Default 9-year WMAP Q1 and Q2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 
−
* Default 9-year WMAP V1 and V2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 
−
* Default 9-year WMAP W1, W2, W3, and W4 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
 
−
* Re-processed 408 MHz survey map, Remazeilles et al. (2014) [http://lambda.gsfc.nasa.gov/product/foreground/2014_haslam_408_info.cfm (Lambda)]
 
−
All maps are smoothed to a common resolution of 1 degree FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256.
 
  
−
'''Outputs'''
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
 
+
|+ Extension 2 -- COMP-MAP-co32
−
'''Synchrotron emission'''
+
|-
−
 
+
|- bgcolor="ffdead" 
−
<!--<center>
+
! Column Name || Data Type || Units || Description
−
<gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px>
+
|-
−
File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''
+
|I_ML || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior maximum   
−
</gallery>
+
|-
−
</center>-->
+
|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: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-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}}
−
: Reference frequency: 408 MHz
 
 
: Nside = 256
 
: Nside = 256
 
: Angular resolution = 60 arcmin
 
: Angular resolution = 60 arcmin
  
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ HDU -- COMP-MAP-Synchrotron
+
|+ HDU -- COMP-MAP-xline
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum     
+
|I_ML || Real*4 || uK_cmb || Amplitude posterior maximum     
 
|-
 
|-
−
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean  
+
|I_MEAN || Real*4 || uK_cmb || Amplitude posterior mean  
 
|-
 
|-
−
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms
+
|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.
  
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
+
===Thermal dust emission===
−
|+ Extension 1 -- SYNC-TEMP
+
 
−
|-
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}}
−
|- bgcolor="ffdead" 
 
−
! 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: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}}
 
−
: Reference frequency: NA
 
 
: Nside = 256
 
: Nside = 256
 
: Angular resolution = 60 arcmin
 
: Angular resolution = 60 arcmin
  
 +
: Reference frequency: 545 GHz
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ HDU -- COMP-MAP-freefree
+
|+ HDU -- COMP-MAP-dust
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|EM_ML || Real*4 || cm^-6 pc || Emission measure posterior maximum     
+
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum     
 +
|-
 +
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean
 
|-
 
|-
−
|EM_MEAN || Real*4 || cm^-6 pc || Emission measure posterior mean
+
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms
 
|-
 
|-
−
|EM_RMS || Real*4 || cm^-6 pc || Emission measure posterior rms
+
|TEMP_ML || Real*4 || K || Dust temperature posterior maximum   
 
|-
 
|-
−
|TEMP_ML || Real*4 || K || Electron temperature posterior maximum   
+
|TEMP_MEAN || Real*4 || K || Dust temperature posterior mean
 
|-
 
|-
−
|TEMP_MEAN || Real*4 || K || Electron temperature posterior mean
+
|TEMP_RMS || Real*4 || K || Dust temperature posterior rms
 
|-
 
|-
−
|TEMP_RMS || Real*4 || K || Electron 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===
  
−
'''Spinning dust emission'''
+
: 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_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}}
 
 
: Nside = 256
 
: Nside = 256
 
: Angular resolution = 60 arcmin
 
: Angular resolution = 60 arcmin
  
−
Note: The spinning dust component has two independent constituents, each corresponding to one spdust2 component, but with different peak frequencies. The two components are stored in the two first FITS extensions, and the template frequency spectrum is stored in the third extension. 
 
−
 
−
: Reference frequency: 22.8 GHz
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ HDU -- COMP-MAP-AME1
+
|+ HDU -- COMP-MAP-SZ
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I_ML || Real*4 || uK_RJ || Primary amplitude posterior maximum     
+
|Y_ML || Real*4 || y_SZ || Y parameter posterior maximum     
 
|-
 
|-
−
|I_MEAN || Real*4 || uK_RJ || Primary amplitude posterior mean  
+
|Y_MEAN || Real*4 || y_SZ || Y parameter posterior mean  
 
|-
 
|-
−
|I_RMS || Real*4 || uK_RJ || Primary amplitude posterior rms
+
|Y_RMS || Real*4 || y_SZ || Y parameter 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
+
'''High-resolution temperature products'''
−
: Peak frequency: 33.35 GHz
+
 
 +
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz.
 +
 
 +
'''Inputs'''
 +
 
 +
The following data products are used for the low-resolution analysis:
 +
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
 +
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps
 +
* Full-mission 353 GHz detector set ds2 and detector 1 maps
 +
* Full-mission 545 GHz detector 2 and 4 maps
 +
* Full-mission 857 GHz detector 2 map
 +
All maps are smoothed to a common resolution of 7.5 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=2048.
 +
 
 +
'''Outputs'''
 +
 
 +
'''CO J2->1 emission'''
 +
 
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO21-commander_2048_R2.00.fits|link=COM_CompMap_CO21-commander_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 7.5 arcmin
 +
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ Extension 1 -- COMP-MAP-AME2
+
|+ HDU -- COMP-MAP-CO21
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I_ML || Real*4 || uK_RJ || Secondary amplitude posterior maximum     
+
|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_MEAN || Real*4 || uK_RJ || Secondary amplitude posterior mean
+
|I_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission amplitude posterior maximum   
 
|-
 
|-
−
|I_RMS || Real*4 || uK_RJ || Secondary amplitude posterior rms
+
|I_ML_HR1 || Real*4 || K_RJ km/s || First half-ring amplitude posterior maximum   
−
|}
 
−
 
 
−
 
 
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
−
|+ Extension 2 -- SPINNING-DUST-TEMP
 
 
|-
 
|-
−
|- bgcolor="ffdead" 
+
|I_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring amplitude posterior maximum   
−
! Column Name || Data Type || Units || Description
 
 
|-
 
|-
−
|nu  || Real*4 || GHz || Frequency    
+
|I_ML_YR1 || Real*4 || K_RJ km/s || "First year" amplitude posterior maximum    
 
|-
 
|-
−
|j_nu/nH || Real*4 || Jy sr-1 cm2/H || spdust2 spectrum    
+
|I_ML_YR2 || Real*4 || K_RJ km/s || "Second year" amplitude posterior maximum    
 
|}
 
|}
  
−
'''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}}
+
'''Thermal dust emission'''
−
: 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.
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_ThermalDust-commander_2048_R2.00.fits|link=COM_CompMap_ThermalDust-commander_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 7.5 arcmin
  
 +
: Reference frequency: 545 GHz
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ HDU -- COMP-MAP-co10
+
|+ HDU -- COMP-MAP-dust
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I_ML || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior maximum     
+
|I_ML_FULL || Real*4 || uK_RJ || Full-mission amplitude posterior maximum     
 
|-
 
|-
−
|I_MEAN || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior mean
+
|I_ML_HM1 || Real*4 || uK_RJ || First half-mission amplitude posterior maximum   
 
|-
 
|-
−
|I_RMS || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior rms
+
|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   
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
−
|+ Extension 1 -- COMP-MAP-co21
 
 
|-
 
|-
−
|- bgcolor="ffdead" 
+
|I_ML_HR2 || Real*4 || uK_RJ || Second half-ring amplitude posterior maximum   
−
! Column Name || Data Type || Units || Description
 
 
|-
 
|-
−
|I_ML || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior maximum     
+
|I_ML_YR1 || Real*4 || uK_RJ || "First year" amplitude posterior maximum     
 
|-
 
|-
−
|I_MEAN || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior mean
+
|I_ML_YR2 || Real*4 || uK_RJ || "Second year" amplitude posterior maximum   
 
|-
 
|-
−
|I_RMS || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior rms
+
|BETA_ML_FULL || Real*4 || NA || Full-mission emissivity index posterior maximum   
−
|}
 
−
 
 
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
−
|+ Extension 2 -- COMP-MAP-co32
 
 
|-
 
|-
−
|- bgcolor="ffdead" 
+
|BETA_ML_HM1 || Real*4 || NA || First half-mission emissivity index posterior maximum   
−
! Column Name || Data Type || Units || Description
 
 
|-
 
|-
−
|I_ML || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior maximum     
+
|BETA_ML_HM2 || Real*4 || NA || Second half-mission emissivity index posterior maximum     
 
|-
 
|-
−
|I_MEAN || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior mean
+
|BETA_ML_HR1 || Real*4 || NA || First half-ring emissivity index posterior maximum   
 
|-
 
|-
−
|I_RMS || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior rms
+
|BETA_ML_HR2 || Real*4 || NA || Second half-ring emissivity index posterior maximum   
−
|}
 
−
 
 
−
'''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}}
 
−
: Nside = 256
 
−
: Angular resolution = 60 arcmin
 
−
 
 
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
−
|+ HDU -- COMP-MAP-xline
 
 
|-
 
|-
−
|- bgcolor="ffdead" 
+
|BETA_ML_YR1 || Real*4 || NA || "First year" emissivity index posterior maximum   
−
! Column Name || Data Type || Units || Description
 
 
|-
 
|-
−
|I_ML || Real*4 || uK_cmb || Amplitude posterior maximum     
+
|BETA_ML_YR2 || Real*4 || NA || "Second year" emissivity index 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.
+
'''Polarization products'''
  
−
'''Thermal dust emission'''
+
Two polarization foreground products are provided, namely synchrotron and thermal dust emission. The spectral models are assumed identical to the corresponding temperature spectral models.
  
−
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}}
+
'''Inputs'''
−
: Nside = 256
 
−
: Angular resolution = 60 arcmin
 
  
−
: Reference frequency: 545 GHz
+
The following data products are used for the polarization analysis:
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
+
* (Only low-resolution analysis) Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}
−
|+ HDU -- COMP-MAP-dust
+
* (Only low-resolution analysis) Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}
 +
* (Only low-resolution analysis) Full-mission 70 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=70|period=Full|link=LFI 70 GHz frequency maps}}
 +
* Full-mission 100 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=100|period=Full|link=HFI 100 GHz frequency maps}}
 +
* Full-mission 143 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=143|period=Full|link=HFI 143 GHz frequency maps}}
 +
* Full-mission 217 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=217|period=Full|link=HFI 217 GHz frequency maps}}
 +
* Full-mission 353 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=353|period=Full|link=HFI 353 GHz frequency maps}}
 +
In the low-resolution analysis, all maps are smoothed to a common resolution of 40 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256. In the high-resolution analysis (including only CMB and thermal dust emission), the corresponding resolution is 10 arcmin FWHM and Nside=1024.
 +
 
 +
'''Outputs'''
 +
'''Synchrotron emission'''
 +
 
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits|link=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits}}
 +
: Nside = 256
 +
: Angular resolution = 40 arcmin
 +
 
 +
: Reference frequency: 30 GHz
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-SynchrotronPol
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I_ML || Real*4 || uK_RJ || Amplitude posterior maximum     
+
|Q_ML_FULL || Real*4 || K_RJ km/s || Full-mission Stokes Q posterior maximum     
 
|-
 
|-
−
|I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean
+
|U_ML_FULL || Real*4 || K_RJ km/s || Full-mission Stokes U posterior maximum   
 
|-
 
|-
−
|I_RMS || Real*4 || uK_RJ || Amplitude posterior rms
+
|Q_ML_HM1 || Real*4 || K_RJ km/s || First half-mission Stokes Q posterior maximum   
 
|-
 
|-
−
|TEMP_ML || Real*4 || K || Dust temperature posterior maximum     
+
|U_ML_HM1 || Real*4 || K_RJ km/s || First half-mission Stokes U posterior maximum     
 
|-
 
|-
−
|TEMP_MEAN || Real*4 || K || Dust temperature posterior mean
+
|Q_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission Stokes Q posterior maximum   
 
|-
 
|-
−
|TEMP_RMS || Real*4 || K || Dust temperature posterior rms
+
|U_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission Stokes U posterior maximum   
 +
|-
 +
|Q_ML_HR1 || Real*4 || K_RJ km/s || First half-ring Stokes Q posterior maximum   
 +
|-
 +
|U_ML_HR1 || Real*4 || K_RJ km/s || First half-ring Stokes U posterior maximum   
 +
|-
 +
|Q_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring Stokes Q posterior maximum   
 +
|-
 +
|U_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring Stokes U posterior maximum   
 +
|-
 +
|Q_ML_YR1 || Real*4 || K_RJ km/s || "First year" Stokes Q posterior maximum   
 
|-
 
|-
−
|BETA_ML || Real*4 || NA || Emissivity index posterior maximum     
+
|U_ML_YR1 || Real*4 || K_RJ km/s || "First year" Stokes U posterior maximum     
 
|-
 
|-
−
|BETA_MEAN || Real*4 || NA || Emissivity index posterior mean
+
|Q_ML_YR2 || Real*4 || K_RJ km/s || "Second year" Stokes Q posterior maximum
 
|-
 
|-
−
|BETA_RMS || Real*4 || NA || Emissivity index posterior rms
+
|U_ML_YR2 || Real*4 || K_RJ km/s || "Second year" Stokes U posterior maximum     
 
|}
 
|}
  
−
'''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}}
+
'''Thermal dust emission'''
−
: Nside = 256
+
 
−
: Angular resolution = 60 arcmin
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_DustPol-commander_1024_R2.00.fits|link=COM_CompMap_DustPol-commander_1024_R2.00.fits}}
 +
: Nside = 1024
 +
: Angular resolution = 10 arcmin
  
 +
: Reference frequency: 353 GHz
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ HDU -- COMP-MAP-SZ
+
|+ HDU -- COMP-MAP-DustPol
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|Y_ML || Real*4 || y_SZ || Y parameter posterior maximum     
+
|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     
 
|-
 
|-
−
|Y_MEAN || Real*4 || y_SZ || Y parameter posterior mean
+
|Q_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes Q posterior maximum
 
|-
 
|-
−
|Y_RMS || Real*4 || y_SZ || Y parameter posterior rms
+
|U_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes U posterior maximum     
 
|}
 
|}
  
−
'''High-resolution temperature products'''
+
''' Modelling of the thermal dust emission with the Draine and Li dust model '''
  
−
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz.  
+
The Planck, IRAS, and WISE infrared observations were fit with the dust model presented by Draine & Li in 2007 (DL07).
 +
The input maps, the DL07 model, and the fitting procedure and results are presented in {{PlanckPapers|planck2014-XXIX}}.
 +
Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.
  
 
'''Inputs'''
 
'''Inputs'''
  
−
The following data products are used for the low-resolution analysis:
+
The following data have been fit:
−
* Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
 
−
* Full-mission 217 GHz detector 1, 2, 3 and 4 maps
 
−
* Full-mission 353 GHz detector set ds2 and detector 1 maps
 
−
* Full-mission 545 GHz detector 2 and 4 maps
 
−
* Full-mission 857 GHz detector 2 map
 
−
All maps are smoothed to a common resolution of 7.5 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=2048.
 
  
−
'''Outputs'''
+
* 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
  
−
'''CO J2->1 emission'''
+
The CIB monopole, the CMB anisotropries and the zodiacal light were subtracted to obtain dust emission maps from the sky emission maps.
 +
All maps were smoothed to a common angular resolution of 5'.
  
−
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO21-commander_2048_R2.00.fits|link=COM_CompMap_CO21-commander_2048_R2.00.fits}}
+
'''Model Parameters'''
−
: Nside = 2048
 
−
: Angular resolution = 7.5 arcmin
 
  
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
+
For each pixel of the inputs maps, we have fitted four parameters of the DL07 model:
−
|+ HDU -- COMP-MAP-CO21
+
 
 +
* the dust mass surface density, Sigma_Mdust,
 +
* the dust mass fraction in small PAH grains, q_PAH,
 +
* the fraction of the total luminosity from dust heated by intense radiation fields, f_PDR,
 +
* the starlight intensity heating the bulk of the dust, U_min.
 +
 
 +
The parameter maps and their uncertainties are gathered in one file. This file also includes the
 +
chi2 of the fit per degree of freedom.
 +
 
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 5 arcmin
 +
 
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-Dust-DL07-Parameters
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I_ML_FULL || Real*4 || K_RJ km/s || Full-mission amplitude posterior maximum   
+
|Sigma_Mdust || Real*4 || Solar masses/kpc^2 || Dust mass surface density
 
|-
 
|-
−
|I_ML_HM1 || Real*4 || K_RJ km/s || First half-mission amplitude posterior maximum   
+
|Sigma_Mdust_unc || Real*4 || Solar masses/kpc^2 || Uncertainty (1 sigma) on Sigma_Mdust
 
|-
 
|-
−
|I_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission amplitude posterior maximum   
+
|q_PAH || Real*4 || dimensionless || Dust mass fraction in small PAH grains   
 
|-
 
|-
−
|I_ML_HR1 || Real*4 || K_RJ km/s || First half-ring amplitude posterior maximum   
+
|q_PAH_unc || Real*4 || dimensionless || Uncertainty (1 sigma) on q_PAH
 
|-
 
|-
−
|I_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring amplitude posterior maximum   
+
|f_PDR || Real*4 || dimensionless || Fraction of the total luminosity from dust heated by intense radiation fields
 
|-
 
|-
−
|I_ML_YR1 || Real*4 || K_RJ km/s || "First year" amplitude posterior maximum   
+
|f_PDR_unc || Real*4 || dimensionless || Uncertainty (1 sigma) on f_PDR
 
|-
 
|-
−
|I_ML_YR2 || Real*4 || K_RJ km/s || "Second year" amplitude posterior maximum    
+
|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'''
  
−
'''Thermal dust emission'''
+
We provide two exinctions maps at the visible V band: the value from the model (Av_DL) and the 
 +
renormalized one (Av_RQ) that matches extinction estimates for quasars (QSOs) derived from the Sloan digital sky survey (SDSS) data.
  
−
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_ThermalDust-commander_2048_R2.00.fits|link=COM_CompMap_ThermalDust-commander_2048_R2.00.fits}}
+
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits}}
 
: Nside = 2048
 
: Nside = 2048
−
: Angular resolution = 7.5 arcmin
+
: Angular resolution = 5 arcmin
  
−
: Reference frequency: 545 GHz
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ HDU -- COMP-MAP-dust
+
|+ HDU -- COMP-MAP-Dust-DL07-AvMaps
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Column Name || Data Type || Units || Description
 
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I_ML_FULL || Real*4 || uK_RJ || Full-mission amplitude posterior maximum   
+
|Av_DL || Real*4 || magnitude || Extinction in the V band from the DL model
 
|-
 
|-
−
|I_ML_HM1 || Real*4 || uK_RJ || First half-mission amplitude posterior maximum   
+
|Av_DL_unc || Real*4 || magnitude || Uncertainty (1 sigma) on Av_DL
 
|-
 
|-
−
|I_ML_HM2 || Real*4 || uK_RJ || Second half-mission amplitude posterior maximum   
+
|Av_RQ || Real*4 || magnitude || Extinction in the V band renormalized to match estimates from QSO SDSS observations 
 
|-
 
|-
−
|I_ML_HR1 || Real*4 || uK_RJ || First half-ring amplitude posterior maximum   
+
|Av_RQ_unc || Real*4 || magnitude || Uncertainty (1 sigma) on Av_RQ
−
|-
+
|}
−
|I_ML_HR2 || Real*4 || uK_RJ || Second half-ring amplitude posterior maximum   
+
 
 +
'''Model Fluxes'''
 +
 
 +
We provide the model predicted fluxes in the following file.
 +
 
 +
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits}}
 +
: Nside = 2048
 +
: Angular resolution = 5 arcmin
 +
 
 +
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|+ HDU -- COMP-MAP-Dust-DL07-ModelFluxes
 
|-
 
|-
−
|I_ML_YR1 || Real*4 || uK_RJ || "First year" amplitude posterior maximum   
+
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
|I_ML_YR2 || Real*4 || uK_RJ || "Second year" amplitude posterior maximum   
+
|Planck_857 || Real*4 || MJy/sr || Model flux in the Planck 857 GHz band
 
|-
 
|-
−
|BETA_ML_FULL || Real*4 || NA || Full-mission emissivity index posterior maximum   
+
|Planck_545 || Real*4 || MJy/sr || Model flux in the Planck 545 GHz band   
 
|-
 
|-
−
|BETA_ML_HM1 || Real*4 || NA || First half-mission emissivity index posterior maximum   
+
|Planck_353 || Real*4 || MJy/sr || Model flux in the Planck 353 GHz band
 
|-
 
|-
−
|BETA_ML_HM2 || Real*4 || NA || Second half-mission emissivity index posterior maximum    
+
|WISE_12 || Real*4 || MJy/sr || Model flux in the WISE 12 micron band    
 
|-
 
|-
−
|BETA_ML_HR1 || Real*4 || NA || First half-ring emissivity index posterior maximum   
+
|IRAS_60 || Real*4 || MJy/sr || Model flux in the IRAS 60 micron band    
−
|-
 
−
|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    
 
 
|-
 
|-
 +
|IRAS_100 || Real*4 || MJy/sr || Model flux in the IRAS 100 micron band   
 
|}
 
|}
  
−
'''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:
+
== Thermal dust and CIB all-sky maps from GNILC component separation ==
−
* (Only low-resolution analysis) Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}
+
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.
−
* (Only low-resolution analysis) Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}
+
 
−
* (Only low-resolution analysis) Full-mission 70 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=70|period=Full|link=LFI 70 GHz frequency maps}}
+
===Method===
−
* Full-mission 100 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=100|period=Full|link=HFI 100 GHz frequency maps}}
+
 
−
* Full-mission 143 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=143|period=Full|link=HFI 143 GHz frequency maps}}
+
: 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.
−
* Full-mission 217 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=217|period=Full|link=HFI 217 GHz frequency maps}}
+
 
−
* Full-mission 353 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=353|period=Full|link=HFI 353 GHz frequency maps}}
+
===Data===
−
In the low-resolution analysis, all maps are smoothed to a common resolution of 40 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256. In the high-resolution analysis (including only CMB and thermal dust emission), the corresponding resolution is 10 arcmin FWHM and Nside=1024.
+
 
 +
: The data used by GNILC for the analysis are the Planck data release 2 (PR2) frequency maps from 30 to 857 GHz, and a 100 micron hybrid map combined from the SFD map ([http://adsabs.harvard.edu/abs/1998ApJ...500..525S  Schlegel et al, ApJ 1998]) at large angular scales (> 30') and the IRIS map ([http://adsabs.harvard.edu/abs/2005ApJS..157..302M  Miville-Deschênes et al, ApJS 2005]) at small angular scales (< 30'). This special 100 micron map can be obtained in the External Maps section of the PLA.
 +
 
 +
===Pre-processing===
 +
 
 +
: The point-sources with a signal-to-noise ratio, S/N > 5, in each individual frequency map (30 to 857 GHz, and 100 micron) have been pre-processed by a minimum curvature surface inpainting technique ([http://adsabs.harvard.edu/abs/2015MNRAS.451.4311R  Remazeilles et al, MNRAS 2015]) prior to performing component separation with GNILC.
 +
 
 +
===GNILC thermal dust and CIB products===
  
−
'''Outputs'''
+
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.
−
'''Synchrotron emission'''
 
  
−
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits|link=COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits}}
+
====Thermal dust maps====
−
: Nside = 256
 
−
: Angular resolution = 40 arcmin
 
  
−
: Reference frequency: 30 GHz
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ HDU -- COMP-MAP-SynchrotronPol
+
|+ HDU -- COMP-MAP-DUST
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
! Column Name || Data Type || Units || Description
+
! File Name || Nside || Units || Reference frequency || Angular resolution || Description
 
|-
 
|-
−
|Q_ML_FULL || Real*4 || K_RJ km/s || Full-mission Stokes Q posterior maximum   
+
|{{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
 
|-
 
|-
−
|U_ML_FULL || Real*4 || K_RJ km/s || Full-mission Stokes U posterior maximum   
+
|{{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
 
|-
 
|-
−
|Q_ML_HM1 || Real*4 || K_RJ km/s || First half-mission Stokes Q posterior maximum   
+
|{{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
−
|-
 
−
|U_ML_HM1 || Real*4 || K_RJ km/s || First half-mission Stokes U posterior maximum   
 
 
|-
 
|-
−
|Q_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission Stokes Q posterior maximum   
+
|{{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
 
|-
 
|-
−
|U_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission Stokes U posterior maximum   
+
|{{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
 
|-
 
|-
−
|Q_ML_HR1 || Real*4 || K_RJ km/s || First half-ring Stokes Q posterior maximum   
+
|{{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
 
|-
 
|-
−
|U_ML_HR1 || Real*4 || K_RJ km/s || First half-ring Stokes U posterior maximum   
+
|{{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
 
|-
 
|-
−
|Q_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring Stokes Q posterior maximum   
+
| {{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
 
|-
 
|-
−
|U_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring Stokes U posterior maximum   
 
−
|-
 
−
|Q_ML_YR1 || Real*4 || K_RJ km/s || "First year" Stokes Q posterior maximum   
 
−
|-
 
−
|U_ML_YR1 || Real*4 || K_RJ km/s || "First year" Stokes U posterior maximum   
 
−
|-
 
−
|Q_ML_YR2 || Real*4 || K_RJ km/s || "Second year" Stokes Q posterior maximum
 
−
|-
 
−
|U_ML_YR2 || Real*4 || K_RJ km/s || "Second year" Stokes U posterior maximum     
 
 
|}
 
|}
  
 +
====CIB maps====
  
−
'''Thermal dust emission'''
 
−
 
−
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_DustPol-commander_1024_R2.00.fits|link=COM_CompMap_DustPol-commander_1024_R2.00.fits}}
 
−
: Nside = 1024
 
−
: Angular resolution = 10 arcmin
 
  
−
: Reference frequency: 353 GHz
 
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
−
|+ HDU -- COMP-MAP-DustPol
+
|+ HDU -- COMP-MAP-CIB
 
|-
 
|-
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
−
! Column Name || Data Type || Units || Description
+
! File Name || Nside || Units || Reference frequency || Angular resolution || Description
 
|-
 
|-
−
|Q_ML_FULL || Real*4 || uK_RJ || Full-mission Stokes Q posterior maximum   
+
|{{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
 
|-
 
|-
−
|U_ML_FULL || Real*4 || uK_RJ || Full-mission Stokes U posterior maximum   
+
|{{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
 
|-
 
|-
−
|Q_ML_HM1 || Real*4 || uK_RJ || First half-mission Stokes Q posterior maximum   
+
|{{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
 
|-
 
|-
−
|U_ML_HM1 || Real*4 || uK_RJ || First half-mission Stokes U posterior maximum   
+
|}
 +
 
 +
 
 +
== Other Special maps ==
 +
 
 +
===Introduction===
 +
 
 +
This section describes the map-based products that required special processing.
 +
 
 +
 
 +
=== 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 [[: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.
 +
 
 +
<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.
 +
 
 +
<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.
 +
 
 +
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_R2.02.fits.tgz '''
 +
|-  bgcolor="ffdead" 
 +
! Filename || Format || Description
 
|-
 
|-
−
|Q_ML_HM2 || Real*4 || uK_RJ || Second half-mission Stokes Q posterior maximum   
+
| 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.
 
|-
 
|-
−
|U_ML_HM2 || Real*4 || uK_RJ || Second half-mission Stokes U posterior maximum   
+
| 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.
 
|-
 
|-
−
|Q_ML_HR1 || Real*4 || uK_RJ || First half-ring Stokes Q posterior maximum   
+
| 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.
 
|-
 
|-
−
|U_ML_HR1 || Real*4 || uK_RJ || First half-ring Stokes U posterior maximum   
+
| 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.
 
|-
 
|-
−
|Q_ML_HR2 || Real*4 || uK_RJ || Second half-ring Stokes Q posterior maximum   
+
| 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.
 
|-
 
|-
−
|U_ML_HR2 || Real*4 || uK_RJ || Second half-ring Stokes U posterior maximum   
+
| 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.
 
|-
 
|-
−
|Q_ML_YR1 || Real*4 || uK_RJ || "First year" Stokes Q posterior maximum   
+
| 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.
 
|-
 
|-
−
|U_ML_YR1 || Real*4 || uK_RJ || "First year" Stokes U posterior maximum   
+
| 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.
 
|-
 
|-
−
|Q_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes Q posterior maximum
+
| masks.fits || HEALPix FITS format map, with <math> N_{\rm  side} = 2048 </math> || Contains foreground masks.
 
|-
 
|-
−
|U_ML_YR2 || Real*4 || uK_RJ || "Second year" Stokes U posterior maximum     
+
| nilc_bands.fits || ASCII table FITS format || Contains NILC wavelet bands in multipole space
 
|}
 
|}
  
−
''' Modelling of the thermal dust emission with the Draine and Li dust model '''
+
=== 2015 Integrated Sachs-Wolfe effect map ===
  
−
The Planck, IRAS, and WISE infrared observations were fit with the dust model presented by Draine & Li in 2007 (DL07).
+
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:
−
The input maps, the DL07 model, and the fitting procedure and results are presented in {{PlanckPapers|planck2014-XXIX}}.  
 
−
Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.
 
  
−
'''Inputs'''
+
* 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)
  
−
The following data have been fit:
+
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].
  
−
* WISE 12 micron map
+
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.
−
* IRAS 60 micron map
 
−
* IRAS 100 micron map
 
−
* Full-mission 353 GHz PR2 map
 
−
* Full-mission 545 GHz PR2 map
 
−
* Full-mission 857 GHz PR2 map
 
  
−
The CIB monopole, the CMB anisotropries and the zodiacal light were subtracted to obtain dust emission maps from the sky emission maps.
 
−
All maps were smoothed to a common angular resolution of 5'.
 
  
−
'''Model Parameters'''
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 +
|+ ''' 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.
 +
|}
  
−
For each pixel of the inputs maps, we have fitted four parameters of the DL07 model:
 
  
−
* the dust mass surface density, Sigma_Mdust,
+
=== 2015 Low-frequency foregrounds maps (Planck only & Planck+WMAP) ===
−
* the dust mass fraction in small PAH grains, q_PAH,
+
1) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck only)
−
* 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  
+
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.)
−
chi2 of the fit per degree of freedom.
 
  
−
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits}}
+
2) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck + WMAP)
−
: Nside = 2048
+
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}}.)
−
: Angular resolution = 5 arcmin
 
  
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
+
</div>
−
|+ HDU -- COMP-MAP-Dust-DL07-Parameters
+
</div>
−
|-
 
−
|- bgcolor="ffdead" 
 
−
! 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'''
+
<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #EEE8AA;width:80%">
 +
'''Astrophysical components based on the 2013 data release'''
 +
<div class="mw-collapsible-content">
  
−
We provide two exinctions maps at the visible V band: the value from the model (Av_DL) and the 
+
''' Overview '''
−
renormalized one (Av_RQ) that matches extinction estimates for quasars (QSOs) derived from the Sloan digital sky survey (SDSS) data.
 
  
−
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits}}
+
This section describes the maps of astrophysical components produced from the Planck data.  These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.
−
: Nside = 2048
+
All the details can be found in {{PlanckPapers|planck2013-p06}}.
−
: Angular resolution = 5 arcmin
 
  
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
+
'''CMB maps'''
−
|+ HDU -- COMP-MAP-Dust-DL07-AvMaps
 
−
|-
 
−
|- bgcolor="ffdead" 
 
−
! 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.
+
CMB maps have been produced by the SMICA, NILC, SEVEM and COMMANDER-Ruler pipelines. Of these, the SMICA product is considered the preferred one overall and is labelled ''Main product'' in the Planck Legacy Archive, while the other two are labeled as ''Additional product''.
  
−
: File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits}}
+
SMICA and NILC also produce ''inpainted'' maps, in which the Galactic Plane, some bright regions and masked point sources are replaced with a constrained CMB realization such that the whole map has the same statistical distribution as the observed CMB.
−
: Nside = 2048
 
−
: Angular resolution = 5 arcmin
 
  
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
+
The results of SMICA, NILC and SEVEM pipeline are distributed as a FITS file containing 4 extensions:
−
|+ HDU -- COMP-MAP-Dust-DL07-ModelFluxes
+
# CMB maps and ancillary products (3 or 6 maps)
−
|-
+
# CMB-cleaned foreground maps from LFI (3 maps)
−
|- bgcolor="ffdead" 
+
# CMB-cleaned foreground maps from HFI (6 maps)
−
! Column Name || Data Type || Units || Description
+
# Effective beam of the CMB maps (1 vector)
−
|-
 
−
|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   
 
−
|}
 
  
 +
The results of COMMANDER-Ruler are distributed as two FITS files (the high and low resolution) containing the following extensions:
 +
High resolution N$_\rm{side}$=2048 (note that we don't provide the CMB-cleaned foregrounds maps for LFI and HFI because the Ruler resolution (~7.4') is lower than the HFI highest channel and and downgrading it will introduce noise correlation).
 +
# CMB maps and ancillary products (4 maps)
 +
# Effective beam of the CMB maps (1 vector)
  
−
''' Other Special maps '''
+
Low resolution N$_\rm{side}$=256
−
 
+
# CMB maps and ancillary products (3 maps)
−
'''Introduction'''
+
# 10 example CMB maps used in the montecarlo realization (10 maps)
 +
# Effective beam of the CMB maps (1 vector)
  
−
This section describes the map-based products that required special processing.
+
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.
  
−
''' 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}}.
+
{| class="wikitable" border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center" style="background:#efefef;"
−
 
+
|+ style="background:#eeeeee;" | '''The maps (CMB, noise, masks) contained in the first extension'''
−
 
 
−
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>.
+
!width=40px | Col name
 +
!width=200px| SMICA
 +
!width=200px| NILC
 +
!width=200px| SEVEM
 +
!width=200px| COMMANDER-Ruler H
 +
!width=200px| COMMANDER-Ruler L  
 +
!width=300px| Description / notes
 
|-
 
|-
−
| mask.fits.gz || HEALPix FITS format map, with <math>N_{\rm  side}=2048</math> || Contains the lens reconstruction analysis mask.
+
| align="left" | 1: I
 +
| [[File: CMB-smica.png|200px]]
 +
| [[File: CMB-nilc.png|200px]]
 +
| [[File: CMB-sevem.png|200px]]
 +
| [[File: CMB-CR_h.png|200px]]
 +
| [[File: CMB-CR_l.png|200px]]
 +
| Raw CMB anisotropy map.  These are the maps used in the component separation paper {{PlanckPapers|planck2013-p06}}.
 
|-
 
|-
−
| 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}}.
+
| 2: NOISE
−
|}
+
| [[File: CMBnoise-smica.png|200px]]
−
 
+
| [[File: CMBnoise-nilc.png|200px]]
−
''' 2015 Compton <i>y</i> parameter map '''
+
| [[File: CMBnoise-sevem.png|200px]]
−
 
+
| [[File: CMBnoise-CR_h.png|200px]]
−
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.  
+
| align='center' | not applicable
−
 
+
| Noise map. Obtained by propagating the half-ring noise through the CMB cleaning pipelines.
−
<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.
+
| 3: VALMASK
 +
| [[File: valmask-smica.png|200px]]
 +
| [[File: valmask-nilc.png|200px]]
 +
| [[File: valmask-sevem.png|200px]]
 +
| [[File: valmask-cr_h.png|200px]]
 +
| [[File: valmask-cr_l.png|200px]]
 +
| Confidence map. Pixels with an expected low level of foreground contamination.  These maps are only indicative and obtained by different ad hoc methods. They cannot be used to rank the CMB maps.
 
|-
 
|-
−
| 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.
+
| 4: I_MASK
−
|-
+
| [[File: cmbmask-smica.png|200px]]
−
| 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.
+
| [[File: cmbmask-nilc.png|200px]]
 +
| align='center' | not applicable
 +
| align='center' | not applicable
 +
| align='center' | not applicable
 +
| Some areas are masked for the production of the raw CMB maps (for NILC: point sources from 44 GHz to 857 GHz; for SMICA: point sources from 30 GHz to 857 GHz, Galatic region and additional bright regions).
 
|-
 
|-
−
| 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.
+
| 5: INP_CMB
 +
| [[File: CMBinp-smica.png|200px]]
 +
| [[File: CMBinp-nilc.png|200px]]
 +
| align='center' | not applicable
 +
| align='center' | not applicable
 +
| align='center' | not applicable
 +
| Inpainted CMB map.  The raw CMB maps with some regions (as indicated by INP_MASK) replaced by a constrained Gaussian realization. The inpainted SMICA map was used for PR.
 
|-
 
|-
−
| 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.
+
| 6: INP_MASK
−
|-
+
| [[File: inpmask-smica.png|200px]]
−
| 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.
+
| [[File: inpmask-nilc.png|200px]]
−
|-
+
| align='center' | not applicable
−
| 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.
+
| align='center' | not applicable
−
|-
+
| align='center' | not applicable
−
| 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.
+
| Mask of the inpainted regions. For SMICA, this is identical to I_MASK.   For NILC, it is not.
−
|-
+
|}
−
| 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
 
−
|}
 
  
 +
The component separation pipelines are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation|CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.
  
−
''' 2015 lensing-induced <i>B</i>-mode map '''
+
The union (or common) mask is defined as the union of the confidence masks from the four component separation pipelines, the three listed above and Commander-Ruler. It leaves 73% of the sky available, and so it is denoted as U73.
  
−
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.
+
'''Product description '''
  
−
''' Raw products '''
+
'''SMICA'''
  
−
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
+
; Principle
 +
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole.  It includes multipoles up to <math>\ell = 4000</math>.
 +
; Resolution (effective beam)
 +
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''.  It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function.  Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function.  Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.
 +
; Confidence mask
 +
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources.  This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel.
 +
; Masks and inpainting
 +
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'.  The raw SMICA map has been inpainted, producing the map named "INP_CMB".  Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.
  
−
<math> \begin{eqnarray}
+
'''NILC'''
−
\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.   
+
; Principle
 +
: The Needlet-ILC (hereafter NILC) CMB map is constructed from all Planck channels from 44 to 857 GHz and includes multipoles up to <math>\ell = 3200</math>.  It is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range.
 +
; Resolution (effective beam)
 +
: As in the SMICA product except that there is no abrupt truncation at <math>\ell_{max}= 3200</math> but a smooth transition to <math>0</math> over the range <math>2700\leq\ell\leq 3200</math>.
 +
; Confidence mask
 +
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources.  This mask provides a qualitative indication of the cleanliness of a pixel.  The threshold is somewhat arbitrary.
 +
; Masks and inpainting
 +
: The raw NILC map has valid pixels except at the location of masked point sources.  This is indicated with the mask named 'I_MASK'.  The raw NILC map has been inpainted, producing the map named "INP_CMB".  The inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.
  
−
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
+
'''SEVEM'''
−
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
+
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations{{BibCite|leach2008}} and to WMAP polarisation data{{BibCite|fernandezcobos2012}}. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Note that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB ma (''I_MASK'') nor an inpainted version of the map and its associated mask.  On the other hand, it provides ''channel maps'' and 100, 143, and 217 GHz which are used as the building blocks of the final map.
−
 
−
<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 '''  
+
'''COMMANDER-Ruler'''
  
−
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.  
+
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at $N_\rm{side}$=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which
 +
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the {{PlanckPapers|planck2013-p06|1|Planck Component Separation paper}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of:
  
−
It can also be constructed using the raw products described above from  
+
* Maps of the Amplitudes of the CMB at low resolution, $N_\rm{side}$=256, along with the standard deviations of the outputs, beam profiles derived from the production process.
 +
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, $N_\rm{side}$=2048, beam profiles derived from the production process.
 +
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.
  
−
<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>,
+
'''Production process'''
  
−
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.
+
'''SMICA'''
  
−
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>:
+
; 1) Pre-processing
−
+
: All input maps undergo a pre-processing step to deal with point sources.  The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz,  here all point sources with SNR > 7.5 are masked and filled-in similarly.
−
<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>,
+
; 2) Linear combination
 +
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.
 +
; 3) Post-processing
 +
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.
  
−
where <math> G_\ell </math> is the 5 arcmin Gaussian beam that convolves the SMICA CMB maps.  
+
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.
  
  
−
The 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.
+
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]
  
 +
'''NILC'''
 +
 +
; 1) Pre-processing
 +
: Same pre-processing as SMICA (except the 30 GHz channel is not used).
 +
; 2) Linear combination
 +
: The pre-processed Planck frequency channels from 44 to 857 GHz are linearly combined with weights which depend on location on the sky and on the multipole range up to <math>\ell = 3200</math>.  This is achieved using a needlet (redundant spherical wavelet) decomposition.  For more details, see {{PlanckPapers|planck2013-p06}}.
 +
; 3) Post-processing
 +
: The areas masked in the pre-processing plus other bright regions step are replaced by a constrained Gaussian realization as in the SMICA post-processing step.
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
+
'''SEVEM'''
−
|+ ''' 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 L70 mask.
 
−
|-
 
−
| mask_noapo.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm  side} = 2048 </math> || The L70 mask without apodization.
 
−
|-
 
−
| transfer_function_b_l.dat || ASCII text file, with columns = (<math>\ell</math>, <math> \mathcal{B}_\ell </math>) || The transfer function.
 
−
|-
 
−
| 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 9 of {{PlanckPapers|planck2015-XLI}} (for plotting purposes only).
 
−
|}
 
  
−
''' 2015 Integrated Sachs-Wolfe effect map '''
+
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.
  
−
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 construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math>
 +
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).
 +
 
 +
An additional level of flexibility can also be considered: the linear coefficients can be the same for all the sky, or several regions with different sets of coefficients can be considered. The regions are then combined in a smooth way, by weighting the pixels at the boundaries, to avoid discontinuities in the clean maps.
 +
Since the method is linear, we may easily propagate the noise properties to the final CMB map. Moreover, it is very fast and permits the generation of thousands of simulations to character- ize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.
  
−
* 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
+
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.
−
* 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].
+
In particular, we have cleaned the 143 GHz and 217 GHz maps using four templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and (857-545). For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). In order to take into account the different spectral behaviour of the foregrounds at low and high galactic latitudes, we have considered two independent regions of the sky, for which we have used a different set of coefficients. The first region corresponds to the 3 per cent brightest Galactic emission, whereas the second region is defined by the remaining 97 per cent of the sky. For the first region, the coefficients are actually estimated over the whole sky (we find that this is more optimal than perform the minimisation only on the 3 per cent brightest region, where the CMB emission is very sub-dominant) while for the second region, we exclude the 3 per cent brightest region of the sky, point sources detected at any frequency and those pixels which have not been observed at all channels.
 +
Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.
  
−
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.
+
Moreover, additional CMB clean maps (at frequencies between 44 and 353 GHz) have also been produced using different combinations of templates for some of the analyses carried out in {{PlanckPapers|planck2013-p09}} and {{PlanckPapers|planck2013-p14}}. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in {{PlanckPapers|planck2013-p14}}, while frequencies from 70 to 217 GHz were used for consistency tests in {{PlanckPapers|planck2013-p09}}.
  
 +
'''COMMANDER-Ruler'''
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
+
The production process consist in low and high resolution runs according to the description above.  
−
|+ ''' Contents of the ISW maps file: COM_CompMap_ISW_0064_R2.00.fits '''
+
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA.  
−
|-  bgcolor="ffdead"
+
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA.  
−
! 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.
 
−
|}
 
  
 +
''' Masks '''
  
−
''' 2015 Low-frequency foregrounds maps (Planck only & Planck+WMAP) '''
+
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 CMB maps.
−
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.)
+
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 +
|-
 +
|- bgcolor="ffdead" 
 +
! Commander 2013 (PR1) || Used for diffuse inpainting of input frequency maps || Used for constrained Gaussian realization inpaiting of CMB map  || Description
 +
|-
 +
|VALMASK || NO || NO || VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside
  
−
2) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck + WMAP)
+
{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_2048_R1.00.fits|link=COM_CompMap_CMB-commrul_2048_R1.00.fits}} and {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_0256_R1.00.fits|link=COM_CompMap_CMB-commrul_0256_R1.00.fits}} for low resolution analyses.
−
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}}.)
+
|-
−
 
+
|- bgcolor="800000"
−
</div>
+
|
−
</div>
+
! ||
 +
|
 +
|- bgcolor="ffdead" 
 +
! SEVEM 2013 (PR1) || Used diffuse inpainting of input frequency maps || Used for Constrained Gaussian realization inpaiting of CMB map || Description
 +
|-
 +
|VALMASK || NO || NO || VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside
  
−
<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #EEE8AA;width:80%">
+
{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.12.fits|link=COM_CompMap_CMB-sevem_2048_R1.12.fits}}.
−
'''Astrophysical components based on the 2013 data release'''
+
|-
−
<div class="mw-collapsible-content">
+
|- bgcolor="800000"
−
 
+
|
−
''' 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 the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.
+
|- bgcolor="ffdead"
−
All the details can be found in {{PlanckPapers|planck2013-p06}}.
+
! NILC 2013 (PR1) || Used for diffuse inpainting of input frequency maps || Used for constrained Gaussian realization inpaiting of CMB map || Description
−
 
+
|-
−
'''CMB maps'''
+
|VALMASK || NO || NO || VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.fits}}.
−
 
+
|-
−
 
+
|I_MASK || NO || NO || I_MASK defines the regions over which CMB is not built. It is a combination of point source masks, Galactic plane mask and other bright regions like LMC, SMC, etc. It can be found inside {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.fits}}.
−
CMB maps have been produced by the SMICA, NILC, SEVEM and COMMANDER-Ruler pipelines. Of these, the SMICA product is considered the preferred one overall and is labelled ''Main product'' in the Planck Legacy Archive, while the other two are labeled as ''Additional product''.
+
|- 
 +
|INP_MASK || NO || YES || It can be found inside {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.fits}}.
 +
|-
 +
|-
 +
|- bgcolor="800000"
 +
|
 +
! ||
 +
|
 +
|- bgcolor="ffdead" 
 +
! SMICA 2013 (PR1) || Used for diffuse inpainting of input frequency maps || Used for constrained Gaussian realization inpaiting of CMB map  || Description
 +
|-
 +
|VALMASK || NO || NO || VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside
 +
 
 +
{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.20.fits|link=COM_CompMap_CMB-smica_2048_R1.20.fits}}.
 +
|-
 +
|I_MASK || YES || YES || I_MASK defines the regions over which CMB is not built. It is a combination of point source masks, Galactic plane mask and other bright regions like LMC, SMC, etc. It can be found inside {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.20.fits|link=COM_CompMap_CMB-smica_2048_R1.20.fits}}.
 +
|- 
 +
|INP_MASK || YES || YES || INP_MASK for SMICA 2013 release is identical to I_MASK above. 
 +
|-
 +
|-
 +
|}
  
−
SMICA and NILC also produce ''inpainted'' maps, in which the Galactic Plane, some bright regions and masked point sources are replaced with a constrained CMB realization such that the whole map has the same statistical distribution as the observed CMB. 
 
  
−
The results of SMICA, NILC and SEVEM pipeline are distributed as a FITS file containing 4 extensions:
+
'''Inputs'''
−
# CMB maps and ancillary products (3 or 6 maps)
 
−
# CMB-cleaned foreground maps from LFI (3 maps)
 
−
# CMB-cleaned foreground maps from HFI (6 maps)
 
−
# Effective beam of the CMB maps (1 vector)
 
  
−
The results of COMMANDER-Ruler are distributed as two FITS files (the high and low resolution) containing the following extensions:  
+
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz.
−
High resolution N$_\rm{side}$=2048 (note that we don't provide the CMB-cleaned foregrounds maps for LFI and HFI because the Ruler resolution (~7.4') is lower than the HFI highest channel and and downgrading it will introduce noise correlation).  
+
 
−
# CMB maps and ancillary products (4 maps)
+
'''File names and structure'''
−
# Effective beam of the CMB maps (1 vector)
+
 
 +
The FITS files corresponding to the three CMB products are the following:
 +
 
 +
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.fits}}
 +
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.12.fits|link=COM_CompMap_CMB-sevem_2048_R1.12.fits}}
 +
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.20.fits|link=COM_CompMap_CMB-smica_2048_R1.20.fits}}
 +
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_2048_R1.00.fits|link=COM_CompMap_CMB-commrul_2048_R1.00.fits}}
 +
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_0256_R1.00.fits|link=COM_CompMap_CMB-commrul_0256_R1.00.fits}}
  
−
Low resolution N$_\rm{side}$=256
 
−
# CMB maps and ancillary products (3 maps)
 
−
# 10 example CMB maps used in the montecarlo realization (10 maps)
 
−
# Effective beam of the CMB maps (1 vector)
 
  
−
For a complete description of the data structure, see the [[#File names and structure | below]]; the content of the first extensions is illustrated and commented in the table below.
+
The files contain a minimal primary extension with no data and four ''BINTABLE'' data extensions. Each column of the ''BINTABLE'' is a (Healpix) map; the column names and the most important keywords of each extension are described in the table below; for the remaining keywords, please see the FITS files directly.  
  
  
−
{| class="wikitable"  border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center" style="background:#efefef;"
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
−
|+ style="background:#eeeeee;" | '''The maps (CMB, noise, masks) contained in the first extension'''
+
|+ '''CMB map file data structure'''
 +
|- bgcolor="ffdead"  
 +
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data Type || Units || Description
 
|-
 
|-
−
!width=40px | Col name
+
|I    || Real*4 || uK_cmb || CMB temperature map
−
!width=200px| SMICA
+
|-
−
!width=200px| NILC
+
|NOISE  || Real*4 || uK_cmb || Estimated noise map (note 1)
−
!width=200px| SEVEM
 
−
!width=200px| COMMANDER-Ruler H
 
−
!width=200px| COMMANDER-Ruler L
 
−
!width=300px| Description / notes
 
 
|-
 
|-
−
| align="left" | 1: I
+
|I_STDEV|| Real*4 || uK_cmb || Standard deviation, ONLY on COMMANDER-Ruler products
−
| [[File: CMB-smica.png|200px]]
 
−
| [[File: CMB-nilc.png|200px]]
 
−
| [[File: CMB-sevem.png|200px]]
 
−
| [[File: CMB-CR_h.png|200px]]
 
−
| [[File: CMB-CR_l.png|200px]]
 
−
| Raw CMB anisotropy map.  These are the maps used in the component separation paper {{PlanckPapers|planck2013-p06}}.
 
 
|-
 
|-
−
| 2: NOISE
+
|VALMASK|| Byte || none || Confidence mask (note 2)
−
| [[File: CMBnoise-smica.png|200px]]
 
−
| [[File: CMBnoise-nilc.png|200px]]
 
−
| [[File: CMBnoise-sevem.png|200px]]
 
−
| [[File: CMBnoise-CR_h.png|200px]]
 
−
| align='center' | not applicable
 
−
| Noise map.  Obtained by propagating the half-ring noise through the CMB cleaning pipelines.
 
 
|-
 
|-
−
| 3: VALMASK
+
|I_MASK|| Byte || none || Mask of regions over which CMB map is not built (Optional - see note 3)
−
| [[File: valmask-smica.png|200px]]
+
|-
−
| [[File: valmask-nilc.png|200px]]
+
|INP_CMB || Real*4 || uK_cmb ||  Inpainted CMB temperature map (Optional - see note 3)
−
| [[File: valmask-sevem.png|200px]]
+
|-
−
| [[File: valmask-cr_h.png|200px]]
+
|INP_MASK || Byte || none || mask of inpainted pixels (Optional - see note 3)
−
| [[File: valmask-cr_l.png|200px]]
 
−
| Confidence map. Pixels with an expected low level of foreground contamination.  These maps are only indicative and obtained by different ad hoc methods.  They cannot be used to rank the CMB maps.
 
 
|-
 
|-
−
| 4: I_MASK
+
|- bgcolor="ffdead" 
−
| [[File: cmbmask-smica.png|200px]]
+
! Keyword || Data Type || Value || Description
−
| [[File: cmbmask-nilc.png|200px]]
 
−
| align='center' | not applicable
 
−
| align='center' | not applicable
 
−
| align='center' | not applicable
 
−
| Some areas are masked for the production of the raw CMB maps (for NILC: point sources from 44 GHz to 857 GHz; for SMICA: point sources from 30 GHz to 857 GHz, Galatic region and additional bright regions).
 
 
|-
 
|-
−
| 5: INP_CMB
+
|AST-COMP ||  String || CMB || Astrophysical compoment name
−
| [[File: CMBinp-smica.png|200px]]
 
−
| [[File: CMBinp-nilc.png|200px]]
 
−
| align='center' | not applicable
 
−
| align='center' | not applicable
 
−
| align='center' | not applicable
 
−
| Inpainted CMB map.  The raw CMB maps with some regions (as indicated by INP_MASK) replaced by a constrained Gaussian realization.  The inpainted SMICA map was used for PR.
 
−
|-
 
−
| 6: INP_MASK
 
−
| [[File: inpmask-smica.png|200px]]
 
−
| [[File: inpmask-nilc.png|200px]]
 
−
| align='center' | not applicable
 
−
| align='center' | not applicable
 
−
| align='center' | not applicable
 
−
| Mask of the inpainted regions.  For SMICA, this is identical to I_MASK.  For NILC, it is not.
 
−
|}
 
−
 
 
−
The component separation pipelines are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation|CMB and foreground separation]] section and also in Section 3 and Appendices A-D of {{PlanckPapers|planck2013-p06}} and references therein.
 
−
 
 
−
The union (or common) mask is defined as the union of the confidence masks from the four component separation pipelines, the three listed above and Commander-Ruler. It leaves 73% of the sky available, and so it is denoted as U73.
 
−
 
 
−
 
 
−
'''Product description '''
 
−
 
 
−
'''SMICA'''
 
−
 
 
−
; Principle
 
−
: SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole.  It includes multipoles up to <math>\ell = 4000</math>.
 
−
; Resolution (effective beam)
 
−
: The SMICA map has an effective beam window function of 5 arc-minutes truncated at <math>\ell=4000</math> '''and deconvolved from the pixel window'''.  It means that, ideally, one would have <math>C_\ell(map) = C_\ell(sky) * B_\ell(5')^2</math>, where <math>C_\ell(map)</math> is the angular spectrum of the map, where <math>C_\ell(sky)</math> is the angular spectrum of the CMB and <math>B_\ell(5')</math> is a 5-arcminute Gaussian beam function.  Note however that, by convention, the effective beam window function <math>B_\ell(fits)</math> provided in the FITS file does include a pixel window function.  Therefore, it is equal to <math>B_\ell(fits) = B_\ell(5') / p_\ell(2048)</math> where <math>p_\ell(2048)</math> denotes the pixel window function for an Nside=2048 pixelization.
 
−
; Confidence mask
 
−
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources.  This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel.
 
−
; Masks and inpainting
 
−
: The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions.  Those invalid pixels are indicated with the mask named 'I_MASK'.  The raw SMICA map has been inpainted, producing the map named "INP_CMB".  Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.
 
−
 
 
−
'''NILC'''
 
−
 
 
−
; Principle
 
−
: The Needlet-ILC (hereafter NILC) CMB map is constructed from all Planck channels from 44 to 857 GHz and includes multipoles up to <math>\ell = 3200</math>.  It is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range.
 
−
; Resolution (effective beam)
 
−
: As in the SMICA product except that there is no abrupt truncation at <math>\ell_{max}= 3200</math> but a smooth transition to <math>0</math> over the range <math>2700\leq\ell\leq 3200</math>.
 
−
; Confidence mask
 
−
: A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources.  This mask provides a qualitative indication of the cleanliness of a pixel.  The threshold is somewhat arbitrary.
 
−
; Masks and inpainting
 
−
: The raw NILC map has valid pixels except at the location of masked point sources.  This is indicated with the mask named 'I_MASK'.  The raw NILC map has been inpainted, producing the map named "INP_CMB".  The inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.
 
−
 
 
−
'''SEVEM'''
 
−
 
 
−
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations{{BibCite|leach2008}} and to WMAP polarisation data{{BibCite|fernandezcobos2012}}. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.  Note that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB ma (''I_MASK'') nor an inpainted version of the map and its associated mask.  On the other hand, it provides ''channel maps'' and 100, 143, and 217 GHz which are used as the building blocks of the final map.
 
−
 
 
−
'''COMMANDER-Ruler'''
 
−
 
 
−
COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at $N_\rm{side}$=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which
 
−
is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the {{PlanckPapers|planck2013-p06|1|Planck Component Separation paper}} additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of:
 
−
 
 
−
* Maps of the Amplitudes of the CMB at low resolution, $N_\rm{side}$=256, along with the standard deviations of the outputs, beam profiles derived from the production process.
 
−
* Maps of the CMB amplitude, along with the standard deviations, at high resolution, $N_\rm{side}$=2048, beam profiles derived from the production process.
 
−
* Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see {{PlanckPapers|planck2013-p06}}.
 
−
 
 
−
'''Production process'''
 
−
 
 
−
'''SMICA'''
 
−
 
 
−
; 1) Pre-processing
 
−
: All input maps undergo a pre-processing step to deal with point sources.  The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz,  here all point sources with SNR > 7.5 are masked and filled-in similarly.
 
−
; 2) Linear combination
 
−
: The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to <math>\ell = 4000</math> and co-added with multipole-dependent weights as shown in the figure.
 
−
; 3) Post-processing
 
−
: The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.
 
−
 
 
−
Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.
 
−
 
 
−
 
 
−
[[File:smica.jpg|thumb|center|500px|'''Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]
 
−
 
 
−
'''NILC'''
 
−
 
 
−
; 1) Pre-processing
 
−
: Same pre-processing as SMICA (except the 30 GHz channel is not used).
 
−
; 2) Linear combination
 
−
: The pre-processed Planck frequency channels from 44 to 857 GHz are linearly combined with weights which depend on location on the sky and on the multipole range up to <math>\ell = 3200</math>.  This is achieved using a needlet (redundant spherical wavelet) decomposition.  For more details, see {{PlanckPapers|planck2013-p06}}.
 
−
; 3) Post-processing
 
−
: The areas masked in the pre-processing plus other bright regions step are replaced by a constrained Gaussian realization as in the SMICA post-processing step.
 
−
 
 
−
'''SEVEM'''
 
−
 
 
−
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization{{BibCite|casaponsa2011}}) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.
 
−
 
 
−
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky: <math> T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) </math>
 
−
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).
 
−
 
 
−
An additional level of flexibility can also be considered: the linear coefficients can be the same for all the sky, or several regions with different sets of coefficients can be considered. The regions are then combined in a smooth way, by weighting the pixels at the boundaries, to avoid discontinuities in the clean maps.
 
−
Since the method is linear, we may easily propagate the noise properties to the final CMB map. Moreover, it is very fast and permits the generation of thousands of simulations to character- ize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.
 
−
 
 
−
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.
 
−
 
 
−
In particular, we have cleaned the 143 GHz and 217 GHz maps using four templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and (857-545). For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). In order to take into account the different spectral behaviour of the foregrounds at low and high galactic latitudes, we have considered two independent regions of the sky, for which we have used a different set of coefficients. The first region corresponds to the 3 per cent brightest Galactic emission, whereas the second region is defined by the remaining 97 per cent of the sky. For the first region, the coefficients are actually estimated over the whole sky (we find that this is more optimal than perform the minimisation only on the 3 per cent brightest region, where the CMB emission is very sub-dominant) while for the second region, we exclude the 3 per cent brightest region of the sky, point sources detected at any frequency and those pixels which have not been observed at all channels.
 
−
Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.
 
−
 
 
−
Moreover, additional CMB clean maps (at frequencies between 44 and 353 GHz) have also been produced using different combinations of templates for some of the analyses carried out in {{PlanckPapers|planck2013-p09}} and {{PlanckPapers|planck2013-p14}}. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in {{PlanckPapers|planck2013-p14}}, while frequencies from 70 to 217 GHz were used for consistency tests in {{PlanckPapers|planck2013-p09}}.
 
−
 
 
−
'''COMMANDER-Ruler'''
 
−
 
 
−
The production process consist in low and high resolution runs according to the description above.
 
−
; Low Resolution Runs: Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA.
 
−
; Ruler Runs: the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA.
 
−
 
 
−
''' Masks '''
 
−
 
 
−
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 CMB maps.
 
−
 
 
−
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
 
−
|-
 
−
|- bgcolor="ffdead" 
 
−
! Commander 2013 (PR1) || Used for diffuse inpainting of input frequency maps || Used for constrained Gaussian realization inpaiting of CMB map  || Description
 
−
|-
 
−
|VALMASK || NO || NO || VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside
 
−
 
 
−
{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_2048_R1.00.fits|link=COM_CompMap_CMB-commrul_2048_R1.00.fits}} and {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_0256_R1.00.fits|link=COM_CompMap_CMB-commrul_0256_R1.00.fits}} for low resolution analyses.
 
−
|-
 
−
|- bgcolor="800000"
 
−
|
 
−
! ||
 
−
|
 
−
|- bgcolor="ffdead" 
 
−
! SEVEM 2013 (PR1) || Used diffuse inpainting of input frequency maps || Used for Constrained Gaussian realization inpaiting of CMB map || Description
 
−
|-
 
−
|VALMASK || NO || NO || VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside
 
−
 
 
−
{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.12.fits|link=COM_CompMap_CMB-sevem_2048_R1.12.fits}}.
 
−
|-
 
−
|- bgcolor="800000"
 
−
|
 
−
! ||
 
−
|
 
−
|- bgcolor="ffdead"
 
−
! NILC 2013 (PR1) || Used for diffuse inpainting of input frequency maps || Used for constrained Gaussian realization inpaiting of CMB map || Description
 
−
|-
 
−
|VALMASK || NO || NO || VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.fits}}.
 
−
|-
 
−
|I_MASK || NO || NO || I_MASK defines the regions over which CMB is not built. It is a combination of point source masks, Galactic plane mask and other bright regions like LMC, SMC, etc. It can be found inside {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.fits}}.
 
−
|- 
 
−
|INP_MASK || NO || YES || It can be found inside {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.fits}}.
 
−
|-
 
−
|-
 
−
|- bgcolor="800000"
 
−
|
 
−
! ||
 
−
|
 
−
|- bgcolor="ffdead" 
 
−
! SMICA 2013 (PR1) || Used for diffuse inpainting of input frequency maps || Used for constrained Gaussian realization inpaiting of CMB map  || Description
 
−
|-
 
−
|VALMASK || NO || NO || VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside
 
−
 
 
−
{{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.20.fits|link=COM_CompMap_CMB-smica_2048_R1.20.fits}}.
 
−
|-
 
−
|I_MASK || YES || YES || I_MASK defines the regions over which CMB is not built. It is a combination of point source masks, Galactic plane mask and other bright regions like LMC, SMC, etc. It can be found inside {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.20.fits|link=COM_CompMap_CMB-smica_2048_R1.20.fits}}.
 
−
|- 
 
−
|INP_MASK || YES || YES || INP_MASK for SMICA 2013 release is identical to I_MASK above. 
 
−
|-
 
−
|-
 
−
|}
 
−
 
 
−
 
 
−
'''Inputs'''
 
−
 
 
−
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. SMICA and SEVEM use all the maps between 30 and 857 GHz; NILC uses the ones between 44 and 857 GHz. Commander-Ruler uses frequency channel maps from 30 to 353 GHz.
 
−
 
 
−
'''File names and structure'''
 
−
 
 
−
The FITS files corresponding to the three CMB products are the following:
 
−
 
 
−
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.20.fits|link=COM_CompMap_CMB-nilc_2048_R1.20.fits}}
 
−
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.12.fits|link=COM_CompMap_CMB-sevem_2048_R1.12.fits}}
 
−
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.20.fits|link=COM_CompMap_CMB-smica_2048_R1.20.fits}}
 
−
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_2048_R1.00.fits|link=COM_CompMap_CMB-commrul_2048_R1.00.fits}}
 
−
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-commrul_0256_R1.00.fits|link=COM_CompMap_CMB-commrul_0256_R1.00.fits}}
 
−
 
 
−
 
 
−
The files contain a minimal primary extension with no data and four ''BINTABLE'' data extensions. Each column of the ''BINTABLE'' is a (Healpix) map; the column names and the most important keywords of each extension are described in the table below; for the remaining keywords, please see the FITS files directly.
 
−
 
 
−
 
 
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 
−
|+ '''CMB map file data structure'''
 
−
|- bgcolor="ffdead" 
 
−
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)
 
−
|- bgcolor="ffdead" 
 
−
! Column Name || Data Type || Units || Description
 
−
|-
 
−
|I    || Real*4 || uK_cmb || CMB temperature map
 
−
|-
 
−
|NOISE  || Real*4 || uK_cmb || Estimated noise map (note 1)
 
−
|-
 
−
|I_STDEV|| Real*4 || uK_cmb || Standard deviation, ONLY on COMMANDER-Ruler products
 
−
|-
 
−
|VALMASK|| Byte || none || Confidence mask (note 2)
 
−
|-
 
−
|I_MASK|| Byte || none || Mask of regions over which CMB map is not built (Optional - see note 3)
 
−
|-
 
−
|INP_CMB || Real*4 || uK_cmb ||  Inpainted CMB temperature map (Optional - see note 3)
 
−
|-
 
−
|INP_MASK || Byte || none ||  mask of inpainted pixels (Optional - see note 3)
 
−
|-
 
−
|- bgcolor="ffdead" 
 
−
! Keyword || Data Type || Value || Description
 
−
|-
 
−
|AST-COMP ||  String || CMB || Astrophysical compoment name
 
 
|-
 
|-
 
|PIXTYPE ||  String || HEALPIX ||
 
|PIXTYPE ||  String || HEALPIX ||
Line 2,044: Line 1,810:
 
|}
 
|}
  
−
''' Lensing map '''
 
−
 
−
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.
 
−
 
−
'''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
 
−
*''{{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>
 
−
<gallery perrow=3 widths=260px heights=170px>
 
−
File: analysis_lens_pub_map_orth_north_dat_p.png | Galactic north
 
−
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>

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]

Astrophysical components based on the 2015 data release

Overview[edit]

This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of each product and how it is obtained, followed by a description of the FITS file containing the data and associated information. All the details can be found in Planck-2015-A10[4] and {PlanckPapers|planck20}}.

Astrophysical foregrounds from parametric component separation[edit]

We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper Planck-2015-A10[4] for a detailed description of these products. Further scientific discussion and interpretation may be found in Planck-2015-A25[5].

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 FWHM 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[edit]

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


Extension 1 -- SYNC-TEMP
Column Name Data Type Units Description
nu Real*4 Hz Frequency
intensity Real*4 W/Hz/m2/sr GALPROP z10LMPD_SUNfE spectrum


Free-free emission[edit]

File name: COM_CompMap_freefree-commander_0256_R2.00.fits
Reference frequency: NA
Nside = 256
Angular resolution = 60 arcmin
HDU -- COMP-MAP-freefree
Column Name Data Type Units Description
EM_ML Real*4 cm^-6 pc Emission measure posterior maximum
EM_MEAN Real*4 cm^-6 pc Emission measure posterior mean
EM_RMS Real*4 cm^-6 pc Emission measure posterior rms
TEMP_ML Real*4 K Electron temperature posterior maximum
TEMP_MEAN Real*4 K Electron temperature posterior mean
TEMP_RMS Real*4 K Electron temperature posterior rms


Spinning dust emission[edit]

File name: COM_CompMap_AME-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin

Note: The spinning dust component has two independent constituents, each corresponding to one spdust2 component, but with different peak frequencies. The two components are stored in the two first FITS extensions, and the template frequency spectrum is stored in the third extension.

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


Extension 2 -- SPINNING-DUST-TEMP
Column Name Data Type Units Description
nu Real*4 GHz Frequency
j_nu/nH Real*4 Jy sr-1 cm2/H spdust2 spectrum

CO line emission[edit]

File name: COM_CompMap_CO-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin

Note: The CO line emission component has three independent objects, corresponding to the J1->0, 2->1 and 3->2 lines, stored in separate extensions.

HDU -- COMP-MAP-co10
Column Name Data Type Units Description
I_ML Real*4 K_RJ km/s CO(1-0) amplitude posterior maximum
I_MEAN Real*4 K_RJ km/s CO(1-0) amplitude posterior mean
I_RMS Real*4 K_RJ km/s CO(1-0) amplitude posterior rms
Extension 1 -- COMP-MAP-co21
Column Name Data Type Units Description
I_ML Real*4 K_RJ km/s CO(2-1) amplitude posterior maximum
I_MEAN Real*4 K_RJ km/s CO(2-1) amplitude posterior mean
I_RMS Real*4 K_RJ km/s CO(2-1) amplitude posterior rms
Extension 2 -- COMP-MAP-co32
Column Name Data Type Units Description
I_ML Real*4 K_RJ km/s CO(3-2) amplitude posterior maximum
I_MEAN Real*4 K_RJ km/s CO(3-2) amplitude posterior mean
I_RMS Real*4 K_RJ km/s CO(3-2) amplitude posterior rms

94/100 GHz line emission[edit]

File name: COM_CompMap_xline-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin
HDU -- COMP-MAP-xline
Column Name Data Type Units Description
I_ML Real*4 uK_cmb Amplitude posterior maximum
I_MEAN Real*4 uK_cmb Amplitude posterior mean
I_RMS Real*4 uK_cmb Amplitude posterior rms

Note: The amplitude of this component is normalized according to the 100-ds1 detector set map, ie., it is the amplitude as measured by this detector combination.

Thermal dust emission[edit]

File name: COM_CompMap_dust-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin
Reference frequency: 545 GHz
HDU -- COMP-MAP-dust
Column Name Data Type Units Description
I_ML Real*4 uK_RJ Amplitude posterior maximum
I_MEAN Real*4 uK_RJ Amplitude posterior mean
I_RMS Real*4 uK_RJ Amplitude posterior rms
TEMP_ML Real*4 K Dust temperature posterior maximum
TEMP_MEAN Real*4 K Dust temperature posterior mean
TEMP_RMS Real*4 K Dust temperature posterior rms
BETA_ML Real*4 NA Emissivity index posterior maximum
BETA_MEAN Real*4 NA Emissivity index posterior mean
BETA_RMS Real*4 NA Emissivity index posterior rms

Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters[edit]

File name: COM_CompMap_SZ-commander_0256_R2.00.fits
Nside = 256
Angular resolution = 60 arcmin
HDU -- COMP-MAP-SZ
Column Name Data Type Units Description
Y_ML Real*4 y_SZ Y parameter posterior maximum
Y_MEAN Real*4 y_SZ Y parameter posterior mean
Y_RMS Real*4 y_SZ Y parameter posterior rms

High-resolution temperature products

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

Inputs

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

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

All maps are smoothed to a common resolution of 7.5 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=2048.

Outputs

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 FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256. In the high-resolution analysis (including only CMB and thermal dust emission), the corresponding resolution is 10 arcmin FWHM and Nside=1024.

Outputs 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 K_RJ km/s Full-mission Stokes Q posterior maximum
U_ML_FULL Real*4 K_RJ km/s Full-mission Stokes U posterior maximum
Q_ML_HM1 Real*4 K_RJ km/s First half-mission Stokes Q posterior maximum
U_ML_HM1 Real*4 K_RJ km/s First half-mission Stokes U posterior maximum
Q_ML_HM2 Real*4 K_RJ km/s Second half-mission Stokes Q posterior maximum
U_ML_HM2 Real*4 K_RJ km/s Second half-mission Stokes U posterior maximum
Q_ML_HR1 Real*4 K_RJ km/s First half-ring Stokes Q posterior maximum
U_ML_HR1 Real*4 K_RJ km/s First half-ring Stokes U posterior maximum
Q_ML_HR2 Real*4 K_RJ km/s Second half-ring Stokes Q posterior maximum
U_ML_HR2 Real*4 K_RJ km/s Second half-ring Stokes U posterior maximum
Q_ML_YR1 Real*4 K_RJ km/s "First year" Stokes Q posterior maximum
U_ML_YR1 Real*4 K_RJ km/s "First year" Stokes U posterior maximum
Q_ML_YR2 Real*4 K_RJ km/s "Second year" Stokes Q posterior maximum
U_ML_YR2 Real*4 K_RJ km/s "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

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[6]. Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.

Inputs

The following data have been fit:

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

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

Model Parameters

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[edit]

We describe diffuse foreground products for the Planck 2015 release produced with the GNILC component separation method. See the Planck paper Planck-2016-XLVIII[7] for a detailed discussion on these products.

Method[edit]

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

Data[edit]

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

Pre-processing[edit]

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

GNILC thermal dust and CIB products[edit]

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

Thermal dust maps[edit]

HDU -- COMP-MAP-DUST
File Name Nside Units Reference frequency Angular resolution Description
COM_CompMap_Dust-GNILC-F353_2048_R2.00.fits 2048 MJy/sr 353 GHz COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust amplitude at 353 GHz
COM_CompMap_Dust-GNILC-F545_2048_R2.00.fits 2048 MJy/sr 545 GHz COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust amplitude at 545 GHz
COM_CompMap_Dust-GNILC-F857_2048_R2.00.fits 2048 MJy/sr 857 GHz COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust amplitude at 857 GHz
COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.01.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_CompMap_Dust-GNILC-Radiance_2048_R2.00.fits 2048 W/m2/sr NA COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits Thermal dust radiance
COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits 128 Arcminute NA NA Effective dust beam FWHM

CIB maps[edit]

HDU -- COMP-MAP-CIB
File Name Nside Units Reference frequency Angular resolution Description
COM_CompMap_CIB-GNILC-F353_2048_R2.00.fits 2048 MJy/sr 353 GHz 5 arcmin CIB amplitude at 353 GHz
COM_CompMap_CIB-GNILC-F545_2048_R2.00.fits 2048 MJy/sr 545 GHz 5 arcmin CIB amplitude at 545 GHz
COM_CompMap_CIB-GNILC-F857_2048_R2.00.fits 2048 MJy/sr 857 GHz 5 arcmin CIB amplitude at 857 GHz


Other Special maps[edit]

Introduction[edit]

This section describes the map-based products that required special processing.


2015 Compton y parameter map[edit]

We distribute here the Planck full mission Compton parameter maps (y-maps hereafter) obtained using the NILC and MILCA component-separation algorithms as described in Planck-2015-A22[8]. We also provide the ILC weights per scale and per frequency that were used to produce these y-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 y-maps. Additionally we construct noise estimates of full mission Planck y-maps from the half difference of the FIRST and LAST y-maps. These estimates are used to construct standard deviation maps of the noise in the full mission Planck y-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.

Update 04 Aug 2017: 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.

Update 30 July 2018: 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.

The contents of the full data set are described below.

Contents of COM_CompMap_YSZ_R2.02.fits.tgz
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 y-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 y-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 y-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 y-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 y-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 y-map.
nilc_homnoise_spect.fits ASCII table FITS format Contains the angular power spectrum of the homogeneous noise in the NILC full mission y-map.
milca_homnoise_spect.fits ASCII table FITS format Contains the angular power spectrum of the homogeneous noise in the MILCA full mission y-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[edit]

We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in Planck-2015-A21[9] 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 Barreiro et al. 2008 and Bonavera et al. 2016.

These ISW maps, together with their corresponding uncertainties maps and masks, are given in a file named COM_CompMap_ISW_0064_R2.00.fits. Its contents are described below.


Contents of the ISW maps file: COM_CompMap_ISW_0064_R2.00.fits
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)[edit]

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 Planck-2015-A25[5]. 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 Planck-2015-A25[5]. 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 Planck-2015-A25[5].)

Astrophysical components based on the 2013 data release

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 the 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-2013-XII[10].

CMB maps


CMB maps have been produced by the SMICA, NILC, SEVEM and COMMANDER-Ruler pipelines. Of these, the SMICA product is considered the preferred one overall and is labelled Main product in the Planck Legacy Archive, while the other two are labeled as Additional product.

SMICA and NILC also produce inpainted maps, in which the Galactic Plane, some bright regions and masked point sources are replaced with a constrained CMB realization such that the whole map has the same statistical distribution as the observed CMB.

The results of SMICA, NILC and SEVEM pipeline are distributed as a FITS file containing 4 extensions:

  1. CMB maps and ancillary products (3 or 6 maps)
  2. CMB-cleaned foreground maps from LFI (3 maps)
  3. CMB-cleaned foreground maps from HFI (6 maps)
  4. Effective beam of the CMB maps (1 vector)

The results of COMMANDER-Ruler are distributed as two FITS files (the high and low resolution) containing the following extensions: High resolution N$_\rm{side}$=2048 (note that we don't provide the CMB-cleaned foregrounds maps for LFI and HFI because the Ruler resolution (~7.4') is lower than the HFI highest channel and and downgrading it will introduce noise correlation).

  1. CMB maps and ancillary products (4 maps)
  2. Effective beam of the CMB maps (1 vector)

Low resolution N$_\rm{side}$=256

  1. CMB maps and ancillary products (3 maps)
  2. 10 example CMB maps used in the montecarlo realization (10 maps)
  3. Effective beam of the CMB maps (1 vector)

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


The maps (CMB, noise, masks) contained in the first extension
Col name SMICA NILC SEVEM COMMANDER-Ruler H COMMANDER-Ruler L Description / notes
1: I CMB-smica.png CMB-nilc.png CMB-sevem.png CMB-CR h.png CMB-CR l.png Raw CMB anisotropy map. These are the maps used in the component separation paper Planck-2013-XII[10].
2: NOISE CMBnoise-smica.png CMBnoise-nilc.png CMBnoise-sevem.png CMBnoise-CR h.png not applicable Noise map. Obtained by propagating the half-ring noise through the CMB cleaning pipelines.
3: VALMASK Valmask-smica.png Valmask-nilc.png Valmask-sevem.png Valmask-cr h.png Valmask-cr l.png Confidence map. Pixels with an expected low level of foreground contamination. These maps are only indicative and obtained by different ad hoc methods. They cannot be used to rank the CMB maps.
4: I_MASK Cmbmask-smica.png Cmbmask-nilc.png not applicable not applicable not applicable Some areas are masked for the production of the raw CMB maps (for NILC: point sources from 44 GHz to 857 GHz; for SMICA: point sources from 30 GHz to 857 GHz, Galatic region and additional bright regions).
5: INP_CMB CMBinp-smica.png CMBinp-nilc.png not applicable not applicable not applicable Inpainted CMB map. The raw CMB maps with some regions (as indicated by INP_MASK) replaced by a constrained Gaussian realization. The inpainted SMICA map was used for PR.
6: INP_MASK Inpmask-smica.png Inpmask-nilc.png not applicable not applicable not applicable Mask of the inpainted regions. For SMICA, this is identical to I_MASK. For NILC, it is not.

The component separation pipelines are described in the CMB and foreground separation section and also in Section 3 and Appendices A-D of Planck-2013-XII[10] and references therein.

The union (or common) mask is defined as the union of the confidence masks from the four component separation pipelines, the three listed above and Commander-Ruler. It leaves 73% of the sky available, and so it is denoted as U73.


Product description

SMICA

Principle
SMICA produces a CMB map by linearly combining all Planck input channels (from 30 to 857 GHz) with weights which vary with the multipole. It includes multipoles up to [math]\ell = 4000[/math].
Resolution (effective beam)
The SMICA map has an effective beam window function of 5 arc-minutes truncated at [math]\ell=4000[/math] and deconvolved from the pixel window. It means that, ideally, one would have [math]C_\ell(map) = C_\ell(sky) * B_\ell(5')^2[/math], where [math]C_\ell(map)[/math] is the angular spectrum of the map, where [math]C_\ell(sky)[/math] is the angular spectrum of the CMB and [math]B_\ell(5')[/math] is a 5-arcminute Gaussian beam function. Note however that, by convention, the effective beam window function [math]B_\ell(fits)[/math] provided in the FITS file does include a pixel window function. Therefore, it is equal to [math]B_\ell(fits) = B_\ell(5') / p_\ell(2048)[/math] where [math]p_\ell(2048)[/math] denotes the pixel window function for an Nside=2048 pixelization.
Confidence mask
A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative (and subjective) indication of the cleanliness of a pixel.
Masks and inpainting
The raw SMICA CMB map has valid pixels except at the location of masked areas: point sources, Galactic plane, some other bright regions. Those invalid pixels are indicated with the mask named 'I_MASK'. The raw SMICA map has been inpainted, producing the map named "INP_CMB". Inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.

NILC

Principle
The Needlet-ILC (hereafter NILC) CMB map is constructed from all Planck channels from 44 to 857 GHz and includes multipoles up to [math]\ell = 3200[/math]. It is obtained by applying the Internal Linear Combination (ILC) technique in needlet space, that is, with combination weights which are allowed to vary over the sky and over the whole multipole range.
Resolution (effective beam)
As in the SMICA product except that there is no abrupt truncation at [math]\ell_{max}= 3200[/math] but a smooth transition to [math]0[/math] over the range [math]2700\leq\ell\leq 3200[/math].
Confidence mask
A confidence mask is provided which excludes some parts of the Galactic plane, some very bright areas and the masked point sources. This mask provides a qualitative indication of the cleanliness of a pixel. The threshold is somewhat arbitrary.
Masks and inpainting
The raw NILC map has valid pixels except at the location of masked point sources. This is indicated with the mask named 'I_MASK'. The raw NILC map has been inpainted, producing the map named "INP_CMB". The inpainting consists in replacing some pixels (as indicated by the mask named INP_MASK) by the values of a constrained Gaussian realization which is computed to ensure good statistical properties of the whole map (technically, the inpainted pixels are a sample realisation drawn under the posterior distribution given the un-masked pixels.

SEVEM

The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations[11] and to WMAP polarisation data[12]. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. Note that unlike the other products, SEVEM does not provide the mask of regions not used in the productions of the CMB ma (I_MASK) nor an inpainted version of the map and its associated mask. On the other hand, it provides channel maps and 100, 143, and 217 GHz which are used as the building blocks of the final map.

COMMANDER-Ruler

COMMANDER-Ruler is the Planck software implementing a pixel based parametric component separation. Amplitude of CMB and the main diffuse foregrounds along with the relevant spectral parameters for those (see below in the Astrophysical Foreground Section for the latter) are parametrized and fitted in single MCMC chains conducted at $N_\rm{side}$=256 using COMMANDER, implementing a Gibbs Sampling. The CMB amplitude which is obtained in these runs corresponds to the delivered low resolution CMB component from COMMANDER-Ruler which has a FWHM of 40 arcminutes. The sampling of the foreground parameters is applied to the data at full resolution for obtaining the high resolution CMB component from Ruler which is available on the PLA. In the Planck Component Separation paper[10] additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps. The products mainly consist of:

  • Maps of the Amplitudes of the CMB at low resolution, $N_\rm{side}$=256, along with the standard deviations of the outputs, beam profiles derived from the production process.
  • Maps of the CMB amplitude, along with the standard deviations, at high resolution, $N_\rm{side}$=2048, beam profiles derived from the production process.
  • Mask obtained on the basis of the precision in the fitting procedure; the thresholding is evaluated through the COMMANDER-Ruler likelihood analysis and excludes 13% of the sky, see Planck-2013-XII[10].

Production process

SMICA

1) Pre-processing
All input maps undergo a pre-processing step to deal with point sources. The point sources with SNR > 5 in the PCCS catalogue are fitted in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole is filled in by a simple diffusive process to ensure a smooth transition and mitigate spectral leakage. This is done at all frequencies but 545 and 857 GHz, here all point sources with SNR > 7.5 are masked and filled-in similarly.
2) Linear combination
The nine pre-processed Planck frequency channels from 30 to 857 GHzare harmonically transformed up to [math]\ell = 4000[/math] and co-added with multipole-dependent weights as shown in the figure.
3) Post-processing
The areas masked in the pre-processing step are replaced by a constrained Gaussian realization.

Note: The visible power deficit in the raw CMB map around the galactic plane is due to the smooth fill-in of the masked areas in the input maps (the result of the pre-processing). It is not to be confused with the post-processing step of inpainting of the CMB map with a constrained Gaussian realization.


Weights given by SMICA to the input maps (after they are re-beamed to 5 arcmin and expressed in K[math]_\rm{RJ}[/math]), as a function of multipole.

NILC

1) Pre-processing
Same pre-processing as SMICA (except the 30 GHz channel is not used).
2) Linear combination
The pre-processed Planck frequency channels from 44 to 857 GHz are linearly combined with weights which depend on location on the sky and on the multipole range up to [math]\ell = 3200[/math]. This is achieved using a needlet (redundant spherical wavelet) decomposition. For more details, see Planck-2013-XII[10].
3) Post-processing
The areas masked in the pre-processing plus other bright regions step are replaced by a constrained Gaussian realization as in the SMICA post-processing step.

SEVEM

The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization[13]) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.

We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates [math]t_j[/math] is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky: [math] T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x}) [/math] where [math]n_t[/math] is the number of templates. If the cleaning is performed in real space, the [math]α_j[/math] coefficients are obtained by minimising the variance of the clean map [math]T_c[/math] outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).

An additional level of flexibility can also be considered: the linear coefficients can be the same for all the sky, or several regions with different sets of coefficients can be considered. The regions are then combined in a smooth way, by weighting the pixels at the boundaries, to avoid discontinuities in the clean maps. Since the method is linear, we may easily propagate the noise properties to the final CMB map. Moreover, it is very fast and permits the generation of thousands of simulations to character- ize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.

There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.

In particular, we have cleaned the 143 GHz and 217 GHz maps using four templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and (857-545). For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). In order to take into account the different spectral behaviour of the foregrounds at low and high galactic latitudes, we have considered two independent regions of the sky, for which we have used a different set of coefficients. The first region corresponds to the 3 per cent brightest Galactic emission, whereas the second region is defined by the remaining 97 per cent of the sky. For the first region, the coefficients are actually estimated over the whole sky (we find that this is more optimal than perform the minimisation only on the 3 per cent brightest region, where the CMB emission is very sub-dominant) while for the second region, we exclude the 3 per cent brightest region of the sky, point sources detected at any frequency and those pixels which have not been observed at all channels. Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.

Moreover, additional CMB clean maps (at frequencies between 44 and 353 GHz) have also been produced using different combinations of templates for some of the analyses carried out in Planck-2013-XXIII[14] and Planck-2013-XIX[15]. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in Planck-2013-XIX[15], while frequencies from 70 to 217 GHz were used for consistency tests in Planck-2013-XXIII[14].

COMMANDER-Ruler

The production process consist in low and high resolution runs according to the description above.

Low Resolution Runs
Same as the Astrophysics Foregrounds Section below; The CMB amplitude is fitted along with the other foreground parameters and constitutes the CMB Low Resolution Rendering which is in the PLA.
Ruler Runs
the sampling at high resolution is used to infer the probability distribution of spectral parameters which is exploited at full resolution in order to obtain the High Resolution CMB Rendering which is in the PLA.

Masks

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 CMB maps.

Commander 2013 (PR1) Used for diffuse inpainting of input frequency maps Used for constrained Gaussian realization inpaiting of CMB map Description
VALMASK NO NO VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside

COM_CompMap_CMB-commrul_2048_R1.00.fits and COM_CompMap_CMB-commrul_0256_R1.00.fits for low resolution analyses.

SEVEM 2013 (PR1) Used diffuse inpainting of input frequency maps Used for Constrained Gaussian realization inpaiting of CMB map Description
VALMASK NO NO VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside

COM_CompMap_CMB-sevem_2048_R1.12.fits.

NILC 2013 (PR1) Used for diffuse inpainting of input frequency maps Used for constrained Gaussian realization inpaiting of CMB map Description
VALMASK NO NO VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside COM_CompMap_CMB-nilc_2048_R1.20.fits.
I_MASK NO NO I_MASK defines the regions over which CMB is not built. It is a combination of point source masks, Galactic plane mask and other bright regions like LMC, SMC, etc. It can be found inside COM_CompMap_CMB-nilc_2048_R1.20.fits.
INP_MASK NO YES It can be found inside COM_CompMap_CMB-nilc_2048_R1.20.fits.
SMICA 2013 (PR1) Used for diffuse inpainting of input frequency maps Used for constrained Gaussian realization inpaiting of CMB map Description
VALMASK NO NO VALMASK is the confidence mask that defines the region where the reconstructed CMB is trusted. It can be found inside

COM_CompMap_CMB-smica_2048_R1.20.fits.

I_MASK YES YES I_MASK defines the regions over which CMB is not built. It is a combination of point source masks, Galactic plane mask and other bright regions like LMC, SMC, etc. It can be found inside COM_CompMap_CMB-smica_2048_R1.20.fits.
INP_MASK YES YES INP_MASK for SMICA 2013 release is identical to I_MASK above.


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

The FITS files corresponding to the three CMB products are the following:


The files contain a minimal primary extension with no data and four BINTABLE data extensions. Each column of the BINTABLE is a (Healpix) map; the column names and the most important keywords of each extension are described in the table below; for the remaining keywords, please see the FITS files directly.


CMB map file data structure
Ext. 1. EXTNAME = COMP-MAP (BINTABLE)
Column Name Data Type Units Description
I Real*4 uK_cmb CMB temperature map
NOISE Real*4 uK_cmb Estimated noise map (note 1)
I_STDEV Real*4 uK_cmb Standard deviation, ONLY on COMMANDER-Ruler products
VALMASK Byte none Confidence mask (note 2)
I_MASK Byte none Mask of regions over which CMB map is not built (Optional - see note 3)
INP_CMB Real*4 uK_cmb Inpainted CMB temperature map (Optional - see note 3)
INP_MASK Byte none mask of inpainted pixels (Optional - see note 3)
Keyword Data Type Value Description
AST-COMP String CMB Astrophysical compoment name
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
ORDERING String NESTED Healpix ordering
NSIDE Int 2048 Healpix Nside
METHOD String name Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
Ext. 2. EXTNAME = FGDS-LFI (BINTABLE) - Note 4
Column Name Data Type Units Description
LFI_030 Real*4 K_cmb 30 GHz foregrounds
LFI_044 Real*4 K_cmb 44 GHz foregrounds
LFI_070 Real*4 K_cmb 70 GHz foregrounds
Keyword Data Type Value Description
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
ORDERING String NESTED Healpix ordering
NSIDE Int 1024 Healpix Nside
METHOD String name Cleaning method (SMICA/NILC/SEVEM)
Ext. 3. EXTNAME = FGDS-HFI (BINTABLE) - Note 4
Column Name Data Type Units Description
HFI_100 Real*4 K_cmb 100 GHz foregrounds
HFI_143 Real*4 K_cmb 143 GHz foregrounds
HFI_217 Real*4 K_cmb 217 GHz foregrounds
HFI_353 Real*4 K_cmb 353 GHz foregrounds
HFI_545 Real*4 MJy/sr 545 GHz foregrounds
HFI_857 Real*4 MJy/sr 857 GHz foregrounds
Keyword Data Type Value Description
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
ORDERING String NESTED Healpix ordering
NSIDE Int 2048 Healpix Nside
METHOD String name Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
Ext. 4. EXTNAME = BEAM_WF (BINTABLE)
Column Name Data Type Units Description
BEAM_WF Real*4 none The effective beam window function, including the pixel window function. See Note 5.
Keyword Data Type Value Description
LMIN Int value First multipole of beam WF
LMAX Int value Lsst multipole of beam WF
METHOD String name Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)

Notes:

  1. The half-ring half-difference (HRHD) map is made by passing the half-ring frequency maps independently through the component separation pipeline, then computing half their difference. It approximates a noise realisation, and gives an indication of the uncertainties due to instrumental noise in the corresponding CMB map.
  2. The confidence mask indicates where the CMB map is considered valid.
  3. This column is not present in the SEVEM and COMMANDER-Ruler product file. For SEVEM these three columns give the CMB channel maps at 100, 143, and 217 GHz (columns C100, C143, and C217, in units of K_cmb.
  4. The subtraction of the CMB from the sky maps in order to produce the foregrounds map is done after convolving the CMB map to the resolution of the given frequency. Those columns are not present in the COMMANDER-Ruler product file.
  5. The beam window function [math]B_\ell[/math] given here includes the pixel window function [math]p_\ell[/math] for the Nside=2048 pixelization. It means that, ideally, [math]C_\ell(map) = C_\ell(sky) \, B_\ell^2 \, p_\ell^2[/math].

The low resolution COMMANDER-Ruler CMB product is organized in the following way:

CMB low resolution COMMANDER-Ruler map file data structure
Ext. 1. EXTNAME = COMP-MAP (BINTABLE)
Column Name Data Type Units Description
I Real*4 uK_cmb CMB temperature map obtained as average over 1000 samples
I_stdev Real*4 uK_cmb Corresponding Standard deviation amongst the 1000 samples
VALMASK Byte none Confidence mask
Keyword Data Type Value Description
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
ORDERING String NESTED Healpix ordering
NSIDE Int 2048 Healpix Nside
METHOD String name Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
Ext. 2. EXTNAME = CMB-Sample (BINTABLE)
Column Name Data Type Units Description
I_SIM01 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM02 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM03 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM04 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM05 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM06 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM07 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM08 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM09 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
I_SIM10 Real*4 K_cmb CMB Sample, smoothed to 40 arcmin
Keyword Data Type Value Description
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
ORDERING String NESTED Healpix ordering
NSIDE Int 1024 Healpix Nside
METHOD String name Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)
Ext. 4. EXTNAME = BEAM_WF (BINTABLE)
Column Name Data Type Units Description
BEAM_WF Real*4 none The effective beam window function, including the pixel window function.
Keyword Data Type Value Description
LMIN Int value First multipole of beam WF
LMAX Int value Lsst multipole of beam WF
METHOD String name Cleaning method (SMICA/NILC/SEVEM/COMMANDER-Ruler)


The FITS files containing the union (or common) maks is:

which contains a single BINTABLE extension with a single column (named U73) for the mask, which is boolean (FITS TFORM = B), in GALACTIC coordinates, NESTED ordering, and Nside=2048.

For the benefit of users who are only looking for a small file containing the SMICA cmb map with no additional information (noise or masks) we provide such a file here

This file contains a single extension with a single column containing the SMICA cmb temperature map.

Cautionary notes

  1. The half-ring CMB maps are produced by the pipelines with parameters/weights fixed to the values obtained from the full maps. Therefore the CMB HRHD maps do not capture all of the uncertainties due to foreground modelling on large angular scales.
  2. The HRHD maps for the HFI frequency channels underestimate the noise power spectrum at high l by typically a few percent. This is caused by correlations induced in the pre-processing to remove cosmic ray hits. The CMB is mostly constrained by the HFI channels at high l, and so the CMB HRHD maps will inherit this deficiency in power.
  3. The beam transfer functions do not account for uncertainties in the beams of the frequency channel maps.

Astrophysical foregrounds from parametric component separation


We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper Planck-2013-XII[10] for a detailed description and astrophysical discussion of those.

Product description

Low frequency foreground component
The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.
Thermal dust
The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided.
Sky mask
The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.

Production process

CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper Planck-2013-XII[10] additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.

Inputs

Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz (LFI 30 GHz frequency maps, LFI 44 GHz frequency maps and LFI 70 GHz frequency maps, HFI 100 GHz frequency maps, HFI 143 GHz frequency maps,HFI 217 GHz frequency maps and HFI 353 GHz frequency maps) and their II column corresponding to the noise covariance matrix. Halfrings at the same frequencies. Beam window functions as reported in the LFI and HFI RIMO.

Related products

None.

File names

Meta Data

Low frequency foreground component

Low frequency component at N$_\rm{side}$ = 256

File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits

Name HDU -- COMP-MAP

The Fits extension is composed by the columns described below:

FITS header
Column Name Data Type Units Description
I Real*4 uK[math]_{CMB}[/math] Intensity
I_stdev Real*4 uK[math]_{CMB}[/math] standard deviation of intensity
Beta Real*4 effective spectral index
B_stdev Real*4 standard deviation on the effective spectral index
Notes
Comment: The Intensity is normalized at 30 GHz
Comment: The intensity was estimated during mixing matrix estimation

Low frequency component at N$_\rm{side}$ = 2048

File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits


Name HDU -- COMP-MAP

The Fits extension is composed by the columns described below:

FITS header
Column Name Data Type Units Description
I Real*8 uK[math]_{CMB}[/math] Intensity
I_stdev Real*8 uK[math]_{CMB}[/math] standard deviation of intensity
I_hr1 Real*8 uK[math]_{CMB}[/math] Intensity on half ring 1
I_hr2 Real*8 uK[math]_{CMB}[/math] Intensity on half ring 2
Notes
Comment: The intensity was computed after mixing matrix application


Name HDU -- BeamWF

The Fits second extension is composed by the columns described below:

FITS header
Column Name Data Type Units Description
BeamWF Real*4 beam profile
Notes
Comment: Beam window function used in the Component separation process

Thermal dust

Thermal dust component at N$_\rm{side}$=256

File name: COM_CompMap_dust-commrul_0256_R1.00.fits
Name HDU -- COMP-MAP

The Fits extension is composed by the columns described below:

FITS header
Column Name Data Type Units Description
I Real*4 MJy/sr Intensity
I_stdev Real*4 MJy/sr standard deviation of intensity
Em Real*4 emissivity
Em_stdev Real*4 standard deviation on emissivity
T Real*4 uK[math]_{CMB}[/math] temperature
T_stdev Real*4 uK[math]_{CMB}[/math] standard deviation on temerature
Notes
Comment: The intensity is normalized at 353 GHz

Thermal dust component at N$_\rm{side}$=2048

File name: COM_CompMap_dust-commrul_2048_R1.00.fits


Name HDU -- COMP-MAP

The Fits extension is composed by the columns described below:

FITS header
Column Name Data Type Units Description
I Real*8 MJy/sr Intensity
I_stdev Real*8 MJy/sr standard deviation of intensity
I_hr1 Real*8 MJy/sr Intensity on half ring 1
I_hr2 Real*8 MJy/sr Intensity on half ring 2


Name HDU -- BeamWF

The Fits second extension is composed by the columns described below:

FITS header
Column Name Data Type Units Description
BeamWF Real*4 beam profile
Notes
Comment: Beam window function used in the Component separation process

Sky mask

File name: COM_CompMap_Mask-rulerminimal_2048.fits

Name HDU -- COMP-MASK

The Fits extension is composed by the columns described below:

FITS header
Column Name Data Type Units Description
Mask Real*4 Mask

Thermal dust emission


Thermal emission from interstellar dust is captured by Planck-HFI over the whole sky, at all frequencies from 100 to 857 GHz. This emission is well modelled by a modified black body in the far-infrared to millimeter range. It is produced by the biggest interstellar dust grain that are in thermal equilibrium with the radiation field from stars. The grains emission properties in the sub-millimeter are therefore directly linked to their absorption properties in the UV-visible range. By modelling the thermal dust emission in the sub-millimeter, a map of dust reddening in the visible can then be constructed. The details of the model can be found here Planck-2013-XI[16].

Model of all-sky thermal dust emission

The model of the thermal dust emission is based on a modified black body (MBB) fit to the data [math]I_\nu[/math]

[math]I_\nu = A\, B_\nu(T)\, \nu^\beta[/math]

where [math]B_\nu(T)[/math] is the Planck function for dust equilibirum temperature [math]T[/math], [math]A[/math] is the amplitude of the MBB and [math]\beta[/math] the dust spectral index. The dust optical depth at frequency [math]\nu[/math] is

[math]\tau_\nu = I_\nu / B_\nu(T) = A\, \nu^\beta[/math]

The dust parameters provided are [math]T[/math], [math]\beta[/math] and [math]\tau_{353}[/math]. They were obtained by fitting the Planck data at 353, 545 and 857 GHz (from which the Planck zodiacal light model was removed) together with the IRAS 100 micron data. The latter is a combination of the 100 micron maps from IRIS (Miville-Deschenes & Lagache, 2005) and from Schlegel et al. (1998), SFD1998. The IRIS (SFD1998) map is used at scales smaller (larger) than 30 arcmin; this combination allows to take advantage of the higher angular resolution and better control of gain variations of the IRIS map and of the better removal of the zodiacal light emission of the SFD1998 map.

All maps (in Healpix Nside=2048 were smoothed to a common resolution of 5 arcmin. The CMB anisotropies, clearly visible at 353 GHz, were removed from all the HFI maps using the SMICA map. An offset was removed from each map to set a Galactic zero level, using a correlation with the LAB 21 cm data in diffuse areas of the sky ([math]N_{HI} \lt 2\times10^{20} cm^{-2}[/math]). Because the dust emission is so well correlated between frequencies in the Rayleigh-Jeans part of the dust spectrum, the zero level of the 545 and 353 GHz were improved by correlating with the 857 GHz over a larger mask ([math]N_{HI} \lt 3\times10^{20} cm^{-2}[/math]). Faint residual dipole structures, identified in the 353 and 545 GHz maps, were removed prior to the fit.

The MBB fit was performed using a [math]\chi^2[/math] minimization method, assuming errors for each data point that include instrumental noise, calibration uncertainties (on both the dust emission and the CMB anisotropies) and uncertainties on the zero levels. Because of the known degeneracy between [math]T[/math] and [math]\beta[/math] in the presence of noise, we performed tge fit in two steps. First we produced a model of dust emission using data smoothed to 30 arcmin; at such resolution no systematic bias of the parameters is observed. In a second step the map of the spectral index [math]\beta[/math] at 30 arcmin was used to fit the data for [math]T[/math] and [math]\tau_{353}[/math] at 5 arcmin.

The [math]E(B-V)[/math] map for extra-galactic studies For the production of the [math]E(B-V)[/math] map, we used a MBB fit to Planck and IRAS data from which point sources were removed to avoid contamination by galaxies. In the hypothesis of constant dust emission cross-section, the optical depth map [math]\tau_{353}[/math] is proportional to dust column density and therefore often used to estimate E(B-V). The analysis of Planck data revealed that the ratio [math]\tau_{353}/N_{HI}[/math] and [math]\tau_{353}/E(B-V)[/math] are not constant, even in the diffuse ISM, but that they depend on [math]T[/math] revealing possible spatial variations of the dust emission cross-section. It appears that the dust radiance, [math]R[/math], i.e. the dust emission integrated in frequency, is a better tracer of column density in the diffuse ISM, implying small spatial variations of the radiation field strength at high Galactic latitude. Given those results, we also deliver the map of [math]R[/math] as a dust product and we propose to use it as an estimator of Galactic dust reddening for extra-galactic studies: [math]E(B-V) = q\, R[/math].

To estimate the calibration factor q, we followed a method similar to[17] based on SDSS reddening measurements of quasars in the u, g, r, i and z bands[18]. We used a sample of 53 399 quasars, selecting objects at redshifts for which Ly[math]\alpha[/math] does not enter the SDSS filters. The interstellar HI column densities covered on the lines of sight of this sample ranges from [math]0.5[/math] to [math]10\times10^{20}\,cm^{-2}[/math]. Therefore this sample allows us to estimate q in the diffuse ISM where this map of E(B-V) is intended to be used.

Dust optical depth products The dust model maps are found in the file HFI_CompMap_ThermalDustModel_2048_R1.20.fits (see the note below for an important clarification regarding the thermal dust model); its characteristics are:

  • Dust optical depth at 353 GHz: Nside=2048, fwhm=5', no units
  • Dust temperature: Nside 2048, fwhm=5', units=Kelvin
  • Dust spectral index: Nside=2048, fwhm=30', no units
  • Dust radiance: Nside=2048, fwhm=5', units=Wm-2sr-1
  • E(B-V) for extragalactic studies: Nside=2048, fwhm=5', units=magnitude, obtained with data from which point sources were removed.


Dust opacity file data structure
1. EXTNAME = 'COMP-MAP'
Column Name Data Type Units Description
TAU353 Real*4 none The optical depth at 353GHz
ERR_TAU Real*4 none Error on the optical depth
EBV Real*4 mag E(B-V) for extra-galactic studies
RADIANCE Real*4 Wm-2sr-1 Integrated emission
TEMP Real*4 K Dust temperature
ERR_TEMP Real*4 K Error on the temperature
BETA Real*4 none Dust spectral index
ERR_BETA Real*4 none Error on Beta
Keyword Data Type Value Description
AST-COMP String DUST Astrophysical compoment name
PIXTYPE String HEALPIX
COORDSYS String GALACTIC Coordinate system
ORDERING String NESTED Healpix ordering
NSIDE Int 2048 Healpix Nside for LFI and HFI, respectively
FIRSTPIX Int*4 0 First pixel number
LASTPIX Int*4 50331647 Last pixel number, for LFI and HFI, respectively


IMPORTANT NOTE: The dust model has recently (4 December 2013) been updated and the new model is the one being distributed by default. A detailed description of the model can be found here Planck-2013-XI[16]. Users interested in the old dust model map should contact the PLA help desk.

CO emission maps


CO rotational transition line emission is present in all HFI bands but for the 143 GHz channel. It is especially significant in the 100, 217 and 353 GHz channels (due to the 115 (1-0), 230 (2-1) and 345 GHz (3-2) CO transitions). This emission comes essentially from the Galactic interstellar medium and is mainly located at low and intermediate Galactic latitudes. Three approaches (summarised below) have been used to extract CO velocity-integrated emission maps from HFI maps and to make three types of CO products. A full description of how these products were produced is given in Planck-2013-XIII[19].

  • Type 1 product: it is based on a single channel approach using the fact that each CO line has a slightly different transmission in each bolometer at a given frequency channel. These transmissions can be evaluated from bandpass measurements that were performed on the ground or empirically determined from the sky using existing ground-based CO surveys. From these, the J=1-0, J=2-1 and J=3-2 CO lines can be extracted independently. As this approach is based on individual bolometer maps of a single channel, the resulting Signal-to-Noise ratio (SNR) is relatively low. The benefit, however, is that these maps do not suffer from contamination from other HFI channels (as is the case for the other approaches) and are more reliable, especially in the Galactic Plane.
  • Type 2 product: this product is obtained using a multi frequency approach. Three frequency channel maps are combined to extract the J=1-0 (using the 100, 143 and 353 GHz channels) and J=2-1 (using the 143, 217 and 353 GHz channels) CO maps. Because frequency channels are combined, the spectral behaviour of other foregrounds influences the result. The two type 2 CO maps produced in this way have a higher SNR than the type 1 maps at the cost of a larger possible residual contamination from other diffuse foregrounds.
  • Type 3 product: using prior information on CO line ratios and a multi-frequency component separation method, we construct a combined CO emission map with the largest possible SNR. This type 3 product can be used as a sensitive finder chart for low-intensity diffuse CO emission over the whole sky.

The released Type 1 CO maps have been produced using the MILCA-b algorithm, Type 2 maps using a specific implementation of the Commander algorithm, and the Type 3 map using the full Commander-Ruler component separation pipeline (see above).

Characteristics of the released maps are the following. We provide Healpix maps with Nside=2048. For one transition, the CO velocity-integrated line signal map is given in K_RJ.km/s units. A conversion factor from this unit to the native unit of HFI maps (K_CMB) is provided in the header of the data files and in the RIMO. Four maps are given per transition and per type:

  • The signal map
  • The standard deviation map (same unit as the signal),
  • A null test noise map (same unit as the signal) with similar statistical properties. It is made out of half the difference of half-ring maps.
  • A mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.

All products of a given type belong to a single file. Type 1 products have the native HFI resolution i.e. approximately 10, 5 and 5 arcminutes for the CO 1-0, 2-1, 3-2 transitions respectively. Type 2 products have a 15 arcminute resolution The Type 3 product has a 5.5 arcminute resolution.


Type-1 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
I32 Real*4 K_RJ km/sec The CO(3-2) intensity map
E32 Real*4 K_RJ km/sec Uncertainty in the CO(3-2) intensity
N32 Real*4 K_RJ km/sec Map built from the half-ring difference maps
M32 Byte none Region over which the CO(3-2) 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 and HFI, respectively
FIRSTPIX Int*4 0 First pixel number
LASTPIX Int*4 50331647 Last pixel number, for LFI and HFI, 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))


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 and HFI, respectively
FIRSTPIX Int*4 0 First pixel number
LASTPIX Int*4 50331647 Last pixel number, for LFI and HFI, 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))


Type-3 CO map file data structure
1. EXTNAME = 'COMP-MAP'
Column Name Data Type Units Description
INTEN Real*4 K_RJ km/sec The CO intensity map
ERR Real*4 K_RJ km/sec Uncertainty in the intensity
NUL Real*4 K_RJ km/sec Map built from the half-ring difference maps
MASK Byte none Region over which the 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 and HFI, respectively
FIRSTPIX Int*4 0 First pixel number
LASTPIX Int*4 50331647 Last pixel number, for LFI and HFI, respectively
CNV Real*4 value Factor to convert to Kcmb (units Kcmb/(Krj*km/s))


References[edit]

  1. ↑ 1.01.1 Planck 2018 results. IV. Diffuse component separation, Planck Collaboration, 2020, A&A, 641, A4.
  2. ↑ Planck 2018 results. VIII. Lensing, Planck Collaboration, 2020, A&A, 641, A8.
  3. ↑ Planck 2018 results. III. High Frequency Instrument data processing and frequency maps, Planck Collaboration, 2020, A&A, 641, A3.
  4. ↑ 4.04.14.2 Planck 2015 results. X. Diffuse component separation: Foreground maps, Planck Collaboration, 2016, A&A, 594, A10.
  5. ↑ 5.05.15.25.3 Planck 2015 results. XXV. Diffuse low frequency Galactic foregrounds, Planck Collaboration, 2016, A&A, 594, A25.
  6. ↑ Planck intermediate results. XXIX. All-sky dust modelling with Planck, IRAS, and WISE observations', Planck Collaboration Int. XXIX, A&A, 586, A132, (2016).
  7. ↑ Planck intermediate results. XLVIII. Disentangling Galactic dust emission and cosmic infrared background anisotropies, Planck Collaboration Int. XLVIII A&A, 596, A109, (2016).
  8. ↑ Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect, Planck Collaboration, 2016, A&A, 594, A22.
  9. ↑ Planck 2015 results. XXI. The integrated Sachs-Wolfe effect, Planck Collaboration, 2016, A&A, 594, A21.
  10. ↑ 10.010.110.210.310.410.510.610.7 Planck 2013 results. XI. Component separation, Planck Collaboration, 2014, A&A, 571, A11.
  11. ↑ 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. ↑ 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. ↑ 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. ↑ 14.014.1 Planck 2013 results. XXIII. Isotropy and statistics of the CMB, Planck Collaboration, 2014, A&A, 571, A23.
  15. ↑ 15.015.1 Planck 2013 results. XIX. The integrated Sachs-Wolfe effect, Planck Collaboration, 2014, A&A, 571, A19.
  16. ↑ 16.016.1 Planck 2013 results. XII. All-sky model of thermal dust emission, Planck Collaboration, 2014, A&A, 571, A12.
  17. ↑ Calibrating Milky Way dust extinction using cosmological sources, E. Mörtsell, A&A, 550, A80, (2013).
  18. ↑ 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. ↑ 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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