Foreground maps

From Planck Legacy Archive Wiki
Revision as of 18:39, 11 July 2018 by Jcarron (talk | contribs) (2018 Lensing band powers and likelihoods)
Jump to: navigation, search

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_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 = 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

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

2018 Lensing products[edit]

2018 Lensing maps[edit]

We distribute several variations of lensing potential estimates presented in Planck-2020-A8[2] as part of the 2018 data release, together with matching simulation packages.

There are 4 lensing data packages:

  • COM_Lensing_4096_R3.00
Baseline lensing potential estimates from SMICA DX12 CMB maps. Provided are temperature-only (TT), polarization-only (PP) and minimum-variance (MV) estimates.
  • 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. 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:

Contents of lensing data package COM_Lensing_4096_R3.00
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 Planck-2020-A8[2].
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 Planck-2020-A8[2]..
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 Planck-2020-A8[2].

with slight variations:

- in COM_Lensing_Inhf_2048_R3.00, all HEALPix FITS format alm files have [math]L_{\rm max}=2048[/math].
- COM_Lensing-Szdeproj_4096_R3.00 only provides the temperature-only reconstruction.

The matching 4 lensing simulation packages are

  • COM_Lensing-SimMap_4096_R3.00
  • 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:

Contents of lensing simulation package COM_Lensing-SimMap_4096_R3.00
Filenames Format Description
/inputs/mask.fits.gz compressed HEALPix FITS format map, with [math]N_{\rm side}=2048[/math] Lens reconstruction analysis mask.
/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 Planck-2020-A8[2].
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 Planck-2020-A8[2].
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 Planck-2020-A8[2].
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 Planck-2020-A8[2].
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).
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 Planck-2020-A8[2].
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 Planck-2020-A8[2].
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 Planck-2020-A8[2].

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].
- COM_Lensing-SimMap-Szdeproj_4096_R3.00 only provides the temperature-only reconstructions.

We further provide the input lensing convergence realizations of all 300 FFP10 simulations in

  • COM_Lensing-SimMap-inputs_4096_R3.00

with contents

Contents of lensing simulation package COM_Lensing-SimMap-inputs_4096_R3.00
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 Planck-2020-A8[2].
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 Planck-2020-A8[2].

2018 Lensing-induced B-mode maps[edit]

We distribute maps of the lensing-induced B-modes presented in Planck-2020-A8[2], together with a matching simulation suite. The Stokes parameter maps of the lensing B-modes are produced by combining tracers of lensing potential with E-mode data from the SMICA CMB polarization maps. These lensing-induced B-mode polarization maps are provided on approximately 60% of the sky. Planck-2020-A8[2] details the construction of these maps.

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.

These maps are filtered template of the lensing B-mode (both the lensing tracer and [math]E[/math]-mode used to build the B template are Wiener-filtered). The simulation suite may be used to assess the filter, as was done in Planck-2020-A8[2] to produce the B-mode power spectrum (Fig. 14).

The B-mode template package is

  • COM_Lensing-Bmode_2048_R3.00

with contents

Contents of B-mode template data package COM_Lensing-Bmode_2048_R3.00
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 Planck-2020-A8[2].
/inputs/clbb.dat ASCII text file, with columns = ([math]\ell[/math], [math]C_\ell^{BB}[/math]) Input lensing [math]B[/math]-mode power spectrum for the fiducial cosmology used in Planck-2020-A8[2].
dat_blm_TTTEETEE.fits HEALPix FITS format alm, with [math]\ell_{\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.
dat_blm_545_TTTEETEE.fits HEALPix FITS format alm, with [math]\ell_{\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.

The B-mode template simulation package is

  • COM_Lensing-SimMap-Bmode_2048_R3.00

with contents

Contents of B-mode template simulation package COM_Lensing-SimMap-Bmode_2048_R3.00
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 Planck-2020-A8[2].
/inputs/clbb.dat ASCII text file, with columns = ([math]\ell[/math], [math]C_\ell^{BB}[/math]) Input lensing [math]B[/math]-mode power spectrum for the fiducial cosmology used in Planck-2020-A8[2].
/TTTEETE/blm_{???}.fits 300 HEALPix FITS format alm, with [math]\ell_{\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 Planck-2020-A8[2].
/545_TTTEETE/blm_{???}.fits 300 HEALPix FITS format alm, with [math]\ell_{\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 Planck-2020-A8[2].
/TTTEETE/dat_blm.fits HEALPix FITS format alm, with [math]\ell_{\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]\ell_{\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[edit]

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 Planck-2020-A8[2]. The maps are built on about 60% of the sky.

The tracer are Wiener-filtered estimates of the convergence [math]\hat \kappa_{LM} = \frac 12 L (L + 1) \hat \phi_{LM}[/math].

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.

The lensing combined tracer data package is

  • COM_Lensing-CIBcomb_2000_R3.00

with contents

Contents of lensing combined tracer data package COM_Lensing-CIBcomb_2000_R3.00
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 Planck-2020-A8[2].
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).
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).

The lensing combined tracer simulation package is

  • COM_Lensing-SimMap-CIBcomb_2000_R3.00

with contents

Contents of lensing combined tracer simulation package COM_Lensing-SimMap-CIBcomb_2000_R3.00
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 Planck-2020-A8[2].
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 Planck-2020-A8[2].
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 Planck-2020-A8[2].
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).
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 Planck-2020-A8[2]). 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].

Mollveide projection of the minimum variance quadratic estimator lensing map:

  • Lensing_2018_MV_alphaA0_YlGnBu_300dpi_47in_moll.png

Orthographic projection of the minimum variance quadratic estimatorlensing map:

  • Lensing_2018_compMV_alphaA0_YlGnBu_300dpi_47in_moll.png

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

2018 Lensing band powers and likelihoods[edit]

The lensing reconstruction spectrum band powers, covariance matrix and likelihood linear corrections are provided as a zip of a series of ASCII files

  • planck_lensing_2018.zip

The files are in CosmoMC format, a piece of software available here. A new Python code called Cobaya which follows the same methodology will be soon available and should produce the same results.

We provide CosmoMC files for 8 different likelihoods

  • smicadx12_Dec5_ftl_mv2_ndclpttptt_p_teb_consext8
  • smicadx12_Dec5_ftl_mv2_ndclpttptt_p_teb_consext8_CMBmarged
  • smicadx12_Dec5_ftl_mv2_ndclpttptt_p_teb_agr2
  • smicadx12_Dec5_ftl_mv2_ndclpttptt_p_teb_agr2_CMBmarged
  • smicadx12_Dec5_ftl_mv2_ndclpp_p_teb_consext8
  • smicadx12_Dec5_ftl_mv2_ndclpp_p_teb_consext8_CMBmarged
  • smicadx12_Dec5_ftl_mv2_ndclpp_p_teb_agr2
  • smicadx12_Dec5_ftl_mv2_ndclpp_p_teb_agr2_CMBmarged

following these variations:

  • Reconstructions from temperature-only ('pttptt_p_teb') or minimum-variance ('pp_p_teb') combination of temperature and polarization
  • Conservative ('consext8') [math]( 8 \leq L \leq 400 )[/math] or aggressive ('agr2') [math]( 8 \leq L \leq 2048 )[/math] lensing multipole range.
  • Likelihood with ('CMBmarged', used for lensing-only constraints) and without CMB marginalization.

The band powers and likelihood construction, together with detailed consistency and robustness tests are provided in Planck-2020-A8[2]. The aggressive range is considered less reliable than the conservative range.

Lensing-only MCMC chains used for this release are available here. Follow this link for joint constraints and parameter tables.

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

Expand

Astrophysical components based on the 2015 data release

Expand

Astrophysical components based on the 2013 data release

References[edit]

  1. Jump up to: 1.01.1 Planck 2018 results. IV. Diffuse component separation, Planck Collaboration, 2020, A&A, 641, A4.
  2. Jump up to: 2.002.012.022.032.042.052.062.072.082.092.102.112.122.132.142.152.162.172.182.192.202.212.222.232.242.252.262.272.282.29 Planck 2018 results. VIII. Lensing, Planck Collaboration, 2020, A&A, 641, A8.
  3. Jump up Planck 2018 results. III. High Frequency Instrument data processing and frequency maps, Planck Collaboration, 2020, A&A, 641, A3.
  4. Jump up to: 4.04.14.2 Planck 2015 results. X. Diffuse component separation: Foreground maps, Planck Collaboration, 2016, A&A, 594, A10.
  5. Jump up to: 5.05.15.25.3 Planck 2015 results. XXV. Diffuse low frequency Galactic foregrounds, Planck Collaboration, 2016, A&A, 594, A25.
  6. Jump up Planck intermediate results. XXIX. All-sky dust modelling with Planck, IRAS, and WISE observations', Planck Collaboration Int. XXIX, A&A, 586, A132, (2016).
  7. Jump up Planck 2015 results. XV. Gravitational Lensing, Planck Collaboration, 2016, A&A, 594, A15.
  8. Jump up to: 8.08.1 Planck 2015 results. XI. Diffuse component separation: CMB maps, Planck Collaboration, 2016, A&A, 594, A9.
  9. Jump up Planck 2015 results. XIII. Cosmological parameters, Planck Collaboration, 2016, A&A, 594, A13.
  10. Jump up Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect, Planck Collaboration, 2016, A&A, 594, A22.
  11. Jump up to: 11.011.111.211.311.411.511.611.7 Planck intermediate results. XLI. A map of lensing-induced B-modes, Planck Collaboration Int. XLI A&A, 596, A102, (2016).
  12. Jump up Planck 2015 results. XXI. The integrated Sachs-Wolfe effect, Planck Collaboration, 2016, A&A, 594, A21.
  13. Jump up to: 13.013.113.213.313.413.513.613.7 Planck 2013 results. XI. Component separation, Planck Collaboration, 2014, A&A, 571, A11.
  14. Jump up Component separation methods for the PLANCK mission, S. M. Leach, J.-F. Cardoso, C. Baccigalupi, R. B. Barreiro, M. Betoule, J. Bobin, A. Bonaldi, J. Delabrouille, G. de Zotti, C. Dickinson, H. K. Eriksen, J. González-Nuevo, F. K. Hansen, D. Herranz, M. Le Jeune, M. López-Caniego, E. Martínez-González, M. Massardi, J.-B. Melin, M.-A. Miville-Deschênes, G. Patanchon, S. Prunet, S. Ricciardi, E. Salerno, J. L. Sanz, J.-L. Starck, F. Stivoli, V. Stolyarov, R. Stompor, P. Vielva, A&A, 491, 597-615, (2008).
  15. Jump up Multiresolution internal template cleaning: an application to the Wilkinson Microwave Anisotropy Probe 7-yr polarization data, R. Fernández-Cobos, P. Vielva, R. B. Barreiro, E. Martínez-González, MNRAS, 420, 2162-2169, (2012).
  16. Jump up Wilkinson Microwave Anisotropy Probe 7-yr constraints on fNL with a fast wavelet estimator, B. Casaponsa, R. B. Barreiro, A. Curto, E. Martínez-González, P. Vielva, MNRAS, 411, 2019-2025, (2011).
  17. Jump up to: 17.017.1 Planck 2013 results. XXIII. Isotropy and statistics of the CMB, Planck Collaboration, 2014, A&A, 571, A23.
  18. Jump up to: 18.018.1 Planck 2013 results. XIX. The integrated Sachs-Wolfe effect, Planck Collaboration, 2014, A&A, 571, A19.
  19. Jump up to: 19.019.1 Planck 2013 results. XII. All-sky model of thermal dust emission, Planck Collaboration, 2014, A&A, 571, A12.
  20. Jump up Calibrating Milky Way dust extinction using cosmological sources, E. Mörtsell, A&A, 550, A80, (2013).
  21. Jump up The Sloan Digital Sky Survey Quasar Catalog. IV. Fifth Data Release, D. P. Schneider, P. B. Hall, G. T. Richards, M. A. Strauss, D. E. Vanden Berk, S. F. Anderson, W. N. Brandt, X. Fan, S. Jester, J. Gray, J. E. Gunn, M. U. SubbaRao, A. R. Thakar, C. Stoughton, A. S. Szalay, B. Yanny, D. G. York, N. A. Bahcall, J. Barentine, M. R. Blanton, H. Brewington, J. Brinkmann, R. J. Brunner, F. J. Castander, I. Csabai, J. A. Frieman, M. Fukugita, M. Harvanek, D. W. Hogg, Z. Ivezic, S. M. Kent, S. J. Kleinman, G. R. Knapp, R. G. Kron, J. Krzesinski, D. C. Long, R. H. Lupton, A. Nitta, J. R. Pier, D. H. Saxe, Y. Shen, S. A. Snedden, D. H. Weinberg, J. Wu, ApJ, 134, 102-117, (2007).
  22. Jump up Planck 2013 results. XIII. Galactic CO emission, Planck Collaboration, 2014, A&A, 571, A13.
  23. Jump up to: 23.023.123.223.323.423.5 Planck 2013 results. XVII. Gravitational lensing by large-scale structure, Planck Collaboration, 2014, A&A, 571, A17.

Flexible Image Transfer Specification

Full-Width-at-Half-Maximum

Cosmic Microwave background

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

Sunyaev-Zel'dovich

Planck Legacy Archive

(Planck) Low Frequency Instrument

(Planck) High Frequency Instrument

reduced IMO