Foreground maps
Contents
[hide]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):
- 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 frequency map, LFI 70 GHz frequency maps
- Full-mission 100 GHz frequency map, HFI 100 GHz frequency maps
- Full-mission 143 GHz frequency map, HFI 143 GHz frequency maps
- Full-mission 217 GHz frequency map, HFI 217 GHz frequency maps
- Full-mission 353 GHz frequency map, HFI 353 GHz frequency maps
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
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
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):
- 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 frequency map, LFI 70 GHz frequency maps
- Full-mission 100 GHz frequency map, HFI 100 GHz frequency maps
- Full-mission 143 GHz frequency map, HFI 143 GHz frequency maps
- Full-mission 217 GHz frequency map, HFI 217 GHz frequency maps
- Full-mission 353 GHz frequency map, HFI 353 GHz frequency maps
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
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
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
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:
Filename | Format | Description |
---|---|---|
mask.fits.gz | HEALPix FITS format map, with | Lens reconstruction analysis mask. |
TT/dat_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence | (from temperature only, after mean-field subtraction).
TT/mf_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence mean-field | subtracted from the raw temperature-only data estimate.
PP/dat_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence | (from polarization only, after mean-field subtraction).
PP/mf_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence mean-field | subtracted from the raw polarization-only data estimate.
MV/dat_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence | (minimum-variance estimate from temperature and polarization, after mean-field subtraction).
MV/mf_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence mean-field | subtracted from the raw minimum variance data estimate.
TT/nlkk.dat | ASCII text file, with columns = ( | , , )Temperature-only reconstruction approximate noise Planck-2020-A8[2]. | (and signal+noise, ) power spectrum of , for the fiducial cosmology used in
PP/nlkk.dat | ASCII text file, with columns = ( | , , )Polarization-only reconstruction approximate noise Planck-2020-A8[2].. | (and signal+noise, ) power spectrum of , for the fiducial cosmology used in
MV/nlkk.dat | ASCII text file, with columns = ( | , , )Minimum-variance reconstruction approximate noise Planck-2020-A8[2]. | (and signal+noise, ) power spectrum of , for the fiducial cosmology used in
with slight variations:
- - in COM_Lensing_Inhf_2048_R3.00, all HEALPix FITS format alm files have .
- - 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:
Filenames | Format | Description |
---|---|---|
/inputs/mask.fits.gz | compressed HEALPix FITS format map, with | Lens reconstruction analysis mask. |
/inputs/FFP10_wdipole_lenspotentialCls.dat | ASCII text file, with columns = ( | , , , , , , , )Input unlensed CMB spectra of the fiducial cosmology used in Planck-2020-A8[2]. |
TT/sim_klm_{???}.fits | 300 HEALPix FITS format alm, with | Estimated lensing convergence Planck-2020-A8[2]. | (from temperature only, no mean-field subtraction) of all 300 FFP10 simulations used in
PP/sim_klm_{???}.fits | 300 HEALPix FITS format alm, with | Estimated lensing convergence Planck-2020-A8[2]. | (from polarization only, no mean-field subtraction) of all 300 FFP10 simulations used in
MV/sim_klm_{???}.fits | 300 HEALPix FITS format alm, with | Estimated lensing convergence Planck-2020-A8[2]. | (minimum-variance estimate from temperature and polarization, no mean-field subtraction) of all 300 FFP10 simulations used in
TT/dat_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence | (from temperature only, no mean-field subtraction).
PP/dat_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence | (from polarization only, no mean-field subtraction).
MV/dat_klm.fits | HEALPix FITS format alm, with | Estimated lensing convergence | (minimum-variance estimate from temperature and polarization, no mean-field subtraction).
TT/nlkk.dat | ASCII text file, with columns = ( | , , , , , , )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 = ( | , , , , , , )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 = ( | , , , , , , )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 .
- - 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
Filenames | Format | Description |
---|---|---|
/inputs/clkk.dat | ASCII text file, with columns = ( | , )Input lensing convergence CMB spectrum of the fiducial cosmology used in Planck-2020-A8[2]. |
sky_klm_{???}.fits | 300 HEALPix FITS format alm, with | Input lensing convergence Planck-2020-A8[2]. | realizations of all 300 FFP10 simulations used in
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 CMB maps (we discard and in order to use lensing tracers that are statistically independent of the -mode map). In the second we further add CIB information at 545 GHz (GNILC) to the lensing tracer.
quadratic estimator built from the DX12 SMICAThese maps are filtered template of the lensing B-mode (both the lensing tracer and Planck-2020-A8[2] to produce the B-mode power spectrum (Fig. 14).
-mode used to build the B template are Wiener-filtered). The simulation suite may be used to assess the filter, as was done inThe B-mode template package is
- COM_Lensing-Bmode_2048_R3.00
with contents
Filenames | Format | Description |
---|---|---|
/inputs/mask.fits.gz | compressed HEALPix FITS format map, with | Planck-2020-A8[2]. | -mode analysis mask used in
/inputs/clbb.dat | ASCII text file, with columns = ( | , )Input lensing Planck-2020-A8[2]. | -mode power spectrum for the fiducial cosmology used in
dat_blm_TTTEETEE.fits | HEALPix FITS format alm, with | Lensing | -mode template built from the lensing tracer and -mode map.
dat_blm_545_TTTEETEE.fits | HEALPix FITS format alm, with | Lensing | -mode template built from the lensing tracer and -mode map.
The B-mode template simulation package is
- COM_Lensing-SimMap-Bmode_2048_R3.00
with contents
Filenames | Format | Description |
---|---|---|
/inputs/mask.fits.gz | compressed HEALPix FITS format map, with | Planck-2020-A8[2]. | -mode analysis mask used in
/inputs/clbb.dat | ASCII text file, with columns = ( | , )Input lensing Planck-2020-A8[2]. | -mode power spectrum for the fiducial cosmology used in
/TTTEETE/blm_{???}.fits | 300 HEALPix FITS format alm, with | Lensing Planck-2020-A8[2]. | -mode template built from the lensing tracer and -mode map of all 300 FFP10 simulations used in
/545_TTTEETE/blm_{???}.fits | 300 HEALPix FITS format alm, with | Lensing Planck-2020-A8[2]. | -mode template built from the lensing tracer and -mode map of all 300 FFP10 simulations used in
/TTTEETE/dat_blm.fits | HEALPix FITS format alm, with | Lensing | -mode template built from the lensing tracer and -mode map.
/545_TTTEETE/dat_blm.fits | HEALPix FITS format alm, with | Lensing | -mode template built from the lensing tracer and -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
.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 CMB B-polarization.
quadratic estimator together with the CIB, and is statistically independent from theThe lensing combined tracer data package is
- COM_Lensing-CIBcomb_2000_R3.00
with contents
Filenames | Format | Description |
---|---|---|
/inputs/mask.fits.gz | compressed HEALPix FITS format map, with | Tracer combination analysis mask used in Planck-2020-A8[2]. |
dat_klm_545_MV.fits | HEALPix FITS format alm, with | 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 | Lensing tracer built from the | 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
Filenames | Format | Description |
---|---|---|
/inputs/mask.fits.gz | compressed HEALPix FITS format map, with | Tracer combination analysis mask used in Planck-2020-A8[2]. |
545_MV/sim_klm_{???}.fits | 300 HEALPix FITS format alm, with | 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 | Lensing tracer built from the Planck-2020-A8[2]. | quadratic estimator and the CIB (GNILC 545 GHz map) of all 300 FFP10 simulations used in
545_MV/dat_klm.fits | HEALPix FITS format alm, with | 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 | Lensing tracer built from the | 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 mode of the displacement .
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') or aggressive ('agr2') 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]
Astrophysical components based on the 2015 data release
Astrophysical components based on the 2013 data release
References[edit]
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- Jump up ↑ Planck 2018 results. III. High Frequency Instrument data processing and frequency maps, Planck Collaboration, 2020, A&A, 641, A3.
- ↑ Jump up to: 4.04.14.2 Planck 2015 results. X. Diffuse component separation: Foreground maps, Planck Collaboration, 2016, A&A, 594, A10.
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- 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).
- ↑ Jump up to: 17.017.1 Planck 2013 results. XXIII. Isotropy and statistics of the CMB, Planck Collaboration, 2014, A&A, 571, A23.
- ↑ Jump up to: 18.018.1 Planck 2013 results. XIX. The integrated Sachs-Wolfe effect, Planck Collaboration, 2014, A&A, 571, A19.
- ↑ Jump up to: 19.019.1 Planck 2013 results. XII. All-sky model of thermal dust emission, Planck Collaboration, 2014, A&A, 571, A12.
- Jump up ↑ Calibrating Milky Way dust extinction using cosmological sources, E. Mörtsell, A&A, 550, A80, (2013).
- 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).
- Jump up ↑ Planck 2013 results. XIII. Galactic CO emission, Planck Collaboration, 2014, A&A, 571, A13.
- ↑ 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