Additional maps
Contents
Introduction[edit]
This section describes the map-based products that required special processing.
2015 lensing map[edit]
We distribute the minimum-variance (MV) lensing potential estimate presented in Planck-2015-A15^{[1]} 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 Planck-2015-A09^{[2]}.
The estimate is contained in a single gzipped tarball named 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.
Filename | Format | Description |
---|---|---|
dat_klm.fits | HEALPix FITS format alm, with | Contains the estimated lensing convergence | .
mask.fits.gz | HEALPix FITS format map, with | Contains the lens reconstruction analysis mask. |
nlkk.dat | ASCII text file, with columns = ( | , , )The approximate noise Planck-2015-A13^{[3]}. | (and signal+noise, ) power spectrum of , for the fiducial cosmology used in
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^{[4]}. 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. 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.
The full data set is contained in a single gzipped tarball named COM_CompMap_YSZ_R2.00.fits.tgz. Its contents are described below. Temporarily the tarball file can be found in the Supplement Data area of the PLA (go to pla.esac.esa.int/pla, go to Subsection Supplementary Data and type "YSZ" in the search form)
Filename | Format | Description |
---|---|---|
nilc_ymaps.fits | HEALPix FITS format map in Galactic coordinates with | Contains the NILC full mission, FIRST and LAST y-maps. |
milca_ymaps.fits | HEALPix FITS format map in Galactic coordinates with | Contains the MILCA full mission, FIRST and LAST y-maps. |
nilc_weights_BAND.fits | HEALPix FITS format map in Galactic coordinates with | 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 | 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 | Contains the stddev map for the NILC full mission y-map. |
milca_stddev.fits | HEALPix FITS format map in Galactic coordinates with | 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 | Contains foreground masks. |
nilc_bands.fits | ASCII table FITS format | Contains NILC wavelet bands in multipole space |
2015 lensing-induced B-mode map[edit]
We distribute the lensing-induced B-mode map presented in Planck-2015-XLI^{[5]}. The lensing B-mode Stokes parameter maps are produced by combining the lensing potential reconstruction from the SMICA CMB temperature map with E-mode data from the SMICA CMB polarization maps. The SMICA temperature and polarization products are described in Planck-2015-A09^{[2]}. The lensing-induced B-mode polarization maps are used in cross-correlation with the SMICA CMB polarization maps to obtain a lensing B-mode power spectrum measurement from approximately 70% of the sky, as described in Planck-2015-XLI^{[5]}.
We provide both raw products, which can be utilized to generate products adapted to one's specific needs in term of mask, filtering, etc., and "ready-to-use" products for cross-correlation study purposes.
Raw products[edit]
We deliver the non-normalized lensing-induced Stokes parameter maps, labelled Planck-2015-XLI^{[5]}. They are defined as
and , which form the basis of the final lensing B-mode estimator defined in equation (6) of
where Planck-2015-XLI^{[5]}, and is the filtered lensing potential estimate.
and are the filtered pure E-mode polarization maps given in equation (5) ofWe also provide the normalization transfer function Planck-2015-XLI^{[5]}, as well as the "L70" mask that retains 69% of the sky before apodization, and its apodized version , which has an effective sky fraction .
defined in equation (11) ofAs an example of the utilization of these products, the lensing B-mode maps that are shown in figure 4 of Planck-2015-XLI^{[5]} are generated from
,
where 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 and in the HEALPix "smoothing" routine, and using the product as an input filtering function.
is a Gaussian of 60 arcminSpecific products[edit]
We provide the lensing B-mode spherical harmonic coefficient estimate
over approximately 70% of the sky.It can also be constructed using the raw products described above from
,
where HEALPix "anafast" tool.
is a function for producing band-powers over the range , and is a short-hand notation for transforming a map into spin-weighted spherical harmonic coefficients , and forming . This can be done using, e.g., theThe lensing B-mode power spectrum estimate Planck-2015-XLI^{[5]} is obtained by forming the cross-correlation power spectrum of and the B-mode data from the SMICA polarization maps :
discussed in,
where CMB maps.
is the 5 arcmin Gaussian beam that convolves the SMICA
The products are contained in a single gzipped tarball named COM_Lensing-Bmode_R2.00.tgz. Its contents are described below.
Filename | Format | Description |
---|---|---|
bar_q_lens_map.fits | HEALPix FITS format map in Galactic coordinates with | Contains the non-normalized lensing-induced Q Stokes parameter map | .
bar_u_lens_map.fits | HEALPix FITS format map in Galactic coordinates with | Contains the non-normalized lensing-induced U Stokes parameter map | .
mask.fits | HEALPix FITS format map in Galactic coordinates with | The L70 mask. |
mask_noapo.fits | HEALPix FITS format map in Galactic coordinates with | The L70 mask without apodization. |
transfer_function_b_l.dat | ASCII text file, with columns = ( | , )The transfer function. |
lensing_bmode_b_lm.fits | HEALPix FITS format alm, with | Contains the lensing B-mode harmonic coefficients | .
lensing_bmode_bandpowers.dat | ASCII text file, with columns = ( | , , , , )The lensing B-mode bandpower estimate on approximativily 70% of the sky and over the multipole range from 10 to 2000 shown in figure 9 of Planck-2015-XLI^{[5]} (for plotting purposes only). |
2015 Integrated Sachs-Wolfe effect map[edit]
We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in Planck-2015-A21^{[6]} 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 single gzipped tarball named COM_CompMap_ISW_0064_R2.00.fits. Its contents are described below.
Extension | Format | Description | Used data sets |
---|---|---|---|
0 | HEALPix FITS format map with three components, , 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, , 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, , Ordering='Nest' | Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map | SEVEM DX11 CMB + NVSS + Planck lensing. |
References[edit]
- ↑ Planck 2015 results. XV. Gravitational Lensing, Planck Collaboration, 2016, A&A, 594, A15.
- ↑ ^{2.0}^{2.1} Planck 2015 results. XI. Diffuse component separation: CMB maps, Planck Collaboration, 2016, A&A, 594, A9.
- ↑ Planck 2015 results. XIII. Cosmological parameters, Planck Collaboration, 2016, A&A, 594, A13.
- ↑ Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect, Planck Collaboration, 2016, A&A, 594, A22.
- ↑ ^{5.0}^{5.1}^{5.2}^{5.3}^{5.4}^{5.5}^{5.6}^{5.7} Planck intermediate results. XLI. A map of lensing-induced B-modes, Planck Collaboration Int. XLI A&A, 596, A102, (2016).
- ↑ Planck 2015 results. XXI. The integrated Sachs-Wolfe effect, Planck Collaboration, 2016, A&A, 594, A21.
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).
Flexible Image Transfer Specification
Planck Legacy Archive
Full-Width-at-Half-Maximum