2015 Additional maps

Introduction

This section describes the products that required special processing.

2015 Lensing map

We distribute the minimum-variance (MV) lensing potential estimate presented in Planck-2015-A15 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.

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.

Contents of Lensing package

Filename	Format	Description
dat_klm.fits	HEALPIX FITS format alm, with [math] L_{\rm max} = 2048 [/math]	Contains the estimated lensing convergence [math] \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} [/math].
mask.fits.gz	HEALPIX FITS format map, with [math] N_{\rm side} = 2048 [/math]	Contains the lens reconstruction analysis mask.
nlkk.dat	ASCII text file, with columns = ([math]L[/math], [math]N_L [/math], [math]C_L+N_L[/math])	The approximate noise [math]N_L[/math] (and signal+noise, [math]C_L+N_L[/math]) power spectrum of [math] \hat{\kappa}_{LM} [/math], for the fiducial cosmology used in Planck-2015-A13.

2015 Compton parameter map

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. We also provide the ILC weights per scale and per frequency that were used to produce these y-maps. IDL routines are also provide 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 provide and we call them FIRST and LAST y-maps. Additionally we construct a 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 that 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.

Contents of COM_CompMap_YSZ_R2.00.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 ymaps.
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 ymaps.
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 ymap 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 ymap 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 ymap.
nilc_homnoise_spect.fits	ASCII table FITS format	Contains the angular power spectrum of the homogeneous noise in the NILC full mission ymap.
milca_homnoise_spect.fits	ASCII table FITS format	Contains the angular power spectrum of the homogeneous noise in the MILCA full mission ymap.
masks.fits	HEALPIX FITS format map, with [math] N_{\rm side} = 2048 [/math]	Contains foreground masks.
nilc_bands.fits	ASCII table FITS format	Contains NILC wavelet bands in multipole space

2015 Integrated Sachs-Wolfe effect map

We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in Planck-2015-A21 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 [http://pla.esac.esa.int/pla/aio/product-action?MAP.MAP_ID=== 2015 Integrated Sachs-Wolfe effect map ==

We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in Planck-2015-A21 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 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.