Difference between revisions of "Specially processed maps"
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This section describes products that
This section describes products that special processing.
== Lensing map ==
== Lensing map ==
Revision as of 16:05, 3 February 2015
This section describes the products that required special processing.
We distribute the minimum-variance (MV) lensing potential estimate presented in  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 .
The estimate is contained in a single gzipped tarball named COM_CompMap_Lensing_2048_R2.00.tgz. Its contents are described below.
|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 .(and signal+noise, ) power spectrum of , for the fiducial cosmology used in|
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 . 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 ymap_R0.00.tgz. Its contents are described below.
|nilc_ymaps.fits||HEALPIX FITS format map in Galactic coordinates with||Contains the NILC full mission, FIRST and LAST ymaps.|
|milca_ymaps.fits||HEALPIX FITS format map in Galactic coordinates with||Contains the MILCA full mission, FIRST and LAST ymaps.|
|nilc_weights_BAND.fits||HEALPIX FITS format map in Galactic coordinates with||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||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||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 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||Contains foreground masks.|
|nilc_bands.fits||ASCII table FITS format||Contains NILC wavelet bands in multipole space|
Cosmic Microwave background
Flexible Image Transfer Specification