Difference between revisions of "Specially processed maps"

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== 2015 Lensing map ==
 
== 2015 Lensing map ==
  
We distribute the minimum-variance (MV) lensing potential estimate presented in {{PlanckPapers|planck2014-xxx}} 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 {{PlanckPapers|planck2014-xxx}}.
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We distribute the minimum-variance (MV) lensing potential estimate presented in {{PlanckPapers|planck2014-a17}} 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 {{PlanckPapers|planck2014-a11}}.
  
  
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== 2015 Compton parameter map ==
 
== 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 {{PlanckPapers|planck2014-xxii}}. 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.
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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 {{PlanckPapers|planck2014-a28}}. 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.
 
The full data set is contained in a single gzipped tarball named  ''COM_CompMap_YSZ_R2.00.fits.tgz''. Its contents are described below.

Revision as of 12:39, 5 February 2015

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[1] as part of the 2014 data release. This map represents an estimate of the CMBCosmic Microwave background 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 CMBCosmic Microwave background 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.


Contents of Lensing package
Filename Format Description
dat_klm.fits HEALPIX FITSFlexible Image Transfer Specification 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 FITSFlexible Image Transfer Specification 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 [3].

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[4]. 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 FITSFlexible Image Transfer Specification 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 FITSFlexible Image Transfer Specification 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 FITSFlexible Image Transfer Specification 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 FITSFlexible Image Transfer Specification 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 FITSFlexible Image Transfer Specification 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 FITSFlexible Image Transfer Specification 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 FITSFlexible Image Transfer Specification format Contains the angular power spectrum of the homogeneous noise in the NILC full mission ymap.
milca_homnoise_spect.fits ASCII table FITSFlexible Image Transfer Specification format Contains the angular power spectrum of the homogeneous noise in the MILCA full mission ymap.
masks.fits HEALPIX FITSFlexible Image Transfer Specification format map, with [math] N_{\rm side} = 2048 [/math] Contains foreground masks.
nilc_bands.fits ASCII table FITSFlexible Image Transfer Specification format Contains NILC wavelet bands in multipole space

References

  1. Planck 2015 results. XV. Gravitational Lensing, Planck Collaboration, 2016, A&A, 594, A15.
  2. Planck 2015 results. XI. Diffuse component separation: CMB maps, Planck Collaboration, 2016, A&A, 594, A9.
  3. Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect, Planck Collaboration, 2016, A&A, 594, A22.