Difference between revisions of "Specially processed maps"

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== Lensing map ==
 
== Lensing map ==
=== Description ===
 
  
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of {{PlanckPapers|planck2013-p12}}. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.
+
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}}.
  
We distribute:
 
  
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate <math>\hat{\phi}</math> with the lensing response function <math>R_L^{\phi\phi}</math>. This map has been band-limited between multipoles <math>10 \le L \le 2048</math>.
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The estimate is contained in a single gzipped tarball named ''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R0.00.tgz|link=COM_CompMap_Lensing_2048_R0.00.tgz}}''. Its contents are described below.
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. ''Note'': the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.
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; RLPP : This column contains the response function <math>R_L^{\phi\phi}</math>.
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; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, <math>N_L^{\phi\phi}</math>. The noise is highly coloured. There is a dependence of the noise power spectrum on the local noise level of the map, discussed in Appendix A of {{PlanckPapers|planck2013-p12}}. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.
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Also, the table below gives the lensing curl-mode power spectrum data used to produce Figure A2 of {{PlanckPapers|planck2013-p12}}:
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center"
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|+ ''''MV' curl reconstruction bandpowers from Fig A2 of {{PlanckPapers|planck2013-p12}} '''
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|-  bgcolor="ffdead" 
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! <math>L</math><sub>min</sub> ||  <math>L</math><sub>max</sub> ||  <math>{\hat{C}_L}^{\psi\psi} (L(L+1))^2/(2\pi)</math> || <math> std({\hat{C}_L}^{\psi\psi})  (L(L+1))^2 /(2\pi)</math>
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|-
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|    2 ||    7 || -13.6379  || 15.3409
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|-
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|    8 ||  20 ||  6.0184  ||  4.8881
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|-
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|    21 ||  39 ||  -1.0675  ||  3.0940
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|-
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|    40 ||  65 ||  0.6135  ||  1.8474
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|-
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|    66 ||  100 ||  1.5030  ||  1.2696
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|-
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|  101 ||  144 ||  1.3760  ||  0.9950
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|-
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|  145 ||  198 ||  -1.2289  ||  0.8286
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|-
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|  199 ||  263 ||  1.1910  ||  0.7001
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|-
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|  264 ||  338 ||  -0.6567  ||  0.6197
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|-
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|  339 ||  425 ||  -0.8201  ||  0.5235
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|-
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|  426 ||  525 ||  -0.7581  ||  0.4850
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|-
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|  526 ||  637 ||  -0.3201  ||  0.5134
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|-
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|  638 ||  762 ||  -0.1589  ||  0.4073
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|-
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|  763 ||  901 ||  -0.6451  ||  0.4044
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|-
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|  902 || 1054 ||  0.4910  ||  0.3718
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|-
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|  1055 || 1221 ||  -0.2186  ||  0.3702
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|-
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|  1222 || 1404 ||  -0.3295  ||  0.4146
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|-
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|  1405 || 1602 ||  -0.3647  ||  0.4703
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|-
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|  1603 || 1816 ||  -0.1060  ||  0.5904
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|-
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|  1817 || 2020 ||  -0.7887  ||  0.8507
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|}
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=== Production process ===
+
 
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The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of {{PlanckPapers|planck2013-p12}}. The response function <math>R_L^{\phi\phi}</math> here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.
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===Inputs===
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This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.
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The analysis mask is constructed from a combination of thresholding in the 857GHz map (to remove the regions which are most contaminated by Galactic dust) and the [[CMB_and_astrophysical_component_maps#CO_emission_maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is joined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs are given in {{PlanckPapers|planck2013-p12}}.
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===File names and format===
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A single file named  
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*''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R1.10.fits|link=COM_CompMap_Lensing_2048_R1.10.fits}}''  
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with two BINTABLE extensions containing the items described below.  
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For illustration, we show in the figures below the maps of the Wiener-filtered CMB lensing potential in Galactic coordinates using orthographic projection. The reconstruction was bandpass filtered to <math>L \in [10, 2048]</math>. Note that the lensing reconstruction, while highly statistically significant, is still noise dominated for every individual mode, and is at best <math>S/N \simeq 0.7</math> around <math>L = 30</math>.
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<center>
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<gallery perrow=3 widths=260px heights=170px>
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File: analysis_lens_pub_map_orth_north_dat_p.png | Galactic north
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File: analysis_lens_pub_map_orth_south_dat_p.png | Galactic south
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</gallery></center>
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
 
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
|+ '''FITS file structure'''
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|+ ''' Contents of {{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R0.00.tgz|link=COM_CompMap_Lensing_2048_R0.00.tgz}} '''
|- bgcolor="ffdead" 
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!colspan="4" | 1. EXTNAME = ''LENS-MAP''
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|-  bgcolor="ffdead"   
 
|-  bgcolor="ffdead"   
! Column Name || Data Type || Units || Description
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! Filename || Format || Description
 
|-
 
|-
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP
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| 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 || Int || none || Region over which the lensing potential is reconstructed
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| mask.fits.gz || HEALPIX FITS format map, with <math> N_{\rm  side} = 2048 </math> || Contains the lens reconstruction analysis mask.
|- bgcolor="ffdead" 
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! Keyword || Data Type || Value || Description
+
 
|-
 
|-
|PIXTYPE  || string || HEALPIX || colspan="2"|  
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| 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 {{PlanckPapers|planck2014-xxx}}.
|-
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|COORDSYS  ||  string || GALACTIC || Coordinate system
+
|-
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|ORDERING  ||  string || NESTED  || Healpix ordering
+
|-
+
|NSIDE  || Int*4  ||  2048 ||colspan="2"| Healpix Nside
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|-
+
|FIRSTPIX || Int*4  ||          0 ||
+
|-
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|LASTPIX || Int*4  || 50331647 ||
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|- bgcolor="ffdead" 
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!colspan="4"| 2. EXTNAME = ''TransFun''
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|-  bgcolor="ffdead" 
+
! Column Name || Data Type || Units || Description
+
|-
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|RLPP || Real*4 || none || Response function
+
|-
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|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate
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|- bgcolor="ffdead" 
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! Keyword || Data Type || Value || Description
+
|-
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|L_MIN || Int*4  ||          0 || First multipole
+
|-
+
|L_MAX || Int*4  ||  2048 || Last multipole
+
 
|}
 
|}
 
  
 
== IRAM Maps of the Crab nebula ==
 
== IRAM Maps of the Crab nebula ==

Revision as of 21:52, 14 December 2014

Overview

This section describes products that require special processing. Only one such product is available at this time; this section will be expanded with time as more products are added.

Lensing map

We distribute the minimum-variance (MV) lensing potential estimate presented in [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 [1].


The estimate is contained in a single gzipped tarball named COM_CompMap_Lensing_2048_R0.00.tgz. Its contents are described below.


Contents of COM_CompMap_Lensing_2048_R0.00.tgz
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 [1].

IRAM Maps of the Crab nebula

Maps of the Crab nebula at 89.189 GHz (HCO+(1-0) transition) in both temperature and polarization, prodouced from observations performed at the IRAM 30m telescope from January 9th to January 12th 2009, are delivered as a tarball of 416 KB in the file

File:Crab IRAM 2010.zip

See README in the tarball for full details. These data were used in[2]

References

  1. 1.0 1.1 1.2
  2. Measurement of the Crab nebula polarization at 90 GHz as a calibrator for CMB experiments, J. Aumont, L. Conversi, C. Thum, H. Wiesemeyer, E. Falgarone, J. F. Macías-Pérez, F. Piacentini, E. Pointecouteau, N. Ponthieu, J. L. Puget, C. Rosset, J. A. Tauber, M. Tristram, A&A, 514, A70+, (2010).