Difference between revisions of "Specially processed maps"

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{{DISPLAYTITLE:Additional maps}}
 
==Overview==
 
==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 ==
 
== Lensing map ==
−
 
 
=== Description ===
 
=== Description ===
  
−
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. 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.
+
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:
 
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 $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.
+
; 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>.
−
; 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.
+
; 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.
−
; RLPP : This column contains the response function $R_L^{\phi\phi}$.
+
; RLPP : This column contains the response function <math>R_L^{\phi\phi}</math>.
−
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.
+
; 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.
 +
 
 +
Also, the table below gives the lensing curl-mode power spectrum data used to produce Figure A2 of {{PlanckPapers|planck2013-p12}}:
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center"
 +
|+ ''''MV' curl reconstruction bandpowers from Fig A2 of {{PlanckPapers|planck2013-p12}} '''
 +
|-  bgcolor="ffdead" 
 +
! <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>
 +
|-
 +
|    2 ||    7 || -13.6379  || 15.3409
 +
|-
 +
|    8 ||  20 ||  6.0184  ||  4.8881
 +
|-
 +
|    21 ||  39 ||  -1.0675  ||  3.0940
 +
|-
 +
|    40 ||  65 ||  0.6135  ||  1.8474
 +
|-
 +
|    66 ||  100 ||  1.5030  ||  1.2696
 +
|-
 +
|  101 ||  144 ||  1.3760  ||  0.9950
 +
|-
 +
|  145 ||  198 ||  -1.2289  ||  0.8286
 +
|-
 +
|  199 ||  263 ||  1.1910  ||  0.7001
 +
|-
 +
|  264 ||  338 ||  -0.6567  ||  0.6197
 +
|-
 +
|  339 ||  425 ||  -0.8201  ||  0.5235
 +
|-
 +
|  426 ||  525 ||  -0.7581  ||  0.4850
 +
|-
 +
|  526 ||  637 ||  -0.3201  ||  0.5134
 +
|-
 +
|  638 ||  762 ||  -0.1589  ||  0.4073
 +
|-
 +
|  763 ||  901 ||  -0.6451  ||  0.4044
 +
|-
 +
|  902 || 1054 ||  0.4910  ||  0.3718
 +
|-
 +
|  1055 || 1221 ||  -0.2186  ||  0.3702
 +
|-
 +
|  1222 || 1404 ||  -0.3295  ||  0.4146
 +
|-
 +
|  1405 || 1602 ||  -0.3647  ||  0.4703
 +
|-
 +
|  1603 || 1816 ||  -0.1060  ||  0.5904
 +
|-
 +
|  1817 || 2020 ||  -0.7887  ||  0.8507
 +
|}
 +
 
  
 
=== Production process ===
 
=== Production process ===
  
−
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ 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.
+
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.
  
 
===Inputs===
 
===Inputs===
  
 
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.
 
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.
−
The analysis mask is constructed using a synthesis of several planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]] catalogues.  
+
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}}.
  
−
===References===
+
===File names and format===
  
−
<biblio force=false>
+
A single file named
−
#[[References]]
+
*''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R1.10.fits|link=COM_CompMap_Lensing_2048_R1.10.fits}}''
−
</biblio>
+
with two BINTABLE extensions containing the items described below.
 +
 +
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>.
  
−
===File names and format===
+
<center>
 +
<gallery perrow=3 widths=260px heights=170px>
 +
File: analysis_lens_pub_map_orth_north_dat_p.png | Galactic north
 +
File: analysis_lens_pub_map_orth_south_dat_p.png | Galactic south
 +
</gallery></center>
  
−
A single file named
 
−
*''COM_CompMap_Lensing_2048_R1.10.fits''
 
−
with two BINTABLE extensions containing the items described below. 
 
  
  
Line 76: Line 130:
 
|}
 
|}
  
 +
== 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{{BibCite|aumont2010}}
  
 +
==References==
 +
<References />
 +
  
  
  
  
−
[[Category:Mission science products|010]]
+
[[Category:Mission products|010]]

Latest revision as of 17:34, 23 July 2014

Overview[edit]

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[edit]

Description[edit]

Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of Planck-2013-XVII[1]. 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:

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].
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.
RLPP 
This column contains the response function [math]R_L^{\phi\phi}[/math].
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 Planck-2013-XVII[1]. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.

Also, the table below gives the lensing curl-mode power spectrum data used to produce Figure A2 of Planck-2013-XVII[1]:

'MV' curl reconstruction bandpowers from Fig A2 of Planck-2013-XVII[1]
[math]L[/math]min [math]L[/math]max [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]
2 7 -13.6379 15.3409
8 20 6.0184 4.8881
21 39 -1.0675 3.0940
40 65 0.6135 1.8474
66 100 1.5030 1.2696
101 144 1.3760 0.9950
145 198 -1.2289 0.8286
199 263 1.1910 0.7001
264 338 -0.6567 0.6197
339 425 -0.8201 0.5235
426 525 -0.7581 0.4850
526 637 -0.3201 0.5134
638 762 -0.1589 0.4073
763 901 -0.6451 0.4044
902 1054 0.4910 0.3718
1055 1221 -0.2186 0.3702
1222 1404 -0.3295 0.4146
1405 1602 -0.3647 0.4703
1603 1816 -0.1060 0.5904
1817 2020 -0.7887 0.8507


Production process[edit]

The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of Planck-2013-XVII[1]. 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.

Inputs[edit]

This product is built from the 143 and 217 GHz Planck frequency maps, with 857GHz projected out as a dust template. 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 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, including the ERCSC, SZ and PCCS . The reconstruction was performed using the fiducial beam window functions B(l) from the HFI RIMO . Details of the procedure used to produce a lensing estimate from these inputs are given in Planck-2013-XVII[1].

File names and format[edit]

A single file named

with two BINTABLE extensions containing the items described below.

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].

  • Galactic north

  • Galactic south


FITS file structure
1. EXTNAME = LENS-MAP
Column Name Data Type Units Description
PHIBAR Real*4 none Map of the lensing potential estimate, convolved with RLPP
MASK Int none Region over which the lensing potential is reconstructed
Keyword Data Type Value Description
PIXTYPE string HEALPIX
COORDSYS string GALACTIC Coordinate system
ORDERING string NESTED Healpix ordering
NSIDE Int*4 2048 Healpix Nside
FIRSTPIX Int*4 0
LASTPIX Int*4 50331647
2. EXTNAME = TransFun
Column Name Data Type Units Description
RLPP Real*4 none Response function
NLPP Real*4 none Sky-averaged noise power spectrum estimate
Keyword Data Type Value Description
L_MIN Int*4 0 First multipole
L_MAX Int*4 2048 Last multipole

IRAM Maps of the Crab nebula[edit]

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[edit]

  1. ↑ 1.01.11.21.31.41.5 Planck 2013 results: Gravitational lensing by large-scale structure, Planck Collaboration XVII, A&A, in press, (2014).
  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).

(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).

Cosmic Microwave background

Flexible Image Transfer Specification

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