Additional maps

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

Description

Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of #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:

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 #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 #planck2013-p12:

'MV' curl reconstruction bandpowers from Fig A2 of #planck2013-p12

[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

The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of #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

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 #planck2013-p12.

File names and format

A single file named

• COM_CompMap_Lensing_2048_R1.10.fits

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

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

See README in the tarball for full details. These data were used in #Aumont2010

References

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1. References

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