Sky temperature maps

General description

Sky maps give the best estimate of the intensity and polarization (Stokes Q and U components), if available, of the signal from the sky after removal, as far as possible, of known systematic effects (mostly instrumental, but including also the solar and earth-motion dipole, and the Zodiacal light). Sky maps are provided for the full Planck mission using all valid detectors in each frequency channel, and also for various subsets by splitting the mission in various time ranges or in subsets of the detectors in a given channel. These products are useful for the study of source variability, but they are especially interesting for characterisation purposes (see also the data validation section). The details of the start and end of the time ranges are given in the table below.

To help in further processing, there are also masks of the Galactic Plane and of point sources, each provided for several different depths.

All sky maps are in Healpix format, with Nside of 2048, in Galactic coordinates, and Nested ordering. The signal is given in units of K_cmb for 30-353 GHz, and of MJy/sr (for a constant [math]\nu F_\nu[/math] energy distribution ) for 545 and 857 GHz. For each frequency channel, the intensity and polarization maps are packaged into a BINTABLE extension of a FITS file together with a hit-count map (or hit map, for short, giving the number of observation samples that are cumulated in a pixel, all detectors combined) and with the variance and covariance maps. Additional information is given in the FITS file header. The structure of the FITS file is given in the FITS file structure section below.

Ranges for mission and surveys

Range	ODs	rings	pointing-IDs	Comment
nominal mission	91 - 563	240 - 14723	00004200 - 03180200
full mission	91 - 974	240 - 27005	00004200 - 05322620	for HFI
full mission	91 - 993	240 - 27641	00004200 - 06344800	for LFI
Survey 1	91 - 270	240 - 5720	00004200 - 01059820
Survey 2	270 - 456	5721 - 11194	01059830 - 02114520
Survey 3	456 - 636	11195 - 16691	02114530 - 03193660
Survey 4	636 - 807	16692 - 21720	03193670 - 04243900
Survey 5	807 - 974	21721 - 27005	05267180 - 05322590	end of mission for HFI
Survey 5	807 - 993	21721 - 27641	05267180 - 06344800	end of survey for LFI
Survey 6	993 - 1177	27642 - tbd	06344810 - 06398120	LFI only
Survey 7	1177 - 1358	tbd - tbd	06398130 - 06456410	LFI only
Survey 8	1358 - 1543	tbd - tbd	06456420 - 06511160	LFI only
Survey 9	1543 - 1604	tbd - tbd	06511170 - 06533320	LFI only
HFI mission-half-1	91 - 531	240 - 13471	00004200 - 03155580
HFI mission-half-2	531 - 974	13472 - 27005	03155590 - 05322590
LFI Year 1	91 - 456	240 - 11194	00004200 - 02114520
LFI Year 2	456 - 807	11195 - 21720	02114530 - 04243900
LFI Year 3	807 - 1177	21721 - tbd	05267180 - 06398120
LFI Year 4	1177 - 1543	tbd - tbd	06398130 - 06511160

Production process

Sky maps are produced by combining appropriately the data of all working detectors in a frequency channel over some period of the mission. They give the best estimate of the signal from the sky (unpolarised) after removal, as far as possible, of known systematic effects and of the dipole signals induced by the motion of the solar system in the CMB and of the Planck satellite in the solar system. In particular, they include the Zodiacal light emission (Zodi for short) and also the scattering from the far-side lobes of the beams (FSL). More on this below.

HFI processing

The mapmaking and calibration process is described in detail in the Map-making section and in the mapmaking paper, where detailed references are found. In brief it consists of:

binning the TOI data onto rings 

Healpix rings (HPRs) are used here, each ring containing the combined data of one pointing period.

flux calibration 

at 100-353 GHz, the flux calibration factors are determined by correlating the signal with the orbital dipole, which is determined very accurately from the Planck satellite orbital parameters provided by Flight Dynamics. This provides a single gain factor per bolometer. At 545 and 857 GHz the gain is determined from the observation of Uranus and Neptune (but not Jupiter which is too bright) and comparison to recent models made explicitly for this mission. A single gain is applied to all rings at these frequencies.

destriping 

in order to remove low-frequency noise, an offset per ring is determined by minimizing the differences between HPRs at their crossings, and removed.

Zodiacal light correction 

a Zodiacal light model is used to build HPRs of the the Zodi emission, which is subtracted from the calibrated HPRs.

projection onto the map 

the offset-corrected, flux-calibrated, and Zodi-cleaned HPRs are projected onto Healpix maps, with the data of each bolometer weighted by a factor of 1/NET of that bolometer.

These steps are followed by some post-processing which is designed to prepare the maps for the component separation work. This post processing consists of:

Dust bandpass leakage correction 

the Q and U maps are corrected for the dust leakage due to the different bandpasses that is determined using the ground method as described here

Far Side Lobe calibration correction 

the 100-217 maps are multiplied by factors of 1.00087, 1.00046, and 1.00043, respectively, to compensate for the non-removal of the far-side lobes, and similarly the corresponding covariance maps have also been corrected by multiplication by the square of the factor.

Fill missing pixels 

missing pixels are filled in with a value that is the mean of valid pixels within a given radius. A radius of 1 deg is used for the full channel maps, and 1.5 deg is used for the detset maps. This step is not applied to the single survey maps since they have large swaths of the sky that are not covered.

These maps provide the main mission products. Together with signal maps, hit count, variance, and variance maps are also produced. The hit maps give the (integer) number of valid TOI-level samples that contribute to the signal of each pixel. All valid samples are counted in the same way, i.e., there is no weighting factor applied. The variance maps project the white noise estimate, provided by the NETs, in the sky domain.

Note that the nominal mission maps have not had the post-processing applied, which makes them more easily comparable to the PR1 products.

LFI processing

LFI maps were constructed with the Madam map-making code, version 3.7.4. The code is based on generalized destriping technique, where the correlated noise component is modeled as a sequence of constant offset, called baselines. A noise filter was used to constrain the baseline solution allowing the use of 1 second baselines.

Radiometers were combined according to the horn-uniform weighting scheme to minimize systematics. The used weights are listed in Map-making. The flagged samples were excluded from the analysis by setting their weights to [math]C_{w}^{-1}[/math] = 0. The galaxy region was masked out in the destriping phase, to reduce error arising from strong signal gradients. The polarization component was included in the analysis...

A detailed description of the map-making procedure is given in Planck-2013-II and in section Map-making.

Types of maps

Full mission, full channel maps (6 HFI, 3 LFI)

Full channel maps are built using all the valid detectors of a frequency channel and cover the either the full or the nominal mission. For HFI, the 143-8 and 545-3 bolometers are rejected entirely as they are seriously affected by RTS noise. For this release, HFI provides the Q and U components for the 353 GHz channel only. LFI provides the I, Q and U maps for all the channels. The I maps are displayed in the figures below. The color range is set using a histogram equalisation scheme (from HEALPIX) that is useful for these non-Gaussian data fields. The Q and U maps are not shown as they look like noise to the naked eye.

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  Full mission, 30 GHz

• 

  Full mission, 44 GHz

• 

  Full mission, 70 GHz

• 

  Full mission, 100 GHz

• 

  Full mission, 143 GHz

• 

  Full mission, 217 GHz

• 

  Full mission, 353 GHz

• 

  Full mission, 545 GHz

• 

  Full mission, 857 GHz

Nominal mission, full channel maps (6 HFI)

These maps are similar to the ones above, but cover the nominal mission only. They are meant primarily to be compared to the PR1 products in order to see the level of improvements in the processing. Because of this, they are produced in Temperature only, and have not had the post-processing applied.

Single survey, full channel maps (30 HFI, 24 LFI)

Single survey maps are built using all valid detectors of a frequency channel; they cover separately the different sky surveys. The surveys are defined as the times over which the satellite spin axis rotates but 180 degrees, which, due to the position of the detectors in the focal plane does not cover the full sky, but a fraction between ~80 and 90% depending on detector position. During adjacent surveys the sky is scanned in opposite directions. More precisely it is the ecliptic equator that is scanned in opposite directions. While these are useful to investigate variable sources, they are also used to study the systematics of the time-response of the detectors as they scan bright sources, like the Galactic Plane, in different directions during different survey. Note that the HFI and LFI missions cover 5 and 9 surveys, respectively, and in both cases the last survey in incomplete.

Year maps, full channel maps (12 HFI, 24 LFI)

These maps are built using the data of surveys 1+2, surveys 3+4, and so forth. They are used to study long-term systematic effects.

Half-mission maps, full channel maps (12 HFI, 6 LFI)

For HFI, the half mission is defined after eliminating those rings discarded for all bolometers. There are 347 such rings, may of which are during the 5th survey when the End-of-Life tests were performed. The remaining 26419 rings are divided in half (up to the odd ring) to define the two halves of the mission. This exercise is done for the full mission only.

Full mission, single detector maps (18 HFI)

These maps are built only for the HFI SWBs (non polarized) and contain only temperature data, of course. They are not built for the polarisation sensitive detectors because they are not fixed on the sky as the polarisation component depends on the position angle at the time of observation. Instead, we provide maps built by quads of polarisation-sensitive detectors (see next section), which have different polarisation angles and that can be used to built I, Q, and U maps

HFI Temperature sensitive bolometers

Frequency	Detector names
143 GHz	143-5, 6, 7
217 GHz	217-1, 2, 3, 4
353 GHz	353-1, 2, 7, 8
545 GHz	545-1, 2, 4
857 GHz	857-1, 2 , 3, 4

The 143-8 and 353-3 bolometer data are affected by strong RTS (random telegraphic signal) noise. They have not been used in the data processing, and are not delivered. For a figure showing the focal plane layout, see this Introduction of the Detector Pointing chapter.

Full mission, detector set or detector pairs maps (8 HFI, 8 LFI)

The objective here is to build independent temperature (I) and polarisation (Q and U) maps with the two pairs of polarisation sensitive detectors of each channel where they are available, i.e. in the 30-353 GHz channels. The table below indicates which detectors were used to built each detector set (detset).

Definition of HFI Detector Sets

Frequency	DetSet1	DetSet2
100 GHz	100-1a/b & 100-4a/b	100-2a/b & 100-3a/b
143 GHz	143-1a/b 1 & 43-3a/b	143-2a/b & 143-4a/b
217 GHz	217-5a/b & 217-7a/b	217-6a/b & 217-8a/b
353 GHz	353-3a/b & 353-5a/b	353-4a/b & 353-6a/b

Half-ring maps (64 HFI, ??? LFI)

These maps are similar to the ones above, but are built using only the first or the second half of each ring (or pointing period). The HFI provides half-ring maps for the full mission only, and for the full channel, the detsets, and the single bolometers. The LFI .....

The Zodiacal light correction maps

The Zodiacal light signal depends on the location of the observer relative to the Zodiacal light bands, and thus it is not a fixed pattern on the sky but depends on the period of observation. The maps presented here are the difference between the uncorrected (and not delivered) and the corrected maps.

Caveats and known issues

TBW

Map zero-level

For the 100 to 857 GHz maps, the zero levels are set to their optimal levels for Galactic and CIB studies. A procedure for adjusting them to astrophysical values is given in the HFI Mapmaking and Calibration paper .

For the 30, 44 and 70 GHz, maps are corrected for zero level monopole by applying an offset correction, see LFI Calibration paper Planck-2013-V section 3.4 "Setting the zero levels in the maps". Note that the offset applied is indicated in the header as a comment keyword.

Inputs

HFI inputs

• The cleaned TOIs of signal of each detector, together with their flags, produced by the TOI processing pipeline
• The TOIs of pointing (quaternions), described in Detector pointing
• Bolometer-level characterization data, from the DPC's internal IMO (not distributed)
• Planck orbit data used to compute and remove the earth dipole
• WMAP solar dipole information used to calibrate the CMB channels
• Planet models used to calibrate the Galactic channels.

LFI inputs

The Madam map-maker takes as an input:

• The calibrated timelines (for details see TOI Processing)
• The detector pointings (for details see Detector pointing)
• The noise information in the form of three-parameter (white noise level ([math]\sigma[/math]), slope, and knee frequency ($f_\mathrm{knee}$)) noise model (for details see RIMO)

Related products

Masks

This section presents the masks of the point sources and of the Galactic plane. These are general purpose masks. Other masks specific to certain products are packaged with the products.

Point source masks

For HFI, two sets of masks are provided:

• Intensity masks, which removes sources detected with SNR > 5.
• Polarisation masks, which remove sources which have polarisation detection significance of 99.97 % or greater at the position of a source detected in intensity. They were derived from the polarisation maps with dust ground bandpass mismatch leakage correction applied. The cut around each source has a radius of 3σ (width) of the beam ~ 1.27 FWHM.

Both sets are found in the file HFI_Mask_PointSrc_2048_R2.00.fits in which the first extension contains the Intensity masks, and the second contains the Polarisation masks.

Galactic Plane masks

Eight masks are provided giving 20, 40, 60, 70, 80, 90, 97, and 99% sky coverage derived from the 353 GHz map, after CMB subtraction. They are independent of frequency channel. Three versions of these are given: not apodized, and apodized by 2 and 5 deg. The filenames are HFI_Mask_GalPlane-apoN_2048_R2.00.fits, where N = 0, 2, 5.

The masks are shows below. The 8 GalPlane masks are combined (added together) and shown in a single figure for each of the three apodization. While the result is quite clear for the case of no apodization, it is less so for the apodized case. The point source masks are shown separately for the Intensity case.

• 

  Galactic Plane masks, no apod

• 

  Galactic Plane masks, apod 2 deg

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  Galactic Plane masks, apod 5 deg

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  PointSource mask 100 GHz

• 

  PointSource mask 143 GHz

• 

  PointSource mask 217 GHz

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  PointSource mask 343 GHz

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  PointSource mask 545 GHz

• 

  PointSource mask 857 GHz

File names

The FITS filenames are of the form {H|L}FI_SkyMap_fff{-tag}_Nside_R2.nn_{coverage}-{type}.fits, where fff are three digits to indicate the Planck frequency band, tag indicates the single detector or the detset, Nside is the Healpix Nside of the map, coverage indicates which part of the mission is covered (full, half mission, survey, year, ...) , and the optional type indicates the subset of input data used. The table below lists the products by type, with the appropriate unix wildcards that form the full filename.

FITS filenames

Coverage	filename	half-ring filename
Full chan, full mission	HFI_SkyMap_???_2048_R2.??_full.fits	HFI_SkyMap_???_2048_R2.??_full-ringhalf-?.fits
Full channel, nominal mission	HFI_SkyMap_???_2048_R2.??_nominal.fits	n/a
Full channel, single survey	HFI_SkyMap_???_2048_R2.??_survey-?.fits	n/a
Full channel, single year	HFI_SkyMap_???_2048_R2.??_year-?.fits	n/a
Full channel, half mission	HFI_SkyMap_???_2048_R2.??_halfmission*-?.fits	n/a
Det-set, full mission	HFI_SkyMap_???-ds?_2048_R2.??_full.fits	HFI_SkyMap_???-ds?_2048_R2.??_full-ringhalf-?.fits
Single SWB, full mission	HFI_SkyMap_???-?_2048_R2.??_full.fits	HFI_SkyMap_???-?_2048_R2.??_full-ringhalf-?.fits

For the benefit of users who are only looking for the frequency maps with no additional information, we also provide a file combining the 9 frequency maps as separate columns in a single extension. The 9 columns in this file contain the intensity maps ONLY and no other information (hit maps and variance maps) is provided.

FITS file structure

The FITS files for the sky maps contain a minimal primary header with no data, and a BINTABLE extension (EXTENSION 1, EXTNAME = FREQ-MAP) containing the data. The structure is shows schematically in the figure below. The FREQ-MAP extension contains a 3- or a 10-column table that contain the signal, hit-count and variance maps, all in Healpix format. The 3-column case is for intensity only maps, the 10-column case is for polarisation. The number of rows is the number of map pixels, which is Npix = 12 Nside² for Healpix maps, where Nside = 2048 for most the maps presented in this chapter.

FITS file structure

Keywords indicate the coordinate system (GALACTIC), the Healpix ordering scheme (NESTED), the units (K_cmb or MJy/sr) of each column, and of course the frequency channel (FREQ). The COMMENT fields give a one-line summary of the product, and some other information useful for traceability within the DPCs. The original filename is also given in the FILENAME keyword. The BAD_DATA keyword gives the value used by Healpix to indicate pixels for which no signal is present (these will also have a hit-count value of 0). The main parameters are summarised below:

Sky map file data structure

1. EXTNAME = 'FREQ-MAP' : Data columns
Column Name	Data Type	Units	Description
I_STOKES	Real*4	K_cmb or MJy/sr	The Stokes I map
Q_STOKES	Real*4	K_cmb or MJy/sr	The Stokes Q map (optional)
U_STOKES	Real*4	K_cmb or MJy/sr	The Stokes U map (optional)
HITS	Int*4	none	The hit-count map
II_COV	Real*4	K_cmb2 or (MJy/sr)2	The II variance map
IQ_COV	Real*4	K_cmb2 or (MJy/sr)2	The IQvariance map (optional)
IU_COV	Real*4	K_cmb2 or (MJy/sr)2	The IQ variance map (optional)
QQ_COV	Real*4	K_cmb2 or (MJy/sr)2	The QQ variance map (optional)
QU_COV	Real*4	K_cmb2 or (MJy/sr)2	The QU variance map (optional)
UU_COV	Real*4	K_cmb2 or (MJy/sr)2	The UU variance map (optional)
Keyword	Data Type	Value	Description
PIXTYPE	string	HEALPIX
COORDSYS	string	GALACTIC	Coordinate system
ORDERING	string	NESTED	Healpix ordering
NSIDE	Int	1024 or 2048	Healpix Nside
FIRSTPIX	Int*4	0	First pixel number
LASTPIX	Int*4	12 Nside2 – 1	Last pixel number
FREQ	string	nnn	The frequency channel

The same structure applies to all SkyMap products, independent of whether they are full channel, survey of half-ring. The distinction between the types of maps is present in the FITS filename (and in the traceability comment fields).

Polarization convention used in the Planck project

The Planck collaboration used the COSMO convention for the polarization angle (as usually used in space based CMB missions), whereas other astronomical fields usually use the IAU convention. In the following document we report the difference between these two conventions, and the consequence if it is NOT taken into account correctly in the analysis.

Figure 1. COSMO convention (left) and IAU convention (right). The versor [math]\hat{z}[/math] points outwards the pointing direction in COSMO, and inwards in IAU. The bottom panel refers to the plane tangent to the sphere.

Changing the orientation convention is equivalent to a transformation [math]\psi'=\pi-\psi[/math] of the polarization angle (Figure 1). The consequence of this transformation is the inversion of the Stokes parameter [math]U[/math]. The components of the polarization tensor in the helicity basis [math]\epsilon^{\pm}=1/\sqrt{2}(\hat{x}\pm i\hat{y})[/math] are:

[math] (Q+iU)(\hat{n}) = \sum _{\ell m}a_{2,lm}{}_{2}Y_{\ell }^{m}(\hat{n}) \\(Q-iU)(\hat{n}) = \sum _{\ell m}a_{-2,lm}{}_{2}Y_{\ell }^{m}(\hat{n}) [/math]

where [math]{}_{2}Y_{\ell }^{m}(\hat{n})[/math] are the spin weighted spherical harmonic functions. The [math]E[/math] and [math]B[/math] modes can be defined as: [math] E(\hat{n}) = \sum_{\ell m}a_{E,\ell m}Y_{\ell }^{m}(\hat{n}) \\B(\hat{n}) = \sum_{\ell m}a_{B,\ell m}Y_{\ell }^{m}(\hat{n}) [/math]

where the coefficients [math]a_{E,\ell m}[/math] and [math]a_{B,\ell m}[/math] are derived from linear combinations of the [math]a_{2,\ell m}[/math] , [math]a_{-2,\ell m}[/math] defined implicitly in the first equation ([math]Q\pm iU[/math]).

Figure 2. Error on Planck-LFI 70 GHz [math]EE[/math] (top) and [math]BB[/math] (bottom) spectra, in case of wrong choice of the coordinate system convention (IAU instead of COSMO).

The effect of the sign inversion of [math]U[/math] on the polarization spectra is a non trivial mixing of [math]E[/math] and [math]B[/math] modes.

An example of the typical error on [math]EE[/math] and [math]BB[/math] auto-spectra in case of a wrong choice of the polarization basis is shown in Figure 2.

BE CAREFUL about the polarization convention you are using. If the IAU convention is used in computing the power spectra, the sign of the [math]U[/math] component of the Planck maps must be inverted before computing [math]E[/math] and [math]B[/math] modes.

Note on the convention used by the Planck Catalog of Compact Sources (PCCS)

For continuity with other compact sources catolgues, the Catalogue of Compact Sources provided by Planck follows the IAU convention, and the polarization angles are defined on an interval of [-90,90] degrees. To switch to the COSMO convention, the polarization angles listed in the catalogue have to be shifted by 90 degrees and multiplied by -1.