https://wiki.cosmos.esa.int/planckpla/api.php?action=feedcontributions&user=Lvibert&feedformat=atomPlanck PLA Wiki - User contributions [en-gb]2024-03-28T12:58:44ZUser contributionsMediaWiki 1.31.6https://wiki.cosmos.esa.int/planckpla/index.php?title=Sky_temperature_maps&diff=7449Sky temperature maps2013-03-21T10:38:45Z<p>Lvibert: </p>
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<div>==General description==<br />
----------------------<br />
<br />
Sky maps give the best estimate of the intensity of the signal from the sky 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. Sky maps are provided for the nominal Planck mission and also, separately, for the first two single surveys, the third one being covered only for a small part during the nominal mission.The details of the start and end times of each are given in [[HFIpreprocessingstatics | this table]]. As a secondary product, maps with estimates of the Zodiacal light and Far-Side-Lobes contribution removed are also provided. <br />
<br />
For characterization purposes, are also provided maps covering the nominal survey but each one using only half of the available data. These are the ''ringhalf_{1|2}'' maps, which are built using the first and second half of the stable pointing part in each pointing period. These maps are used extensively to investigate the (high frequency) noise properties the maps themselves and of other products described elsewhere (see e.g., the [[HFI-Validation | data validation]] section).<br />
<br />
To help in further processing, there are also masks of the Galactic Plane and of point sources, each provided for several different depths.<br />
<br />
All sky maps are in Healpix format, with Nside of 2048 for HFI and of 1024 for LFI, in Galactic coordinates, and Nested ordering. The signal is given in units of K<sub>cmb</sub> for 30-353 GHz, and of MJy/sr (for a constant $\nu F_\nu$ energy distribution ) for 545 and 857 GHz. Each sky map is 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 a variance map (determined from the half-ring maps), and additional information is given in the FITS file header. The structure of the FITS file is given in the [[#Format | FITS file structure]] section below.<br />
<br />
===Types of maps ===<br />
<br />
; Full channel maps<br />
: Full channel maps are built using all the valid detectors of a frequency channel and cover the nominal mission. For HFI, the 143-8 and 545-3 bolometers are rejected entirely as they are seriously affected by RTS noise. The maps are displayed in the figures below. The range is the same from 30 - 143 GHz in order to show the CMB at the same level. At higher frequencies the range is increased in order to keep the Galactic Plane from invading the whole sky.<br />
<br />
<center><br />
<gallery style="padding:0 0 0 0;" perrow=3 widths=260px heights=160px> <br />
File: SkyMap30.png| '''Nominal mission, 30 GHz'''<br />
File: SkyMap44.png | '''Nominal mission, 44 GHz'''<br />
File: SkyMap70.png | '''Nominal mission, 70 GHz'''<br />
File: SkyMap100.png | '''Nominal mission, 100 GHz'''<br />
File: SkyMap143.png | '''Nominal mission, 143 GHz'''<br />
File: SkyMap217.png | '''Nominal mission, 217 GHz'''<br />
File: SkyMap353.png | '''Nominal mission, 353 GHz'''<br />
File: SkyMap545.png | '''Nominal mission, 545 GHz'''<br />
File: SkyMap857.png | '''Nominal mission, 857 GHz'''<br />
</gallery><br />
</center><br />
<br />
; Single survey maps <br />
: 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.<br />
<br />
; Detector set or detector pairs maps<br />
: These are maps built from a subset of the detectors in a frequency channel, typically our of two PSB pairs (i.e., four poloarisation-sensitive bolometers with different orientation on the sky), for HFI in order to extract a single temperature map. While none of these maps are part of the first Planck data release, the concept of ''detset'' is used, and thus it is worth mentioning it here. In particular, information by detector set is available at the [[Frequency_maps_angular_power_spectra | sky power spectrum]] level and in the [[The RIMO | RIMO]].<br />
<br />
; Half-ring maps<br />
: Half-ring maps are built using only the first or the second half of the stable pointing period data. There are thus two half-ring maps per frequency channel named ''ringhalf_1'' and ''ringhalf_2'' respectively. These maps are built for characterization purposes in order to perform null tests. In particular, the difference between the two half-ring maps at a given frequency give a good estimate of the high frequency noise in the data (albeit biased low by ~0.5% for the HFI channels due to specifics of the TOI processing).<br />
<br />
; Masks<br />
: Masks are provided of the Galactic Plane and of the point sources. For the Galactic Plane, eight masks are given covering different fractions of the sky, and for the points sources two masks are given, at the 5 and 10 sigma level, for each Planck HFI frequency channel. These are generic masks, specific masks applicable to other products are delivered with the products themselves.<br />
<br />
=== Caveats and known issues ===<br />
<br />
The primary limitation of the HFI maps are<br />
* the absence of correction of the ADC non-linearities,<br />
* the far-side lobe contribution is not accounted for in the processing and in the calibration,<br />
* the dipole removal is based on the non-relativistic approximation which leaves a weak quadrupole component in the map.<br />
And thus the overall calibration accuracy is at the 0.2% level in 100-217 GHz channels<br />
<br />
==== Map zero-level ====<br />
<br />
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 Calibration paper <cite>#planck2013-p03b</cite> {{P2013|8}}.<br />
<br />
For the 30, 44 and 70 GHz, maps are corrected for zero level monopole by applying an offset correction, see LFI Calibration paper <cite>#planck2013-p02b</cite> {{P2013|5}} section 3.4 "Setting the zero levels in the maps". Note that the offset applied is indicated in the header as a comment keyword.<br />
<br />
==== The Zodiacal light and the Far-Side Lobes ====<br />
<br />
The figures below show the modeled Zodiacal light and Far Side Lobes projected onto the maps; they are simply the difference between the ''main product'' and the ''ZodiCorrected'' maps for the nominal mission. The units are given in the figures. The ''heat'' color table has been used in place of the standard Planck for clarity reasons. <br />
<center><br />
<gallery perrow=3 widths=260px heights=170px><br />
File: ZodiRes100.png | '''zodi/FSL rediduals - 100 GHz'''<br />
File: ZodiRes143.png | '''zodi/FSL rediduals - 143 GHz''' <br />
File: ZodiRes217.png | '''zodi/FSL rediduals - 217 GHz'''<br />
File: ZodiRes353.png | '''zodi/FSL rediduals - 353 GHz'''<br />
File: ZodiRes545.png | '''zodi/FSL rediduals - 545 GHz'''<br />
File: ZodiRes857.png | '''zodi/FSL rediduals - 857 GHz'''<br />
</gallery><br />
</center><br />
The effects of the FSLs are seen most clearly at the highest frequencies, as structures roughly symmetric about the center of the image, which corresponds to the location of the Galactic Centre, which is in turn the source of most of the radiation that is scattered into the FSLs.<br />
<br />
==== Artifacts near caustics of the scanning strategy ==== <br />
<br />
The [[Survey scanning and performance|scanning strategy]] is such that regions around the Ecliptic poles are surveyed very deeply and compared to the average, and the transition from the nominal depth to the high depth, as shows on hit-count maps is very rapid, namely a few pixels, for a contrast of ~30. These transitions, or caustics in the maps, occur at different positions on the sky for different detectors, as the positions depend on their location in the focal plane of the instrument. As a result, when data from different detectors are combined to build a full channel map, the the weights of different detectors in the mix changes rapidly across the caustic, and given the remaining errors in the relative calibration of the detectors, a visible effect can be introduced in the maps, especially when the SNR is very high, i.e. at the highest frequencies and near bright regions like the Galactic Plane. Some examples are shown below.<br />
<br />
<center><br />
<gallery perrow=3 heights=260px widths=260pix ><br />
File: causta857.png | '''857 GHz intensity map around (272.5, -27)'''<br />
File: caustb857.png | '''857 GHz intensity map around (264.5, -37.5)'''<br />
File: caustc857.png | '''857 GHz intensity map around (98.5, 43)'''<br />
File: hita857.png | '''857 GHz hit count map around (272.5, -27)'''<br />
File: hitb857.png | '''857 GHz hit count map around (264.5, -37.5)'''<br />
File: hitc857.png | '''857 GHz hit count map around (98.5, 43)'''<br />
</gallery><br />
</center><br />
<br />
==Production process==<br />
----------------------<br />
<br />
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.<br />
<br />
=== HFI processing ===<br />
<br />
The inputs to the mapmaking are TOIs of signal that have been cleaned (as far as possible) of instrumental effects and calibrated in absorbed watts. While the processing involved is described in detail in the [[TOI processing|TOI processing]] section, we give a very brief summary here for convenience. That pipeline performs the following operations:<br />
<br />
; demodulation: this is performed around a variable level which is determined from the valid input data (a validity flag from a previous version of the processing is used for this purpose), and the data are converted to engineering units (V) using known conversion coefficients.<br />
; despiking: using the demodulated data converted to V (by the transfer function) the glitches are identified and fitted with templates. A glitch flag is produced that identifies the strongest part of the glitches, and a timeline of glitch tails is produced from the template fits, and subtracted from the demodulated timeline from step 1. Finally, the flagged ranges are replaced with data from an average over the pointing period (TBC)<br />
; dark template removal: the two dark bolometers are demodulated and despiked as above; the resulting timelines are then smoothed and used as an indicator of the overall temperature variations of the bolometer plate. Where the variations are consistent with each other, they are combined and removed from the bolometer signal timelines using appropriate coupling coefficients. The few percent of the data where they are not consistent are flagged on the timelines.<br />
; conversion to absorbed power: the timeline is converted to watts of absorbed power using the bolometer function. This includes a non-linearity correction; removal of the 4K cooler lines: the electromagnetic interference of the 4K cooler with the bolometer readout wires induces some sharp lines in the signal power spectra at frequencies of the 4K cooler's fundamental and its multiples, folded by the signal modulations. Fourier coefficients of the relevant lines are determined on a per-ring basis, and then removed from the data. The quality of the removal depends on the bolometer.<br />
; deconvolution by the time transfer function: this is done to correct for the non-instantaneous time response of the bolometers. The function itself is modeled using 4 parameters which are adjusted primarily on the planet data and also from comparisons of the northward and southward scans of the Galactic Plane. It is then removed using Fourier techniques, which has the side-effect of increasing the noise at high frequencies.<br />
; jump correction: removes some (relatively rare: 0.3 jumps per bolometer per pointing period, on average) jumps in the signal baseline. The jumps are detected characterized on smoothed TOIs, and corrected by adding a constant to part of the signal timeline. The origin of the jumps is not known.<br />
<br />
The results of this processing are a timeline of signal (in absorbed watts) and a ''valid data'' flag timeline for each of the 50 valid bolometers processed; these timelines contain the full sky signal, i.e., including the solar and orbital dipoles, the Zodiacal light, and contributions from the Far-Side lobes. The dipoles are necessary for the flux calibration and are removed at the mapmaking stage. The remaining two bolometers (143-8 and 535-3) show semi-random jumps in the signal level, typically jumping over 2-5 different ''pseudo-baseline'' levels, a behavior known as ''Random Telegraphic Signal'', so that these are commonly called the RTS bolometers. Finally, ring-level statistics of different types (mean, median, rms, kurtosis, etc.) are determined on a per-ring basis for all timelines, and a selection based on these statistics is used to discard anomalous rings, which are recorded in a ring-level flag for each valid bolometer timeline (see the [[TOI_processing#Discarded_rings| Discarded rings]] section). <br />
<br />
Throughout this processing, bright planets (Mars, Jupiter, Saturn, Uranus) and bright asteroids are masked in the timeline in order to avoid ringing effects in the processing. Since they move on the sky, the portion of the sky masked during one survey is observed during one, and no hole is left in the final map. In parallel, the planet data are processed in a similar way, but with different parameters for the despiking step, and without the final jump correction step. These results are processed separately to determine the beam shapes and the focal plane geometry.<br />
<br />
The pointing is determined starting from the AHF produced by MOC, which gives the direction and orientation of the LOS of a fiducial position in the focal plane at frequencies of 8Hz during stable pointing and 4 Hz during maneuvers (TBC for details, reference). This is interpolated to the times of data observation (ref to method), corrected for the wobble and other time-dependent offsets determined from the observed positions of a large number of sources around the sky, and finally converted to the LOS of each detector using the quaternions in the IMO (which are determined from observations of bright planets - see the [[Detector_pointing]] section). <br />
<br />
The mapmaking and calibration process is described in detail in the [[Map-making_LFI | Map-making]] section, where detailed references are found. In brief it consists of:<br />
<br />
; binning the TOI data onto ''rings'' : Healpix rings (HPRs) are used here, each ring containing the combined data of one pointing period. <br />
; flux calibration : at 100-353 GHz, the flux calibration factors are determined for each pointing period (or ring) from the solar-motion dipole, using the WMAP dipole as the reference, and after removal of the dipole signal induced by the motion of the Planck satellite in the solar system. This gain by ring is smoothed with a window of width 50 rings, which reveals an apparent variation of ~1-2% on a scale of 100s to 1000s of rings for the 100-217 GHz channels, and is applied. At 353GHz, where the solar motion dipole is weaker compared to the signal, no gain variation is detected (within the uncertainties), and a single fixed gain is applied to all rings. 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.<br />
; 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.<br />
; projection onto the map : the offset-corrected and flux-calibrated HPRs are projected onto Healpix maps, with the data of each bolometer weighted by a factor of 1/NET of that bolometer, and accounting for the slight different band transmission profiles of the bolometers in each band. <br />
<br />
These maps provide the main mission products. A second, reduced, set of maps, cleaned of the Zodiacal emission of the FSL leakage is also produced for the nominal mission and the two single surveys, but not for the half-rings (since the contribution would be the same for the two halves of each ring). For this purpose, the the Zodiacal emission and the FSL contamination, which are not fixed on the sky, are modeled separately at HPR-level, and subtracted from the signal HPR before projecting them onto the maps. <br />
<br />
Together with signal maps, hit count 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.<br />
<br />
=== LFI processing ===<br />
<br />
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.<br />
<br />
Radiometers were combined according to the horn-uniform weighting scheme to minimize systematics. The used weights are listed in [[Map-making LFI#Map-making|Map-making]]. The flagged samples were excluded from the analysis by setting their weights to $C_{w}^{-1}$ = 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, although only the temperature maps are released. <br />
<br />
A detailed description of the map-making procedure is given in <cite>#planck2013-p02</cite> {{P2013|2}} and in section [[Map-making LFI#Map-making|Map-making]].<br />
<br />
==Inputs==<br />
------------<br />
<br />
=== HFI inputs ===<br />
<br />
* The cleaned TOIs of signal of each detector, together with their flags, produced by the [[TOI processing|TOI processing]] pipeline<br />
* The TOIs of pointing (quaternions), described in [[Detector_pointing]]<br />
* Bolometer-level characterization data, from the DPC's internal IMO (not distributed)<br />
* Planck orbit data used to compute and remove the earth dipole<br />
* WMAP solar dipole information used to calibrate the CMB channels<br />
* Planet models used to calibrate the Galactic channels.<br />
<br />
=== LFI inputs ===<br />
<br />
The Madam map-maker takes as an input:<br />
<br />
* The calibrated timelines (for details see [[TOI processing LFI|TOI Processing]])<br />
* The detector pointings (for details see [[Pointing LFI|Detector pointing]])<br />
* The noise information in the form of three-parameter (white noise level ($\sigma$), slope, and knee frequency ($f_\mathrm{knee}$)) noise model (for details see [[The RIMO|RIMO]])<br />
<br />
<br />
==Related products==<br />
---------------------<br />
<br />
=== Masks ===<br />
<br />
Masks are provided of<br />
<br />
; the Galactic Plane<br />
: 8 masks are provided giving 20, 40, 60, 70, 80, 90, 97, and 99% sky coverage in two different files, at Nside=2048. For the HFI they can be used as they are, for the LFI they need to be downgraded at Nside=1024<br />
<br />
; the point sources<br />
: 18 masks are provided, 2 per frequency channel, each masking at the 5 and 10$\sigma$ level. For the HFI they can be used as they are, for the LFI they need to be downgraded at Nside=1024<br />
<br />
The masks are binary, in GALACTIC coordinates, and NESTED ordering. The table below give the filenames. <br />
<br />
{| class="wikitable" align="center" style="text-align:center" border="1" cellpadding="5" cellspacing="0" <br />
|+ '''FITS filenames for masks'''<br />
|- bgcolor="ffdead"<br />
! Galactic Plane masks|| Point Sources masks<br />
|-<br />
| {{PLASingleFile|fileType=map|name=HFI_Mask_GalPlane_2048_R1.10.fits|link=HFI_Mask_GalPlane_2048_R1.10.fits}} || {{PLASingleFile|fileType=map|name=HFI_Mask_PointSrc_2048_R1.10.fits|link=HFI_Mask_PointSrc_2048_R1.10.fits}}<br />
|-<br />
|}<br />
<br />
The masks are shows below in a single figure. While this is quite clear for the Galactic Plane masks, it is less so for the point source masks, but it does give a clear perspective on how the latter are distributed over the sky.<br />
<br />
<center><br />
<gallery perrow=2 widths=300px heights=185px ><br />
File: HFI_GalPlaneMask.png | '''Galactic Plane masks'''<br />
File: HFI_PointSrcMask.png | '''PointSource masks'''<br />
</gallery><br />
</center><br />
<br />
<br />
== File names ==<br />
-----------------<br />
<br />
The FITS filenames are of the form ''{H|L}FI_SkyMap_fff_nnnn_R1.nn_{coverage}_{type}.fits'', where ''fff'' are three digits to indicate the Planck frequency band, and ''nnnn'' is the Healpix Nside of the map, ''coverage'' indicates which part of the mission is covered, and the optional ''type'' indicates the subset of input data used. A full list of products, with links to them in the Archive, is given in the tables below.<br />
<br />
{| class="wikitable" align="center" style="text-align:center" border="1" cellpadding="5" cellspacing="0" width=500px<br />
|+ '''FITS filenames'''<br />
|- bgcolor="ffdead"<br />
! Frequency || Full channel maps<br />
|-<br />
| '''30GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_030_1024_R1.10_nominal.fits|link=LFI_SkyMap_030_1024_R1.10_nominal.fits}}<br />
|-<br />
| '''44GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_044_1024_R1.10_nominal.fits|link=LFI_SkyMap_044_1024_R1.10_nominal.fits}}<br />
|-<br />
| '''70GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_070_1024_R1.10_nominal.fits|link=LFI_SkyMap_070_1024_R1.10_nominal.fits}}<br />
|-<br />
| '''100GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_100_2048_R1.10_nominal.fits|link=HFI_SkyMap_100_2048_R1.10_nominal.fits}}<br />
|-<br />
| '''143GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_143_2048_R1.10_nominal.fits|link=HFI_SkyMap_143_2048_R1.10_nominal.fits}}<br />
|-<br />
| '''217GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_217_2048_R1.10_nominal.fits|link=HFI_SkyMap_217_2048_R1.10_nominal.fits}}<br />
|-<br />
| '''353GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_353_2048_R1.10_nominal.fits|link=HFI_SkyMap_353_2048_R1.10_nominal.fits}}<br />
|-<br />
| '''545GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_nominal.fits|link=HFI_SkyMap_545_2048_R1.10_nominal.fits}}<br />
|-<br />
| '''857GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_857_2048_R1.10_nominal.fits|link=HFI_SkyMap_857_2048_R1.10_nominal.fits}}<br />
|- bgcolor="ffdead"<br />
! Frequency || Full channel, Zodi-corrected maps<br />
|-<br />
| '''100GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_100_2048_R1.10_nominal_ZodiCorrected.fits|link=HFI_SkyMap_100_2048_R1.10_nominal_ZodiCorrected.fits}} <br />
|-<br />
| '''143GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_143_2048_R1.10_nominal_ZodiCorrected.fits|link=HFI_SkyMap_143_2048_R1.10_nominal_ZodiCorrected.fits}}<br />
|-<br />
| '''217GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_217_2048_R1.10_nominal_ZodiCorrected.fits|link=HFI_SkyMap_217_2048_R1.10_nominal_ZodiCorrected.fits}}<br />
|-<br />
| '''353GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_353_2048_R1.10_nominal_ZodiCorrected.fits|link=HFI_SkyMap_353_2048_R1.10_nominal_ZodiCorrected.fits}}<br />
|-<br />
| '''545GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_nominal_ZodiCorrected.fits|link=HFI_SkyMap_545_2048_R1.10_nominal_ZodiCorrected.fits}}<br />
|-<br />
| '''857GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_857_2048_R1.10_nominal_ZodiCorrected.fits|link=HFI_SkyMap_857_2048_R1.10_nominal_ZodiCorrected.fits}}<br />
|}<br />
<br />
<br />
{| class="wikitable" align="center" style="text-align:center" border="1" cellpadding="5" cellspacing="0" width=850px<br />
|+ '''FITS filenames'''<br />
|- bgcolor="ffdead"<br />
! Frequency || Survey 1 maps || Survey 2 maps<br />
|-<br />
| '''30GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_030_1024_R1.10_survey_1.fits|link=LFI_SkyMap_030_1024_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=LFI_SkyMap_030_1024_R1.10_survey_2.fits|link=LFI_SkyMap_030_1024_R1.10_survey_2.fits}}<br />
|-<br />
| '''44GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_044_1024_R1.10_survey_1.fits|link=LFI_SkyMap_044_1024_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=LFI_SkyMap_044_1024_R1.10_survey_2.fits|link=LFI_SkyMap_044_1024_R1.10_survey_2.fits}}<br />
|-<br />
| '''70GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_070_1024_R1.10_survey_1.fits|link=LFI_SkyMap_070_1024_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=LFI_SkyMap_070_1024_R1.10_survey_2.fits|link=LFI_SkyMap_070_1024_R1.10_survey_2.fits}}<br />
|-<br />
| '''100GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_100_2048_R1.10_survey_1.fits|link=HFI_SkyMap_100_2048_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_100_2048_R1.10_survey_2.fits|link=HFI_SkyMap_100_2048_R1.10_survey_2.fits}}<br />
|-<br />
| '''143GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_143_2048_R1.10_survey_1.fits|link=HFI_SkyMap_143_2048_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_143_2048_R1.10_survey_2.fits|link=HFI_SkyMap_143_2048_R1.10_survey_2.fits}}<br />
|-<br />
| '''217GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_217_2048_R1.10_survey_1.fits|link=HFI_SkyMap_217_2048_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_217_2048_R1.10_survey_2.fits|link=HFI_SkyMap_217_2048_R1.10_survey_2.fits}}<br />
|-<br />
| '''353GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_353_2048_R1.10_survey_1.fits|link=HFI_SkyMap_353_2048_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_353_2048_R1.10_survey_2.fits|link=HFI_SkyMap_353_2048_R1.10_survey_2.fits}}<br />
|-<br />
| '''545GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_survey_1.fits|link=HFI_SkyMap_545_2048_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_survey_2.fits|link=HFI_SkyMap_545_2048_R1.10_survey_2.fits}}<br />
|-<br />
| '''857GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_survey_1.fits|link=HFI_SkyMap_545_2048_R1.10_survey_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_survey_2.fits|link=HFI_SkyMap_545_2048_R1.10_survey_2.fits}}<br />
|- bgcolor="ffdead"<br />
! Frequency || Survey 1 Zodi-corrected maps || Survey 2 Zodi-corrected maps<br />
|-<br />
| '''100GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_100_2048_R1.10_survey_1_ZodiCorrected.fits|link=HFI_SkyMap_100_2048_R1.10_survey_1_ZodiCorrected.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_100_2048_R1.10_survey_2_ZodiCorrected.fits|link=HFI_SkyMap_100_2048_R1.10_survey_2_ZodiCorrected.fits}}<br />
|-<br />
| '''143GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_143_2048_R1.10_survey_1_ZodiCorrected.fits|link=HFI_SkyMap_143_2048_R1.10_survey_1_ZodiCorrected.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_143_2048_R1.10_survey_2_ZodiCorrected.fits|link=HFI_SkyMap_143_2048_R1.10_survey_2_ZodiCorrected.fits}}<br />
|-<br />
| '''217GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_217_2048_R1.10_survey_1_ZodiCorrected.fits|link=HFI_SkyMap_217_2048_R1.10_survey_1_ZodiCorrected.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_217_2048_R1.10_survey_2_ZodiCorrected.fits|link=HFI_SkyMap_217_2048_R1.10_survey_2_ZodiCorrected.fits}}<br />
|-<br />
| '''353GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_353_2048_R1.10_survey_1_ZodiCorrected.fits|link=HFI_SkyMap_353_2048_R1.10_survey_1_ZodiCorrected.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_353_2048_R1.10_survey_2_ZodiCorrected.fits|link=HFI_SkyMap_353_2048_R1.10_survey_2_ZodiCorrected.fits}}<br />
|-<br />
| '''545GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_survey_1_ZodiCorrected.fits|link=HFI_SkyMap_545_2048_R1.10_survey_1_ZodiCorrected.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_survey_2_ZodiCorrected.fits|link=HFI_SkyMap_545_2048_R1.10_survey_2_ZodiCorrected.fits}}<br />
|-<br />
| '''857GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_857_2048_R1.10_survey_1_ZodiCorrected.fits|link=HFI_SkyMap_857_2048_R1.10_survey_1_ZodiCorrected.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_857_2048_R1.10_survey_2_ZodiCorrected.fits|link=HFI_SkyMap_857_2048_R1.10_survey_2_ZodiCorrected.fits}}<br />
|- bgcolor="ffdead"<br />
! Frequency || Half-ring 1 maps ||Half-ring 2 maps<br />
|-<br />
| '''30GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_030_1024_R1.10_nominal_ringhalf_1.fits|link=LFI_SkyMap_030_1024_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=LFI_SkyMap_030_1024_R1.10_nominal_ringhalf_2.fits|link=LFI_SkyMap_030_1024_R1.10_nominal_ringhalf_2.fits}}<br />
|-<br />
| '''44GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_044_1024_R1.10_nominal_ringhalf_1.fits|link=LFI_SkyMap_044_1024_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=LFI_SkyMap_044_1024_R1.10_nominal_ringhalf_2.fits|link=LFI_SkyMap_044_1024_R1.10_nominal_ringhalf_2.fits}}<br />
|-<br />
| '''70GHz''' || {{PLASingleFile|fileType=map|name=LFI_SkyMap_070_1024_R1.10_nominal_ringhalf_1.fits|link=LFI_SkyMap_070_1024_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=LFI_SkyMap_070_1024_R1.10_nominal_ringhalf_2.fits|link=LFI_SkyMap_070_1024_R1.10_nominal_ringhalf_2.fits}}<br />
|-<br />
| '''100GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_100_2048_R1.10_nominal_ringhalf_1.fits|link=HFI_SkyMap_100_2048_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_100_2048_R1.10_nominal_ringhalf_2.fits|link=HFI_SkyMap_100_2048_R1.10_nominal_ringhalf_2.fits}} ||<br />
|-<br />
| '''143GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_143_2048_R1.10_nominal_ringhalf_1.fits|link=HFI_SkyMap_143_2048_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_143_2048_R1.10_nominal_ringhalf_2.fits|link=HFI_SkyMap_143_2048_R1.10_nominal_ringhalf_2.fits}} ||<br />
|-<br />
| '''217GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_217_2048_R1.10_nominal_ringhalf_1.fits|link=HFI_SkyMap_217_2048_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_217_2048_R1.10_nominal_ringhalf_2.fits|link=HFI_SkyMap_217_2048_R1.10_nominal_ringhalf_2.fits}} ||<br />
|-<br />
| '''353GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_353_2048_R1.10_nominal_ringhalf_1.fits|link=HFI_SkyMap_353_2048_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_353_2048_R1.10_nominal_ringhalf_2.fits|link=HFI_SkyMap_353_2048_R1.10_nominal_ringhalf_2.fits}} ||<br />
|-<br />
| '''545GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_nominal_ringhalf_1.fits|link=HFI_SkyMap_545_2048_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_545_2048_R1.10_nominal_ringhalf_2.fits|link=HFI_SkyMap_545_2048_R1.10_nominal_ringhalf_2.fits}} ||<br />
|-<br />
| '''857GHz''' || {{PLASingleFile|fileType=map|name=HFI_SkyMap_857_2048_R1.10_nominal_ringhalf_1.fits|link=HFI_SkyMap_857_2048_R1.10_nominal_ringhalf_1.fits}} ||<br />
{{PLASingleFile|fileType=map|name=HFI_SkyMap_857_2048_R1.10_nominal_ringhalf_2.fits|link=HFI_SkyMap_857_2048_R1.10_nominal_ringhalf_2.fits}} ||<br />
|}<br />
<br />
== FITS file structure ==<br />
----------------------<br />
<br />
[[File:FITS_FreqMap.png | 500px | right | thumb | '''FITS file structure''']]<br />
<br />
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 at right. <br />
<br />
The ''FREQ-MAP'' extension contains is a 3-column table that contain the signal, hit-count and variance maps, all in Healpix format, in columns 1, 2, and 3, respectively. The number of rows is 50331648 for HFI and 12582912 for LFI, corresponding to the number of pixels in a Healpix map of Nside= 2048 and 1024, respectively (N.B: Npix = 12 Nside^2). The three columns are ''I_STOKES'' for the intensity (or temperature) signal, ''HIT'' for the hit-count and ''II_COV'' for the variance. The exact order of the columns in the figure is indicative only, and the details can be found in the keywords. <br />
<br />
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 as are the datasum and the md5 checksum for the extension. 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 COMMENT fields give further information including some traceability data for the DPC's. The main parameters are summarised below:<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Sky map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'FREQ-MAP' : Data columns<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I_STOKES || Real*4 || K_cmb or MJy/sr || The signal map<br />
|-<br />
|HITS || Int*4 || none || The hit-count map<br />
|-<br />
|II_COV || Real*4 || K_cmb<sup>2</sup> or (MJy/sr)<sup>2</sup> || The variance map<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX ||<br />
|-<br />
|COORDSYS || string || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 or 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 12582911 or 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|FREQ || string || nnn || The frequency channel <br />
|}<br />
<br />
<br />
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).<br />
<br />
<br />
== References ==<br />
---------------<br />
<br />
<biblio force=false><br />
#[[References]]<br />
</biblio><br />
<br />
<br />
[[Category:Mission products|002]]</div>Lviberthttps://wiki.cosmos.esa.int/planckpla/index.php?title=CMB_and_astrophysical_component_maps&diff=7322CMB and astrophysical component maps2013-03-19T17:06:20Z<p>Lvibert: </p>
<hr />
<div>== Overview ==<br />
<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in <cite>#planck2013-p06</cite>.<br />
<br />
==CMB maps==<br />
<br />
Four pipelines have been used to produce maps of the CMB:<br />
Commander-Ruler, NILC, SEVEM and SMICA. The last three have been<br />
delivered as Legacy Archive products.<br />
<br />
<center><br />
<gallery perrow=3 widths=260px heights=170px> <br />
File: CMB-smica.png | SMICA<br />
File: CMB-nilc.png | NILC<br />
File: CMB-sevem.png | SEVEM<br />
</gallery></center><br />
<br />
The front-runner CMB map is the SMICA one. This product is labeled as "Main product" in the Planck Legacy Archive Java interface while the two others (NILC, SEVEM) are labeled as "Additional product".<br />
<br />
The component separation pipelines are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation|CMB and foreground separation]] section and also in Section 3 and Appendices A-D of <cite>#planck2013-p06</cite> {{P2013|12}} and references therein.<br />
<br />
===Product description ===<br />
<br />
; SMICA<br />
<br />
* Principle:<br />
SMICA produces a CMB map by linearly combining all Planck<br />
input channels (from 30 to 857 GHz) with weights which vary with the<br />
multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
<br />
* Resolution (effective beam):<br />
The SMICA map has an effective beam window function of 5 arc-minutes,<br />
deconvolved from the pixel window. It means that, ideally, one would<br />
have <math>C_\ell(map) = C_\ell(sky) * B_{(5')}^2</math>, where<br />
<math>C_\ell(map)</math> is the angular spectrum of the map, where<br />
<math>C_\ell(sky)</math> is the angular spectrum of the CMB and<br />
<math>B_{(5')}</math> is a 5-arcminute Gaussian beam function.<br />
<br />
* Confidence mask:<br />
a confidence mask is provided which excludes some<br />
parts of the Galactic plane, some very bright areas and the masked<br />
point sources.<br />
<br />
* Invalid pixels:<br />
SMICA combines the input maps after some regions with strong emission<br />
have been replaced by a smooth fill-in (in order to mitigate spectral<br />
leakage). This is done over 3% of the sky, as indicated by the field<br />
INPMASK in the SMICA CMB FITS file. See the resulting obvious deficit<br />
of the CMB signal close to the Galactic plane in the above thumbnail.<br />
<br />
<br />
; NILC<br />
<br />
* Principle: <br />
The Needlet-ILC (hereafter NILC) CMB map is constructed<br />
from all Planck channels from 44 to 857 GHz and includes multipoles up<br />
to <math>\ell = 3200</math>. It is obtained by applying the Internal<br />
Linear Combination (ILC) technique in needlet space, that is, with<br />
combination weights which are allowed to vary over the sky and over<br />
the whole multipole range.<br />
<br />
* Confidence mask:<br />
a confidence mask is provided which excludes some<br />
parts of the Galactic plane, some very bright areas and the masked<br />
point sources.<br />
<br />
* Invalid pixels:<br />
The NILC MAP has valid pixels except at point source location (see the NILC description below).<br />
The <span style="color:red">current</span> product contains an "INPMASK" which does<br />
<span style="color:red"> not</span> reflect the actual point-source masking and<br />
<span style="color:red">should be ignored</span>.<br />
<br />
<br />
; SEVEM<br />
<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations Leach et al., 2008 <cite>#leach2008</cite> and to WMAP polarisation data Fernandez-Cobos et al., 2012 <cite>xx</cite>. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.<br />
<br />
<br />
===Production process===<br />
<br />
; SMICA<br />
<br />
Some implementation details about the SMICA products.<br />
<br />
The SMICA map is a combination of all nine Planck frequency channels<br />
from 30 to 857 GHz, harmonically transformed up to <math>\ell = 4000<br />
</math>.<br />
<br />
Before applying the SMICA weights in the harmonic domain, the input<br />
maps undergo a pre-processing step to deal with point sources. The<br />
point sources with SNR > 5 in the PCCS catalogue are fitted in each<br />
input map. If the fit is successful, the fitted point source is<br />
removed from the map; otherwise it is masked and the hole is<br />
in-painted by a simple diffusive process to ensure a smooth transition<br />
and mitigate spectral leakage. This is done at all frequencies but 545<br />
and 857 GHz, where all point sources with SNR > 7.5 are masked and<br />
in-painted.<br />
<br />
Viewed as a filter, SMICA can be summarized by the weights<br />
<math>\mathbf{w}_\ell</math> applied to each input map as a function<br />
of multipole. In this sense, SMICA is strictly equivalent to co-adding<br />
the input maps after convolution by specific axi-symmetric kernels<br />
directly related to the corresponding entry of<br />
<math>\mathbf{w}_\ell</math>. The SMICA weights used here are shown in<br />
the figure below for input maps in units of<br />
K<math>_\rm{RJ}</math>. They show, in particular, the (expected)<br />
progressive attenuation of the lowest resolution channels with<br />
increasing multipole.<br />
<br />
[[File:smica.jpg|thumb|center|600px|'''Weights <math>w_\ell</math> given by SMICA to the input maps, after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
<br />
; NILC<br />
<br />
The NILC method combines linearly input maps varying over the sky and<br />
over multipoles. In the needlet framework, harmonic localisation is<br />
achieved using a set of bandpass filters defining ‘scales’ and spatial<br />
localization is achieved, at each scale, by defining zones over the<br />
sky. The harmonic localisation used here uses 9 spectral bands<br />
covering multipoles up to <math>\ell</math> = 3200 (see figure<br />
below). The spatial localisation depends on the scale: at the coarsest<br />
scale, which include the multipoles of lowest degree, we use a single<br />
zone (no localization) while at the finest scales (which include the<br />
highest degree multipoles), the sky is partitioned in up to 20 zones<br />
(again, see figure below).<br />
<br />
<center><br />
<gallery perrow=2 widths=300px heights=180px><br />
File:Nilc1.jpg | Spectral window functions defining nine ''needlet scales''<br />
File:Nilc2.jpg | The 2-zone partition for scale 2.<br />
File:Nilc3.jpg | The 4-zone partition for scale 3.<br />
File:Nilc4.jpg | The 20-zone partition for scales 5 to 9.<br />
</gallery><br />
</center><br />
<br />
The actual processing differs from the above scenario in several respects: pre-processing of point sources, dealing with frequency-dependent beams, and dealing with statistical issues (the ILC bias) in the coarsest scale.<br />
* ''Pre-processing of point sources''. Identical to the SMICA pre-processing.<br />
* ''Masking and inpainting''. The NILC CMB map is actually produced in a two step process. In a first step, the NILC weights are computed from needlet statistics evaluated using a Galactic mask which covers about 98% of the sky (and is apodiwed at 1 degree). In a second step, those NILC weights on are applied to needlet coefficients computed over the whole sky (the point sources having been subtracted or fitted at the pre-processing stage), yielding a NILC CMB estimate over the whole sky, except for the point source mask. <br />
* ''ILC bias and spectral statistics for the coarsest scale''. The coarsest scale of the NILC filter is not localized. Therefore, the NILC map at the coarsest scale is equivalent to a plain pixel-based ILC which is known to be quite susceptible to an ‘ILC bias’ due to chance correlations between the CMB and foregrounds. In order to mitigate that effect, the covariance matrix which determines the ILC coefficients at the coarsest scale is not computed as a pixel average but is rather estimated in the spectral domain with a spectral weight which equalizes the power of the CMB modes (based on a fiducial spectrum).<br />
<br />
<br />
For more details, see <cite>#planck2013-p06</cite>.<br />
<br />
; SEVEM<br />
<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization; Casaponsa et al. 2011 <cite>#Casaponsa2011</cite>) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky:<br />
<br />
:<math> \label{eq:eq4}<br />
T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x})<br />
</math><br />
<br />
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
An additional level of flexibility can also be considered: the linear coefficients can be the same for all the sky, or several regions with different sets of coefficients can be considered. The regions are then combined in a smooth way, by weighting the pixels at the boundaries, to avoid discontinuities in the clean maps.<br />
Since the method is linear, we may easily propagate the noise properties to the final CMB map. Moreover, it is very fast and permits the generation of thousands of simulations to character- ize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
In particular, we have cleaned the 143 GHz and 217 GHz maps using four templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and (857-545). For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). In order to take into account the different spectral behaviour of the foregrounds at low and high galactic latitudes, we have considered two independent regions of the sky, for which we have used a different set of coefficients. The first region corresponds to the 3 per cent brightest Galactic emission, whereas the second region is defined by the remaining 97 per cent of the sky. For the first region, the coefficients are actually estimated over the whole sky (we find that this is more optimal than perform the minimisation only on the 3 per cent brightest region, where the CMB emission is very sub-dominant) while for the second region, we exclude the 3 per cent brightest region of the sky, point sources detected at any frequency and those pixels which have not been observed at all channels.<br />
Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
Moreover, additional CMB clean maps (at frequencies between 44 and 353 GHz) have also been produced using different combinations of templates for some of the analyses carried out in <cite>#planck2013-p09</cite> {{P2013|23}} and <cite>#planck2013-p14</cite> {{P2013|19}}. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in <cite>#planck2013-p14</cite>, while frequencies from 70 to 217 GHz were used for consistency tests in <cite>#planck2013-p09</cite>.<br />
<br />
The method has been successfully applied to Planck simulations <cite>#leach2008</cite> and to WMAP polarisation data <cite>#Fernandez-Cobos2012</cite>.<br />
<br />
===Inputs===<br />
<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. <br />
<br />
; SMICA<br />
<br />
SMICA uses all nine Planck frequency channels from 30 to 857 GHz. SMICA uses a pre-processing step in which point sources are subtracted or masked as described above.<br />
<br />
; NILC<br />
<br />
NILC uses eight frequency channels from 44 to 857 GHz and the same pre-processing step as SMICA.<br />
<br />
; SEVEM <br />
<br />
SEVEM uses all nine Planck frequency channel maps. The 30 - 70 GHz and 353 - 857 GHz maps are used to construct templates by taking the differences (30 - 44) GHz, (44 - 70) GHz, (545 - 353) GHz and (857 - 545) GHz, after smoothing to a common resolution. The 100, 143 and 217 GHz maps are cleaned using the templates.<br />
<br />
<br />
===File names and structure===<br />
<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.11.fits|link=COM_CompMap_CMB-nilc_2048_R1.11.fits}}<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.11.fits|link=COM_CompMap_CMB-sevem_2048_R1.11.fits}}<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.11.fits|link=COM_CompMap_CMB-smica_2048_R1.11.fits}}<br />
<br />
<br />
The files contains a minimal primary extension with no data and four data extensions which are described in the table below:<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || The CMB temperature map<br />
|-<br />
|NOISE || Real*4 || uK_cmb || Estimated noise map (Note 1)<br />
|-<br />
|VALMASK|| Byte || none || Validity, or confidence mask (note 2)<br />
|-<br />
|INPMASK || Byte || none || <span style="color:red"> Inpainted mask (Optional - see Note 3) </span> <br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''FGDS-LFI'' (BINTABLE) - Note 4<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|LFI_030 || Real*4 || K_cmb || 30 GHz foregrounds<br />
|-<br />
|LFI_044 || Real*4 || K_cmb || 44 GHz foregrounds<br />
|-<br />
|LFI_070 || Real*4 || K_cmb || 70 GHz foregrounds<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 3. EXTNAME = ''FGDS-HFI'' (BINTABLE) - Note 4<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|HFI_100 || Real*4 || K_cmb || 100 GHz foregrounds<br />
|-<br />
|HFI_143 || Real*4 || K_cmb || 143 GHz foregrounds<br />
|-<br />
|HFI_217 || Real*4 || K_cmb || 217 GHz foregrounds<br />
|-<br />
|HFI_353 || Real*4 || K_cmb || 353 GHz foregrounds<br />
|-<br />
|HFI_545 || Real*4 || MJy/sr || 545 GHz foregrounds<br />
|-<br />
|HFI_857 || Real*4 || MJy/sr || 857 GHz foregrounds<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || uK_cmb || The CMB temperature map<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|}<br />
<br />
<br />
Notes:<br />
# The half-ring half-difference (HRHD) map is made by passing the half-ring frequency maps independently through the component separation pipeline, then computing half their difference. It approximates a noise realisation, and gives an indication of the uncertainties due to instrumental noise in the corresponding CMB map. <br />
# The confidence mask indicates where the CMB map is considered valid. <br />
# In the SMICA map, the CMB values have not been computed over 3% of the sky (point sources and bright regions of the sky) as indicated in the INPMASK column. This column is not correctly set in the NILC product file and must be ignored. This column is not present in the SEVEM product file.<br />
# The subtraction of the CMB from the sky maps in order to produce the foregrounds map is done after convolving the CMB map to the resolution of the given frequency.<br />
<br />
===Cautionary notes===<br />
<br />
# The half-ring CMB maps are produced by the pipelines with parameters/weights fixed to the values obtained from the full maps. Therefore the CMB HRHD maps do not capture all of the uncertainties due to foreground modelling on large angular scales.<br />
# The HRHD maps for the HFI frequency channels underestimate the noise power spectrum at high l by typically a few percent. This is caused by correlations induced in the pre-processing to remove cosmic ray hits. The CMB is mostly constrained by the HFI channels at high l, and so the CMB HRHD maps will inherit this deficiency in power.<br />
# The beam transfer functions do not account for uncertainties in the beams of the frequency channel maps.<br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper <cite>#planck2013-p06</cite> {{P2013|12}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper <cite>#planck2013-p06</cite> {{p2013|12}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
<br />
None. <br />
<br />
===File names===<br />
<br />
* Low frequency component at N$_\rm{side}$ 256: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
<br />
* Mask: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
<br />
====Low frequency foreground component====<br />
<br />
=====Low frequency component at N$_\rm{side}$ 256=====<br />
<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<math>_{CMB}</math>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
Below an example of the header. <br />
<!--pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 16 / width of table in bytes<br />
NAXIS2 = 786432 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'uK_CMB ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT2 = 'uK_CMB ' / physical unit of field<br />
TTYPE3 = 'Beta ' / label for field 3<br />
TFORM3 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT3 = 'none ' / physical unit of field<br />
TTYPE4 = 'B_stdev ' / label for field 4<br />
TFORM4 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT4 = 'none ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-13T13:26:14' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'QXaaRVZTQVaZQVYZ' / HDU checksum updated 2013-02-13T13:26:14<br />
DATASUM = '2752450756' / data unit checksum updated 2013-02-13T13:26:14<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 256 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 786431 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity is normalized at 30GHz<br />
COMMENT The intensity was estimated during mixing matrix estimation<br />
COMMENT Object:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_stddev.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
=====Low frequency component at N$_\rm{side}$ 2048=====<br />
<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<math>_{CMB}</math>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<math>_{CMB}</math> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
Below an example of the header of the first and second extension respectively. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 32 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT1 = 'uK_CMB ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT2 = 'uK_CMB ' / physical unit of field<br />
TTYPE3 = 'I_hr1 ' / label for field 3<br />
TFORM3 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT3 = 'uK_CMB ' / physical unit of field<br />
TTYPE4 = 'I_hr2 ' / label for field 4<br />
TFORM4 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT4 = 'uK_CMB ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-15T17:12:04' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'dlA5ei24di94di94' / HDU checksum updated 2013-02-15T17:12:13<br />
DATASUM = '3117718572' / data unit checksum updated 2013-02-15T17:12:13<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity was computed after mixibg matrix application<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_lowfreq.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_lowfreq_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_lowfreq.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_lowfreq.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre><br />
<br />
<pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 1501 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'BeamWF ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'BeamWF '<br />
DATE = '2013-02-15T17:12:17' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '74GA849274E97499' / HDU checksum updated 2013-02-15T17:12:17<br />
DATASUM = '3098248385' / data unit checksum updated 2013-02-15T17:12:17<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
MAX-LPOL= 1500 / Maximum L multipole<br />
POLAR = T / Polarization included (True/False)<br />
BCROSS = T / Magnetic cross terms included (True/False)<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity was computed after mixing matrix application<br />
COMMENT<br />
COMMENT Objects used:<br />
COMMENT<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_beams/dx9_delta_v1_7b_lowfreq_beam.fits<br />
COMMENT<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
====Thermal dust====<br />
<br />
=====Thermal dust component at N$_\rm{side}$=256=====<br />
<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<math>_{CMB}</math> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
Below an example of the header. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 24 / width of table in bytes<br />
NAXIS2 = 786432 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 6 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'MJy/sr ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT2 = 'MJy/sr ' / physical unit of field<br />
TTYPE3 = 'Em ' / label for field 3<br />
TFORM3 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT3 = 'uK_CMB ' / physical unit of field<br />
TTYPE4 = 'Em_stdev' / label for field 4<br />
TFORM4 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT4 = 'none ' / physical unit of field<br />
TTYPE5 = 'T ' / label for field 5<br />
TFORM5 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT5 = 'uK_CMB ' / physical unit of field<br />
TTYPE6 = 'T_stdev ' / label for field 6<br />
TFORM6 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT6 = 'uK_CMB ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-13T13:31:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '9OAOJO7N9OANGO7N' / HDU checksum updated 2013-02-13T13:31:15<br />
DATASUM = '4139938263' / data unit checksum updated 2013-02-13T13:31:15<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 256 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 786431 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_dust-commrul_0256_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity is normalized at 353 GHz<br />
COMMENT Object:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_stddev.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
=====Thermal dust component at N$_\rm{side}$=2048=====<br />
<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
Below an example of the header of the first and second extension respectively. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 32 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT1 = 'MJy/sr ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT2 = 'MJy/sr ' / physical unit of field<br />
TTYPE3 = 'I_hr1 ' / label for field 3<br />
TFORM3 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT3 = 'MJy/sr ' / physical unit of field<br />
TTYPE4 = 'I_hr2 ' / label for field 4<br />
TFORM4 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT4 = 'MJy/sr ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-16T10:23:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '6k8A7i826i896i89' / HDU checksum updated 2013-02-16T10:23:32<br />
DATASUM = '3817117839' / data unit checksum updated 2013-02-16T10:23:32<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_dust-commrul_2048_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_dust_flux.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_dust_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_dust_flux.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_dust_flux.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre><br />
<br />
<pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 3001 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'BeamWF ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'BeamWF '<br />
DATE = '2013-02-16T10:23:34' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'FBGWI9EWFAEWF7EW' / HDU checksum updated 2013-02-16T10:23:34<br />
DATASUM = '4096860189' / data unit checksum updated 2013-02-16T10:23:34<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
MAX-LPOL= 3000 / Maximum L multipole<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Beam window function used in the Component separation process<br />
COMMENT<br />
COMMENT Objects used:<br />
COMMENT<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_beams/dx9_delta_v1_7b_dust_beam.fits<br />
COMMENT<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
====Sky mask====<br />
<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
Below an example of the header. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'Mask ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-16T21:07:43' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '5fQAAeQ45eQAAeQ3' / HDU checksum updated 2013-02-16T21:07:44<br />
DATASUM = '1075621420' / data unit checksum updated 2013-02-16T21:07:44<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
OBJECT = 'FULLSKY ' / Sky coverage, either FULLSKY or PARTIAL<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Mask-rulerminimal_2048.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_masks/deltadx9_ruler_mask_total_minimal.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
== Dust optical depth map and model ==<br />
<br />
Thermal emission from interstellar dust is captured by Planck-HFI over the whole sky, at all frequencies from 100 to 857 GHz. This emission is well modelled by a modified black body in the far-infrared to millimeter range. It is produced by the biggest interstellar dust grain that are in thermal equilibrium with the radiation field from stars. The grains emission properties in the sub-millimeter are therefore directly linked to their absorption properties in the UV-visible range. By modelling the thermal dust emission in the sub-millimeter, a map of dust reddening in the visible can then be constructed. <br />
<br />
; Model of thermal dust emission<br />
<br />
The model of the thermal dust emission is based on a modify black body fit to the data $I_\nu$<br />
<br />
$I_\nu = A\, B_\nu(T)\, \nu^\beta$<br />
<br />
where B_nu(T) is the Planck function for dust equilibirum temperature T, A is the amplitude of the MBB and beta the dust spectral index. The dust optical depth at frequency nu is<br />
<br />
$\tau_\nu = I_\nu / B_\nu(T) = A\, \nu^\beta$<br />
<br />
The dust parameters provided are $T$, beta and $\tau_{353}$. They were obtained by fitting the Planck data at 353, 545 and 857 GHz together with the IRAS (IRIS) 100 micron data. All maps (in Healpix N$_\rm{side}$=2048) were smoothed to a common resolution of 5 arcmin. The CMB anisotropies, clearly visible at 353 GHz, were removed from all the HFI maps using the SMICA map. An offset was removed from each map to obtained a meaningful Galactic zero level, using a correlation with the LAB 21 cm data in diffuse areas of the sky ($N_{HI} < 2\times10^{20} cm^{-2}$). Because the dust emission is so well correlated between frequencies in the Rayleigh-Jeans part of the dust spectrum, the zero level of the 545 and 353 GHz were improved by correlating with the 857 GHz over a larger mask ($N_{HI} < 3\times10^{20} cm^{-2}$). Faint residual dipole structures, identified in the 353 and 545 GHz maps, were removed prior to the fit.<br />
<br />
The MBB fit was performed using a chi-square minimization, assuming errors for each data point that include instrumental noise, calibration uncertainties (on both the dust emission and the CMB anisotropies) and uncertainties on the zero level. Because of the known degeneracy between $T$ and $\beta$ in the presence of noise, we produced a model of dust emission using data smoothed to 35 arcmin; at such resolution no systematic bias of the parameters is observed. The map of the spectral index $\beta$ at 35 arcmin was than used to fit the data for $T$ and $\tau_{353}$ at 5 arcmin. <br />
<br />
; The $E(B-V)$ map <br />
For the production of the $E(B-V)$ map, we used Planck and IRAS data from which point sources in diffuse areas were removed to avoid contamination by galaxies. In the hypothesis of constant dust emission cross-section, the optical depth map $\tau_{353}$ is proportional to dust column density. It can then be used to estimate E(B-V), also proportional to dust column density in the hypothesis of a constant differential absorption cross-section between the B and V bands. Given those assumptions, $ E(B-V) = q\, \tau_{353}$.<br />
<br />
To estimate the calibration factor q, we followed a method similar to <cite>#mortsell2013</cite> based on SDSS reddening measurements ($E(g-r)$ which corresponds closely to $E(B-V)$) of 77 429 Quasars <cite>#schneider2007</cite>. The interstellar HI column densities covered on the lines of sight of this sample ranges from $0.5$ to $10\times10^{20}\,cm^{-2}$. Therefore this sample allows to estimate q in the diffuse ISM where dust properties are expected to vary less than in denser clouds where coagulation and grain growth might modify dust emission and absorption cross sections. <br />
<br />
; Dust optical depth products<br />
<br />
The characteristics of the dust model maps are the following.<br />
* Dust optical depth at 353 GHz : N$_\rm{side}$=2048, fwhm=5 arcmin, no units<br />
* Dust reddening E(B-V) : N$_\rm{side}$=2048, fwhm=5 arcmin, units=magnitude, obtained with data from which point sources were removed.<br />
* Dust temperature : N$_\rm{side}$ 2048, fwhm=5 arcmin, units=Kelvin<br />
* Dust spectral index : N$_\rm{side}$=2048, fwhm=35 arcmin, no units<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Dust opacity file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
| TAU353 || Real*4 || none || The opacity at 353GHz<br />
|-<br />
| TAU353ERR || Real*4 || none || Error in the opacity<br />
|-<br />
| EBV || Real*4 || mag || E(B-V)<br />
|-<br />
| EBV_ERR || Real*4 || mag || Error in E(B-V)<br />
|-<br />
|T_HF || Real*4 || K || Temperature for the high frequency correction<br />
|-<br />
|T_HF_ERR || Real*4 || K || Error on the temperature<br />
|-<br />
| BETAHF || Real*4 || none || Beta for the high frequency correction<br />
|-<br />
| BETAHFERR || Real*4 || none || Error on beta<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
| AST-COMP || String || DUST-OPA|| Astrophysical compoment name<br />
|-<br />
| PIXTYPE || String || HEALPIX ||<br />
|-<br />
| COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
| ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
| NSIDE || Int || 2048 || Healpix N$_\rm{side}$ for LFI and HFI, respectively<br />
|-<br />
| FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
| LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|}<br />
<br />
== CO emission maps ==<br />
<br />
CO rotational transition line emission is present in all HFI bands but for the 143 GHz channel. It is especially significant in the 100, 217 and 353 GHz channels (due to the 115 (1-0), 230 (2-1) and 345 GHz (3-2) CO transitions). This emission comes essentially from the Galactic interstellar medium and is mainly located at low and intermediate Galactic latitudes. Three approaches (summarised below) have been used to extract CO velocity-integrated emission maps from HFI maps and to make three types of CO products. An introduction is given in [[Science#CO_maps|Section]] and a full description of these products is given in <cite>#planck2013-p03a</cite>.<br />
* Type 1 product: it is based on a single channel approach using the fact that each CO line has a slightly different transmission in each bolometer at a given frequency channel. These transmissions can be evaluated from bandpass measurements that were performed on the ground or empirically determined from the sky using existing ground-based CO surveys. From these, the J=1-0, J=2-1 and J=3-2 CO lines can be extracted independently. As this approach is based on individual bolometer maps of a single channel, the resulting Signal-to-Noise ratio (SNR) is relatively low. The benefit, however, is that these maps do not suffer from contamination from other HFI channels (as is the case for the other approaches) and are more reliable, especially in the Galactic Plane.<br />
<br />
* Type 2 product: this product is obtained using a multi frequency approach. Three frequency channel maps are combined to extract the J=1-0 (using the 100, 143 and 353 GHz channels) and J=2-1 (using the 143, 217 and 353 GHz channels) CO maps. Because frequency channels are combined, the spectral behaviour of other foregrounds influences the result. The two type 2 CO maps produced in this way have a higher SNR than the type 1 maps at the cost of a larger possible residual contamination from other diffuse foregrounds.<br />
<br />
* Type 3 product: using prior information on CO line ratios and a multi-frequency component separation method, we construct a combined CO emission map with the largest possible SNR. This type 3 product can be used as a sensitive finder chart for low-intensity diffuse CO emission over the whole sky.<br />
<br />
The released Type 1 CO maps have been produced using the MILCA-b algorithm, Type 2 maps using a specific implementation of the Commander algorithm, and the Type 3 map using the full Commander-Ruler component separation pipeline (see [[Astrophysical_component_maps#Maps_of_astrophysical_foregrounds|above]]).<br />
<br />
Characteristics of the released maps are the following. We provide Healpix maps with N$_\rm{side}$=2048. For one transition, the CO velocity-integrated line signal map is given in K_RJ.km/s units. A conversion factor from this unit to the native unit of HFI maps (K_CMB) is provided in the header of the data files and in the RIMO. Four maps are given per transition and per type:<br />
* The signal map<br />
* The standard deviation map (same unit as the signal), <br />
* A null test noise map (same unit as the signal) with similar statistical properties. It is made out of half the difference of half-ring maps.<br />
* A mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.<br />
<br />
All products of a given type belong to a single file.<br />
Type 1 products have the native HFI resolution i.e. approximately 10, 5 and 5 arcminutes for the CO 1-0, 2-1, 3-2 transitions respectively.<br />
Type 2 products have a 15 arcminute resolution<br />
The Type 3 product has a 5.5 arcminute resolution.<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-1 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map<br />
|-<br />
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity<br />
|-<br />
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable<br />
|-<br />
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map<br />
|-<br />
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity<br />
|-<br />
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable<br />
|-<br />
|I32 || Real*4 || K_RJ km/sec || The CO(3-2) intensity map<br />
|-<br />
|E32 || Real*4 || K_RJ km/sec || Uncertainty in the CO(3-2) intensity<br />
|-<br />
|N32 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M32 || Byte || none || Region over which the CO(3-2) intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || string || CO-TYPE2 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix N$_\rm{side}$ for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 3-2 || Real*4 || value || Factor to convert CO(3-2) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-2 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map<br />
|-<br />
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity<br />
|-<br />
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable<br />
|-<br />
|-<br />
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map<br />
|-<br />
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity<br />
|-<br />
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CO-TYPE2 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-3 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|INTEN || Real*4 || K_RJ km/sec || The CO intensity map<br />
|-<br />
|ERR || Real*4 || K_RJ km/sec || Uncertainty in the intensity<br />
|-<br />
|NUL || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|MASK || Byte || none || Region over which the intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CO-TYPE1 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV || Real*4 || value || Factor to convert to Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
== References ==<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Lviberthttps://wiki.cosmos.esa.int/planckpla/index.php?title=CMB_and_astrophysical_component_maps&diff=7321CMB and astrophysical component maps2013-03-19T15:21:48Z<p>Lvibert: </p>
<hr />
<div>== Overview ==<br />
<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in <cite>#planck2013-p06</cite>.<br />
<br />
==CMB maps==<br />
<br />
Four pipelines have been used to produce maps of the CMB: Commander-Ruler, NILC, SEVEM and SMICA. The last three have been delivered as Legacy Archive products.<br />
<br />
The front-runner CMB map is the SMICA one. This product is labeled as "Main product" in the Planck Legacy Archive Java interface while the two others (NILC, SEVEM) are labeled as "Additional product".<br />
<br />
The component separation pipelines are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation|CMB and foreground separation]] section and also in Section 3 and Appendices A-D of <cite>#planck2013-p06</cite> {{P2013|12}} and references therein.<br />
<br />
===Product description ===<br />
<br />
; SMICA<br />
<br />
* Principle:<br />
SMICA produces a CMB map by linearly combining all Planck<br />
input channels (from 30 to 857 GHz) with weights which vary with the<br />
multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
<br />
* Resolution (effective beam):<br />
The SMICA map has an effective beam window function of 5 arc-minutes,<br />
deconvolved from the pixel window. It means that, ideally, one would<br />
have <math>C_\ell(map) = C_\ell(sky) * B_{(5')}^2</math>, where<br />
<math>C_\ell(map)</math> is the angular spectrum of the map, where<br />
<math>C_\ell(sky)</math> is the angular spectrum of the CMB and<br />
<math>B_{(5')}</math> is a 5-arcminute Gaussian beam function.<br />
<br />
* Confidence mask:<br />
a confidence mask is provided which excludes some<br />
parts of the Galactic plane, some very bright areas and the masked<br />
point sources.<br />
<br />
* Undefined pixels:<br />
The SMICA map has valid pixels over 97% of the<br />
sky: a binary mask describing the valid pixels is provided (as the 4th<br />
column of the FITS file). The 3% invalid pixels are not set to zero<br />
(or to some NaN value): their values result from the pre-processing<br />
step in which this area is filled-in by a smooth field in order to<br />
avoid spectral leakage. <br />
<br />
<br />
<br />
; NILC<br />
<br />
* Principle: <br />
The Needlet-ILC (hereafter NILC) CMB map is constructed<br />
from all Planck channels from 44 to 857 GHz and includes multipoles up<br />
to <math>\ell = 3200</math>. It is obtained by applying the Internal<br />
Linear Combination (ILC) technique in needlet space, that is, with<br />
combination weights which are allowed to vary over the sky and over<br />
the whole multipole range.<br />
<br />
* Confidence mask:<br />
a confidence mask is provided which excludes some<br />
parts of the Galactic plane, some very bright areas and the masked<br />
point sources.<br />
<br />
* Undefined pixels:<br />
The NILC data structure contains an "INPMASK" '''which should be ignored'''.<br />
<br />
<br />
; SEVEM<br />
<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations Leach et al., 2008 <cite>#leach2008</cite> and to WMAP polarisation data Fernandez-Cobos et al., 2012 <cite>xx</cite>. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.<br />
<br />
<br />
===Production process===<br />
<br />
; SMICA<br />
<br />
Some implementation details about the SMICA products.<br />
<br />
All nine Planck frequency channels from 30 to 857 GHz, harmonically transformed up to <math>\ell = 4000 </math>.<br />
<br />
<br />
Before applying the SMICA weights in the harmonic domain, the input<br />
maps undergo a pre-processing step to deal with point sources. The<br />
point sources with SNR > 5 in the PCCS catalogue are fitted in each<br />
input map. If the fit is successful, the fitted point source is<br />
removed from the map; otherwise it is masked and the hole is<br />
in-painted by a simple diffusive process to ensure a smooth transition<br />
and mitigate spectral leakage. This is done at all frequencies but 545<br />
and 857 GHz, where all point sources with SNR > 7.5 are masked and<br />
in-painted.<br />
<br />
Viewed as a filter, SMICA can be summarized by the weights<br />
<math>\mathbf{w}_\ell</math> applied to each input map as a function<br />
of multipole. In this sense, SMICA is strictly equivalent to co-adding<br />
the input maps after convolution by specific axi-symmetric kernels<br />
directly related to the corresponding entry of<br />
<math>\mathbf{w}_\ell</math>. The SMICA weights used here are shown in<br />
the figure below for input maps in units of<br />
K<math>_\rm{RJ}</math>. They show, in particular, the (expected)<br />
progressive attenuation of the lowest resolution channels with<br />
increasing multipole.<br />
<br />
[[File:smica.jpg|thumb|center|600px|'''Weights <math>w_\ell</math> given by SMICA to the input maps, after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
<br />
; NILC<br />
<br />
The NILC method combines linearly input maps varying over the sky and<br />
over multipoles. In the needlet framework, harmonic localisation is<br />
achieved using a set of bandpass filters defining ‘scales’ and spatial<br />
localization is achieved, at each scale, by defining zones over the<br />
sky. The harmonic localisation used here uses 9 spectral bands<br />
covering multipoles up to <math>\ell</math> = 3200 (see figure<br />
below). The spatial localisation depends on the scale: at the coarsest<br />
scale, which include the multipoles of lowest degree, we use a single<br />
zone (no localization) while at the finest scales (which include the<br />
highest degree multipoles), the sky is partitioned in up to 20 zones<br />
(again, see figure below).<br />
<br />
<center><br />
<gallery perrow=2 widths=300px heights=180px><br />
File:Nilc1.jpg | Spectral window functions defining nine ''needlet scales''<br />
File:Nilc2.jpg | The 2-zone partition for scale 2.<br />
File:Nilc3.jpg | The 4-zone partition for scale 3.<br />
File:Nilc4.jpg | The 20-zone partition for scales 5 to 9.<br />
</gallery><br />
</center><br />
<br />
The actual processing differs from the above scenario in several respects: pre-processing of point sources, dealing with frequency-dependent beams, and dealing with statistical issues (the ILC bias) in the coarsest scale.<br />
* ''Pre-processing of point sources''. Identical to the SMICA pre-processing.<br />
* ''Masking and inpainting''. The NILC CMB map is actually produced in a two step process. In a first step, the NILC weights are computed from needlet statistics evaluated using a Galactic mask which covers about 98% of the sky (and is apodiwed at 1 degree). In a second step, those NILC weights on are applied to needlet coefficients computed over the whole sky (the point sources having been subtracted or fitted at the pre-processing stage), yielding a NILC CMB estimate over the whole sky, except for the point source mask. <br />
* ''ILC bias and spectral statistics for the coarsest scale''. The coarsest scale of the NILC filter is not localized. Therefore, the NILC map at the coarsest scale is equivalent to a plain pixel-based ILC which is known to be quite susceptible to an ‘ILC bias’ due to chance correlations between the CMB and foregrounds. In order to mitigate that effect, the covariance matrix which determines the ILC coefficients at the coarsest scale is not computed as a pixel average but is rather estimated in the spectral domain with a spectral weight which equalizes the power of the CMB modes (based on a fiducial spectrum).<br />
* ''Using SMICA recalibration''. In our current rendering, the NILC uses for the CMB emission law the values determined by SMICA.<br />
<br />
For more details, see <cite>#planck2013-p06</cite>.<br />
<br />
; SEVEM<br />
<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization; Casaponsa et al. 2011 <cite>#Casaponsa2011</cite>) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky:<br />
<br />
:<math> \label{eq:eq4}<br />
T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x})<br />
</math><br />
<br />
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
An additional level of flexibility can also be considered: the linear coefficients can be the same for all the sky, or several regions with different sets of coefficients can be considered. The regions are then combined in a smooth way, by weighting the pixels at the boundaries, to avoid discontinuities in the clean maps.<br />
Since the method is linear, we may easily propagate the noise properties to the final CMB map. Moreover, it is very fast and permits the generation of thousands of simulations to character- ize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
In particular, we have cleaned the 143 GHz and 217 GHz maps using four templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and (857-545). For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). In order to take into account the different spectral behaviour of the foregrounds at low and high galactic latitudes, we have considered two independent regions of the sky, for which we have used a different set of coefficients. The first region corresponds to the 3 per cent brightest Galactic emission, whereas the second region is defined by the remaining 97 per cent of the sky. For the first region, the coefficients are actually estimated over the whole sky (we find that this is more optimal than perform the minimisation only on the 3 per cent brightest region, where the CMB emission is very sub-dominant) while for the second region, we exclude the 3 per cent brightest region of the sky, point sources detected at any frequency and those pixels which have not been observed at all channels.<br />
Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
Moreover, additional CMB clean maps (at frequencies between 44 and 353 GHz) have also been produced using different combinations of templates for some of the analyses carried out in <cite>#planck2013-p09</cite> {{P2013|23}} and <cite>#planck2013-p14</cite> {{P2013|19}}. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in <cite>#planck2013-p14</cite>, while frequencies from 70 to 217 GHz were used for consistency tests in <cite>#planck2013-p09</cite>.<br />
<br />
The method has been successfully applied to Planck simulations <cite>#leach2008</cite> and to WMAP polarisation data <cite>#Fernandez-Cobos2012</cite>.<br />
<br />
===Inputs===<br />
<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. <br />
<br />
; SMICA<br />
<br />
SMICA uses all nine Planck frequency channels from 30 to 857 GHz. SMICA uses a pre-processing step in which point sources are subtracted or masked as described above.<br />
<br />
; NILC<br />
<br />
NILC uses eight frequency channels from 44 to 857 GHz and the same pre-processing step as SMICA.<br />
<br />
; SEVEM <br />
<br />
SEVEM uses all nine Planck frequency channel maps. The 30 - 70 GHz and 353 - 857 GHz maps are used to construct templates by taking the differences (30 - 44) GHz, (44 - 70) GHz, (545 - 353) GHz and (857 - 545) GHz, after smoothing to a common resolution. The 100, 143 and 217 GHz maps are cleaned using the templates.<br />
<br />
<br />
===File names and structure===<br />
<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.11.fits|link=COM_CompMap_CMB-nilc_2048_R1.11.fits}}<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.11.fits|link=COM_CompMap_CMB-sevem_2048_R1.11.fits}}<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.11.fits|link=COM_CompMap_CMB-smica_2048_R1.11.fits}}<br />
<br />
and the CMB they contain is shows below.<br />
<br />
<center><br />
<gallery perrow=3 widths=260px heights=170px> <br />
File: CMB-smica.png | SMICA<br />
File: CMB-nilc.png | NILC<br />
File: CMB-sevem.png | SEVEM<br />
</gallery></center><br />
<br />
<br />
The files contains a minimal primary extension with no data and four data extensions which are described in the table below:<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || The CMB temperature map<br />
|-<br />
|NOISE || Real*4 || uK_cmb || Estimated noise map (Note 1)<br />
|-<br />
|VALMASK|| Byte || none || Validity, or confidence mask (note 2)<br />
|-<br />
|INPMASK || Byte || none || Inpainted mask (Optional - see Note 3) <br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''FGDS-LFI'' (BINTABLE) - Note 4<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|LFI_030 || Real*4 || K_cmb || 30 GHz foregrounds<br />
|-<br />
|LFI_044 || Real*4 || K_cmb || 44 GHz foregrounds<br />
|-<br />
|LFI_070 || Real*4 || K_cmb || 70 GHz foregrounds<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 3. EXTNAME = ''FGDS-HFI'' (BINTABLE) - Note 4<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|HFI_100 || Real*4 || K_cmb || 100 GHz foregrounds<br />
|-<br />
|HFI_143 || Real*4 || K_cmb || 143 GHz foregrounds<br />
|-<br />
|HFI_217 || Real*4 || K_cmb || 217 GHz foregrounds<br />
|-<br />
|HFI_353 || Real*4 || K_cmb || 353 GHz foregrounds<br />
|-<br />
|HFI_545 || Real*4 || MJy/sr || 545 GHz foregrounds<br />
|-<br />
|HFI_857 || Real*4 || MJy/sr || 857 GHz foregrounds<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || uK_cmb || The CMB temperature map<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|}<br />
<br />
<br />
Notes:<br />
# The half-ring half-difference (HRHD) map is made by passing the half-ring frequency maps independently through the component separation pipeline, then computing half their difference. It approximates a noise realisation, and gives an indication of the uncertainties due to instrumental noise in the corresponding CMB map. <br />
# The confidence mask indicates where the CMB map is considered valid. <br />
# NILC and SMICA CMB maps have been inpainted in the Galactic plane and around some bright sources with a constrained realisation of the signal. The inpainted area covers approximately 3% of the sky. This column is not present in the SEVEM product file.<br />
# The subtraction of the CMB from the sky maps in order to produce the foregrounds map is done after convolving the CMB map to the resolution of the given frequency.<br />
<br />
===Cautionary notes===<br />
<br />
# The half-ring CMB maps are produced by the pipelines with parameters/weights fixed to the values obtained from the full maps. Therefore the CMB HRHD maps do not capture all of the uncertainties due to foreground modelling on large angular scales.<br />
# The HRHD maps for the HFI frequency channels underestimate the noise power spectrum at high l by typically a few percent. This is caused by correlations induced in the pre-processing to remove cosmic ray hits. The CMB is mostly constrained by the HFI channels at high l, and so the CMB HRHD maps will inherit this deficiency in power.<br />
# The beam transfer functions do not account for uncertainties in the beams of the frequency channel maps.<br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper <cite>#planck2013-p06</cite> {{P2013|12}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper <cite>#planck2013-p06</cite> {{p2013|12}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
<br />
None. <br />
<br />
===File names===<br />
<br />
* Low frequency component at N$_\rm{side}$ 256: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
<br />
* Mask: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
<br />
====Low frequency foreground component====<br />
<br />
=====Low frequency component at N$_\rm{side}$ 256=====<br />
<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<math>_{CMB}</math>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
Below an example of the header. <br />
<!--pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 16 / width of table in bytes<br />
NAXIS2 = 786432 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'uK_CMB ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT2 = 'uK_CMB ' / physical unit of field<br />
TTYPE3 = 'Beta ' / label for field 3<br />
TFORM3 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT3 = 'none ' / physical unit of field<br />
TTYPE4 = 'B_stdev ' / label for field 4<br />
TFORM4 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT4 = 'none ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-13T13:26:14' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'QXaaRVZTQVaZQVYZ' / HDU checksum updated 2013-02-13T13:26:14<br />
DATASUM = '2752450756' / data unit checksum updated 2013-02-13T13:26:14<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 256 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 786431 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity is normalized at 30GHz<br />
COMMENT The intensity was estimated during mixing matrix estimation<br />
COMMENT Object:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_stddev.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
=====Low frequency component at N$_\rm{side}$ 2048=====<br />
<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<math>_{CMB}</math>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<math>_{CMB}</math> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
Below an example of the header of the first and second extension respectively. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 32 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT1 = 'uK_CMB ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT2 = 'uK_CMB ' / physical unit of field<br />
TTYPE3 = 'I_hr1 ' / label for field 3<br />
TFORM3 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT3 = 'uK_CMB ' / physical unit of field<br />
TTYPE4 = 'I_hr2 ' / label for field 4<br />
TFORM4 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT4 = 'uK_CMB ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-15T17:12:04' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'dlA5ei24di94di94' / HDU checksum updated 2013-02-15T17:12:13<br />
DATASUM = '3117718572' / data unit checksum updated 2013-02-15T17:12:13<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity was computed after mixibg matrix application<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_lowfreq.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_lowfreq_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_lowfreq.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_lowfreq.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre><br />
<br />
<pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 1501 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'BeamWF ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'BeamWF '<br />
DATE = '2013-02-15T17:12:17' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '74GA849274E97499' / HDU checksum updated 2013-02-15T17:12:17<br />
DATASUM = '3098248385' / data unit checksum updated 2013-02-15T17:12:17<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
MAX-LPOL= 1500 / Maximum L multipole<br />
POLAR = T / Polarization included (True/False)<br />
BCROSS = T / Magnetic cross terms included (True/False)<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity was computed after mixing matrix application<br />
COMMENT<br />
COMMENT Objects used:<br />
COMMENT<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_beams/dx9_delta_v1_7b_lowfreq_beam.fits<br />
COMMENT<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
====Thermal dust====<br />
<br />
=====Thermal dust component at N$_\rm{side}$=256=====<br />
<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<math>_{CMB}</math> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
Below an example of the header. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 24 / width of table in bytes<br />
NAXIS2 = 786432 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 6 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'MJy/sr ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT2 = 'MJy/sr ' / physical unit of field<br />
TTYPE3 = 'Em ' / label for field 3<br />
TFORM3 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT3 = 'uK_CMB ' / physical unit of field<br />
TTYPE4 = 'Em_stdev' / label for field 4<br />
TFORM4 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT4 = 'none ' / physical unit of field<br />
TTYPE5 = 'T ' / label for field 5<br />
TFORM5 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT5 = 'uK_CMB ' / physical unit of field<br />
TTYPE6 = 'T_stdev ' / label for field 6<br />
TFORM6 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT6 = 'uK_CMB ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-13T13:31:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '9OAOJO7N9OANGO7N' / HDU checksum updated 2013-02-13T13:31:15<br />
DATASUM = '4139938263' / data unit checksum updated 2013-02-13T13:31:15<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 256 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 786431 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_dust-commrul_0256_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity is normalized at 353 GHz<br />
COMMENT Object:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_stddev.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
=====Thermal dust component at N$_\rm{side}$=2048=====<br />
<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
Below an example of the header of the first and second extension respectively. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 32 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT1 = 'MJy/sr ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT2 = 'MJy/sr ' / physical unit of field<br />
TTYPE3 = 'I_hr1 ' / label for field 3<br />
TFORM3 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT3 = 'MJy/sr ' / physical unit of field<br />
TTYPE4 = 'I_hr2 ' / label for field 4<br />
TFORM4 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT4 = 'MJy/sr ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-16T10:23:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '6k8A7i826i896i89' / HDU checksum updated 2013-02-16T10:23:32<br />
DATASUM = '3817117839' / data unit checksum updated 2013-02-16T10:23:32<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_dust-commrul_2048_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_dust_flux.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_dust_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_dust_flux.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_dust_flux.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre><br />
<br />
<pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 3001 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'BeamWF ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'BeamWF '<br />
DATE = '2013-02-16T10:23:34' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'FBGWI9EWFAEWF7EW' / HDU checksum updated 2013-02-16T10:23:34<br />
DATASUM = '4096860189' / data unit checksum updated 2013-02-16T10:23:34<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
MAX-LPOL= 3000 / Maximum L multipole<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Beam window function used in the Component separation process<br />
COMMENT<br />
COMMENT Objects used:<br />
COMMENT<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_beams/dx9_delta_v1_7b_dust_beam.fits<br />
COMMENT<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
====Sky mask====<br />
<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
Below an example of the header. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'Mask ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-16T21:07:43' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '5fQAAeQ45eQAAeQ3' / HDU checksum updated 2013-02-16T21:07:44<br />
DATASUM = '1075621420' / data unit checksum updated 2013-02-16T21:07:44<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
OBJECT = 'FULLSKY ' / Sky coverage, either FULLSKY or PARTIAL<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Mask-rulerminimal_2048.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_masks/deltadx9_ruler_mask_total_minimal.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
== Dust optical depth map and model ==<br />
<br />
Thermal emission from interstellar dust is captured by Planck-HFI over the whole sky, at all frequencies from 100 to 857 GHz. This emission is well modelled by a modified black body in the far-infrared to millimeter range. It is produced by the biggest interstellar dust grain that are in thermal equilibrium with the radiation field from stars. The grains emission properties in the sub-millimeter are therefore directly linked to their absorption properties in the UV-visible range. By modelling the thermal dust emission in the sub-millimeter, a map of dust reddening in the visible can then be constructed. <br />
<br />
; Model of thermal dust emission<br />
<br />
The model of the thermal dust emission is based on a modify black body fit to the data $I_\nu$<br />
<br />
$I_\nu = A\, B_\nu(T)\, \nu^\beta$<br />
<br />
where B_nu(T) is the Planck function for dust equilibirum temperature T, A is the amplitude of the MBB and beta the dust spectral index. The dust optical depth at frequency nu is<br />
<br />
$\tau_\nu = I_\nu / B_\nu(T) = A\, \nu^\beta$<br />
<br />
The dust parameters provided are $T$, beta and $\tau_{353}$. They were obtained by fitting the Planck data at 353, 545 and 857 GHz together with the IRAS (IRIS) 100 micron data. All maps (in Healpix N$_\rm{side}$=2048) were smoothed to a common resolution of 5 arcmin. The CMB anisotropies, clearly visible at 353 GHz, were removed from all the HFI maps using the SMICA map. An offset was removed from each map to obtained a meaningful Galactic zero level, using a correlation with the LAB 21 cm data in diffuse areas of the sky ($N_{HI} < 2\times10^{20} cm^{-2}$). Because the dust emission is so well correlated between frequencies in the Rayleigh-Jeans part of the dust spectrum, the zero level of the 545 and 353 GHz were improved by correlating with the 857 GHz over a larger mask ($N_{HI} < 3\times10^{20} cm^{-2}$). Faint residual dipole structures, identified in the 353 and 545 GHz maps, were removed prior to the fit.<br />
<br />
The MBB fit was performed using a chi-square minimization, assuming errors for each data point that include instrumental noise, calibration uncertainties (on both the dust emission and the CMB anisotropies) and uncertainties on the zero level. Because of the known degeneracy between $T$ and $\beta$ in the presence of noise, we produced a model of dust emission using data smoothed to 35 arcmin; at such resolution no systematic bias of the parameters is observed. The map of the spectral index $\beta$ at 35 arcmin was than used to fit the data for $T$ and $\tau_{353}$ at 5 arcmin. <br />
<br />
; The $E(B-V)$ map <br />
For the production of the $E(B-V)$ map, we used Planck and IRAS data from which point sources in diffuse areas were removed to avoid contamination by galaxies. In the hypothesis of constant dust emission cross-section, the optical depth map $\tau_{353}$ is proportional to dust column density. It can then be used to estimate E(B-V), also proportional to dust column density in the hypothesis of a constant differential absorption cross-section between the B and V bands. Given those assumptions, $ E(B-V) = q\, \tau_{353}$.<br />
<br />
To estimate the calibration factor q, we followed a method similar to <cite>#mortsell2013</cite> based on SDSS reddening measurements ($E(g-r)$ which corresponds closely to $E(B-V)$) of 77 429 Quasars <cite>#schneider2007</cite>. The interstellar HI column densities covered on the lines of sight of this sample ranges from $0.5$ to $10\times10^{20}\,cm^{-2}$. Therefore this sample allows to estimate q in the diffuse ISM where dust properties are expected to vary less than in denser clouds where coagulation and grain growth might modify dust emission and absorption cross sections. <br />
<br />
; Dust optical depth products<br />
<br />
The characteristics of the dust model maps are the following.<br />
* Dust optical depth at 353 GHz : N$_\rm{side}$=2048, fwhm=5 arcmin, no units<br />
* Dust reddening E(B-V) : N$_\rm{side}$=2048, fwhm=5 arcmin, units=magnitude, obtained with data from which point sources were removed.<br />
* Dust temperature : N$_\rm{side}$ 2048, fwhm=5 arcmin, units=Kelvin<br />
* Dust spectral index : N$_\rm{side}$=2048, fwhm=35 arcmin, no units<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Dust opacity file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
| TAU353 || Real*4 || none || The opacity at 353GHz<br />
|-<br />
| TAU353ERR || Real*4 || none || Error in the opacity<br />
|-<br />
| EBV || Real*4 || mag || E(B-V)<br />
|-<br />
| EBV_ERR || Real*4 || mag || Error in E(B-V)<br />
|-<br />
|T_HF || Real*4 || K || Temperature for the high frequency correction<br />
|-<br />
|T_HF_ERR || Real*4 || K || Error on the temperature<br />
|-<br />
| BETAHF || Real*4 || none || Beta for the high frequency correction<br />
|-<br />
| BETAHFERR || Real*4 || none || Error on beta<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
| AST-COMP || String || DUST-OPA|| Astrophysical compoment name<br />
|-<br />
| PIXTYPE || String || HEALPIX ||<br />
|-<br />
| COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
| ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
| NSIDE || Int || 2048 || Healpix N$_\rm{side}$ for LFI and HFI, respectively<br />
|-<br />
| FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
| LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|}<br />
<br />
== CO emission maps ==<br />
<br />
CO rotational transition line emission is present in all HFI bands but for the 143 GHz channel. It is especially significant in the 100, 217 and 353 GHz channels (due to the 115 (1-0), 230 (2-1) and 345 GHz (3-2) CO transitions). This emission comes essentially from the Galactic interstellar medium and is mainly located at low and intermediate Galactic latitudes. Three approaches (summarised below) have been used to extract CO velocity-integrated emission maps from HFI maps and to make three types of CO products. An introduction is given in [[Science#CO_maps|Section]] and a full description of these products is given in <cite>#planck2013-p03a</cite>.<br />
* Type 1 product: it is based on a single channel approach using the fact that each CO line has a slightly different transmission in each bolometer at a given frequency channel. These transmissions can be evaluated from bandpass measurements that were performed on the ground or empirically determined from the sky using existing ground-based CO surveys. From these, the J=1-0, J=2-1 and J=3-2 CO lines can be extracted independently. As this approach is based on individual bolometer maps of a single channel, the resulting Signal-to-Noise ratio (SNR) is relatively low. The benefit, however, is that these maps do not suffer from contamination from other HFI channels (as is the case for the other approaches) and are more reliable, especially in the Galactic Plane.<br />
<br />
* Type 2 product: this product is obtained using a multi frequency approach. Three frequency channel maps are combined to extract the J=1-0 (using the 100, 143 and 353 GHz channels) and J=2-1 (using the 143, 217 and 353 GHz channels) CO maps. Because frequency channels are combined, the spectral behaviour of other foregrounds influences the result. The two type 2 CO maps produced in this way have a higher SNR than the type 1 maps at the cost of a larger possible residual contamination from other diffuse foregrounds.<br />
<br />
* Type 3 product: using prior information on CO line ratios and a multi-frequency component separation method, we construct a combined CO emission map with the largest possible SNR. This type 3 product can be used as a sensitive finder chart for low-intensity diffuse CO emission over the whole sky.<br />
<br />
The released Type 1 CO maps have been produced using the MILCA-b algorithm, Type 2 maps using a specific implementation of the Commander algorithm, and the Type 3 map using the full Commander-Ruler component separation pipeline (see [[Astrophysical_component_maps#Maps_of_astrophysical_foregrounds|above]]).<br />
<br />
Characteristics of the released maps are the following. We provide Healpix maps with N$_\rm{side}$=2048. For one transition, the CO velocity-integrated line signal map is given in K_RJ.km/s units. A conversion factor from this unit to the native unit of HFI maps (K_CMB) is provided in the header of the data files and in the RIMO. Four maps are given per transition and per type:<br />
* The signal map<br />
* The standard deviation map (same unit as the signal), <br />
* A null test noise map (same unit as the signal) with similar statistical properties. It is made out of half the difference of half-ring maps.<br />
* A mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.<br />
<br />
All products of a given type belong to a single file.<br />
Type 1 products have the native HFI resolution i.e. approximately 10, 5 and 5 arcminutes for the CO 1-0, 2-1, 3-2 transitions respectively.<br />
Type 2 products have a 15 arcminute resolution<br />
The Type 3 product has a 5.5 arcminute resolution.<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-1 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map<br />
|-<br />
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity<br />
|-<br />
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable<br />
|-<br />
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map<br />
|-<br />
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity<br />
|-<br />
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable<br />
|-<br />
|I32 || Real*4 || K_RJ km/sec || The CO(3-2) intensity map<br />
|-<br />
|E32 || Real*4 || K_RJ km/sec || Uncertainty in the CO(3-2) intensity<br />
|-<br />
|N32 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M32 || Byte || none || Region over which the CO(3-2) intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || string || CO-TYPE2 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix N$_\rm{side}$ for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 3-2 || Real*4 || value || Factor to convert CO(3-2) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-2 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map<br />
|-<br />
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity<br />
|-<br />
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable<br />
|-<br />
|-<br />
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map<br />
|-<br />
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity<br />
|-<br />
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CO-TYPE2 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-3 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|INTEN || Real*4 || K_RJ km/sec || The CO intensity map<br />
|-<br />
|ERR || Real*4 || K_RJ km/sec || Uncertainty in the intensity<br />
|-<br />
|NUL || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|MASK || Byte || none || Region over which the intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CO-TYPE1 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV || Real*4 || value || Factor to convert to Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
== References ==<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Lviberthttps://wiki.cosmos.esa.int/planckpla/index.php?title=CMB_and_astrophysical_component_maps&diff=7320CMB and astrophysical component maps2013-03-19T15:18:05Z<p>Lvibert: </p>
<hr />
<div>== Overview ==<br />
<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in <cite>#planck2013-p06</cite>.<br />
<br />
==CMB maps==<br />
<br />
Four pipelines have been used to produce maps of the CMB: Commander-Ruler, NILC, SEVEM and SMICA. The last three have been delivered as Legacy Archive products.<br />
<br />
The front-runner CMB map is the SMICA one. This product is labeled as "Main product" in the Planck Legacy Archive Java interface while the two others (NILC, SEVEM) are labeled as "Additional product".<br />
<br />
The component separation pipelines are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation|CMB and foreground separation]] section and also in Section 3 and Appendices A-D of <cite>#planck2013-p06</cite> {{P2013|12}} and references therein.<br />
<br />
===Product description ===<br />
<br />
; SMICA<br />
<br />
* Principle:<br />
SMICA produces a CMB map by linearly combining all Planck<br />
input channels (from 30 to 857 GHz) with weights which vary with the<br />
multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
<br />
* Resolution (effective beam):<br />
The SMICA map has an effective beam window function of 5 arc-minutes,<br />
deconvolved from the pixel window. It means that, ideally, one would<br />
have <math>C_\ell(map) = C_\ell(sky) * B_{(5')}^2</math>, where<br />
<math>C_\ell(map)</math> is the angular spectrum of the map, where<br />
<math>C_\ell(sky)</math> is the angular spectrum of the CMB and<br />
<math>B_{(5')}</math> is a 5-arcminute Gaussian beam function.<br />
<br />
* Confidence mask:<br />
a confidence mask is provided which excludes some<br />
parts of the Galactic plane, some very bright areas and the masked<br />
point sources.<br />
<br />
* Undefined pixels:<br />
The SMICA map has valid pixels over 97% of the<br />
sky: a binary mask describing the valid pixels is provided (as the 4th<br />
column of the FITS file). The 3% invalid pixels are not set to zero<br />
(or to some NaN value): their values result from the pre-processing<br />
step in which this area is filled-in by a smooth field in order to<br />
avoid spectral leakage. <br />
<br />
<br />
<br />
; NILC<br />
<br />
* Principle: <br />
The Needlet-ILC (hereafter NILC) CMB map is constructed<br />
from all Planck channels from 44 to 857 GHz and includes multipoles up<br />
to <math>\ell = 3200</math>. It is obtained by applying the Internal<br />
Linear Combination (ILC) technique in needlet space, that is, with<br />
combination weights which are allowed to vary over the sky and over<br />
the whole multipole range.<br />
<br />
* Confidence mask:<br />
a confidence mask is provided which excludes some<br />
parts of the Galactic plane, some very bright areas and the masked<br />
point sources.<br />
<br />
* Undefined pixels:<br />
The NILC data structure contains an "INPMASK" '''which should be ignored'''.<br />
<br />
<br />
; SEVEM<br />
<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations Leach et al., 2008 <cite>#leach2008</cite> and to WMAP polarisation data Fernandez-Cobos et al., 2012 <cite>xx</cite>. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.<br />
<br />
<br />
===Production process===<br />
<br />
; SMICA<br />
<br />
Some implementation details about the SMICA products.<br />
<br />
All nine Planck frequency channels from 30 to 857 GHz, harmonically transformed up to <math>\ell = 4000 </math>.<br />
<br />
<br />
Before applying the SMICA weights in the harmonic domain, the input<br />
maps undergo a pre-processing step to deal with point sources. The<br />
point sources with SNR > 5 in the PCCS catalogue are fitted in each<br />
input map. If the fit is successful, the fitted point source is<br />
removed from the map; otherwise it is masked and the hole is<br />
in-painted by a simple diffusive process to ensure a smooth transition<br />
and mitigate spectral leakage. This is done at all frequencies but 545<br />
and 857 GHz, where all point sources with SNR > 7.5 are masked and<br />
in-painted.<br />
<br />
Viewed as a filter, SMICA can be summarized by the weights<br />
<math>\mathbf{w}_\ell</math> applied to each input map as a function<br />
of multipole. In this sense, SMICA is strictly equivalent to co-adding<br />
the input maps after convolution by specific axi-symmetric kernels<br />
directly related to the corresponding entry of<br />
<math>\mathbf{w}_\ell</math>. The SMICA weights used here are shown in<br />
the figure below for input maps in units of<br />
K<math>_\rm{RJ}</math>. They show, in particular, the (expected)<br />
progressive attenuation of the lowest resolution channels with<br />
increasing multipole.<br />
<br />
[[File:smica.jpg|thumb|center|600px|'''Weights <math>w_\ell</math> given by SMICA to the input maps, after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
<br />
; NILC<br />
<br />
The NILC method combines linearly input maps varying over the sky and<br />
over multipoles. In the needlet framework, harmonic localisation is<br />
achieved using a set of bandpass filters defining ‘scales’ and spatial<br />
localization is achieved, at each scale, by defining zones over the<br />
sky. The harmonic localisation used here uses 9 spectral bands<br />
covering multipoles up to <math>\ell</math> = 3200 (see figure<br />
below). The spatial localisation depends on the scale: at the coarsest<br />
scale, which include the multipoles of lowest degree, we use a single<br />
zone (no localization) while at the finest scales (which include the<br />
highest degree multipoles), the sky is partitioned in up to 20 zones<br />
(again, see figure below).<br />
<br />
<center><br />
<gallery perrow=2 widths=300px heights=180px><br />
File:Nilc1.jpg | Spectral window functions defining nine ''needlet scales''<br />
File:Nilc2.jpg | The 2-zone partition for scale 2.<br />
File:Nilc3.jpg | The 4-zone partition for scale 3.<br />
File:Nilc4.jpg | The 20-zone partition for scales 5 to 9.<br />
</gallery><br />
</center><br />
<br />
The actual processing differs from the above scenario in several respects: pre-processing of point sources, dealing with frequency-dependent beams, and dealing with statistical issues (the ILC bias) in the coarsest scale.<br />
* ''Pre-processing of point sources''. Identical to the SMICA pre-processing.<br />
* ''Masking and inpainting''. The NILC CMB map is actually produced in a two step process. In a first step, the NILC weights are computed from needlet statistics evaluated using a Galactic mask which covers about 98% of the sky (and is apodiwed at 1 degree). In a second step, those NILC weights on are applied to needlet coefficients computed over the whole sky (the point sources having been subtracted or fitted at the pre-processing stage), yielding a NILC CMB estimate over the whole sky, except for the point source mask. In a final step, those masked pixels are replaced by the values of a constrained Gaussian realization.<br />
* ''Beam control and transfer function''. As in the SMICA processing (see that section), the input maps are represented by their spherical harmonic coefficients. By internally rebeaming to a 5 arcmin resolution and by the unbiasedness property of the ILC, the resulting CMB map is automatically synthesized with an effective Gaussian beam of 5 arcmin.<br />
* ''ILC bias and spectral statistics for the coarsest scale''. The coarsest scale of the NILC filter is not localized. Therefore, the NILC map at the coarsest scale is equivalent to a plain pixel-based ILC which is known to be quite susceptible to an ‘ILC bias’ due to chance correlations between the CMB and foregrounds. In order to mitigate that effect, the covariance matrix which determines the ILC coefficients at the coarsest scale is not computed as a pixel average but is rather estimated in the spectral domain with a spectral weight which equalizes the power of the CMB modes (based on a fiducial spectrum).<br />
* ''Using SMICA recalibration''. In our current rendering, the NILC uses for the CMB emission law the values determined by SMICA.<br />
<br />
For more details, see <cite>#planck2013-p06</cite>.<br />
<br />
; SEVEM<br />
<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization; Casaponsa et al. 2011 <cite>#Casaponsa2011</cite>) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky:<br />
<br />
:<math> \label{eq:eq4}<br />
T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x})<br />
</math><br />
<br />
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
An additional level of flexibility can also be considered: the linear coefficients can be the same for all the sky, or several regions with different sets of coefficients can be considered. The regions are then combined in a smooth way, by weighting the pixels at the boundaries, to avoid discontinuities in the clean maps.<br />
Since the method is linear, we may easily propagate the noise properties to the final CMB map. Moreover, it is very fast and permits the generation of thousands of simulations to character- ize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
In particular, we have cleaned the 143 GHz and 217 GHz maps using four templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and (857-545). For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). In order to take into account the different spectral behaviour of the foregrounds at low and high galactic latitudes, we have considered two independent regions of the sky, for which we have used a different set of coefficients. The first region corresponds to the 3 per cent brightest Galactic emission, whereas the second region is defined by the remaining 97 per cent of the sky. For the first region, the coefficients are actually estimated over the whole sky (we find that this is more optimal than perform the minimisation only on the 3 per cent brightest region, where the CMB emission is very sub-dominant) while for the second region, we exclude the 3 per cent brightest region of the sky, point sources detected at any frequency and those pixels which have not been observed at all channels.<br />
Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
Moreover, additional CMB clean maps (at frequencies between 44 and 353 GHz) have also been produced using different combinations of templates for some of the analyses carried out in <cite>#planck2013-p09</cite> {{P2013|23}} and <cite>#planck2013-p14</cite> {{P2013|19}}. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in <cite>#planck2013-p14</cite>, while frequencies from 70 to 217 GHz were used for consistency tests in <cite>#planck2013-p09</cite>.<br />
<br />
The method has been successfully applied to Planck simulations <cite>#leach2008</cite> and to WMAP polarisation data <cite>#Fernandez-Cobos2012</cite>.<br />
<br />
===Inputs===<br />
<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. <br />
<br />
; SMICA<br />
<br />
SMICA uses all nine Planck frequency channels from 30 to 857 GHz. SMICA uses a pre-processing step in which point sources are subtracted or masked as described above.<br />
<br />
; NILC<br />
<br />
NILC uses eight frequency channels from 44 to 857 GHz and the same pre-processing step as SMICA.<br />
<br />
; SEVEM <br />
<br />
SEVEM uses all nine Planck frequency channel maps. The 30 - 70 GHz and 353 - 857 GHz maps are used to construct templates by taking the differences (30 - 44) GHz, (44 - 70) GHz, (545 - 353) GHz and (857 - 545) GHz, after smoothing to a common resolution. The 100, 143 and 217 GHz maps are cleaned using the templates.<br />
<br />
<br />
===File names and structure===<br />
<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.11.fits|link=COM_CompMap_CMB-nilc_2048_R1.11.fits}}<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.11.fits|link=COM_CompMap_CMB-sevem_2048_R1.11.fits}}<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.11.fits|link=COM_CompMap_CMB-smica_2048_R1.11.fits}}<br />
<br />
and the CMB they contain is shows below.<br />
<br />
<center><br />
<gallery perrow=3 widths=260px heights=170px> <br />
File: CMB-smica.png | SMICA<br />
File: CMB-nilc.png | NILC<br />
File: CMB-sevem.png | SEVEM<br />
</gallery></center><br />
<br />
<br />
The files contains a minimal primary extension with no data and four data extensions which are described in the table below:<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || The CMB temperature map<br />
|-<br />
|NOISE || Real*4 || uK_cmb || Estimated noise map (Note 1)<br />
|-<br />
|VALMASK|| Byte || none || Validity, or confidence mask (note 2)<br />
|-<br />
|INPMASK || Byte || none || Inpainted mask (Optional - see Note 3) <br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''FGDS-LFI'' (BINTABLE) - Note 4<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|LFI_030 || Real*4 || K_cmb || 30 GHz foregrounds<br />
|-<br />
|LFI_044 || Real*4 || K_cmb || 44 GHz foregrounds<br />
|-<br />
|LFI_070 || Real*4 || K_cmb || 70 GHz foregrounds<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 3. EXTNAME = ''FGDS-HFI'' (BINTABLE) - Note 4<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|HFI_100 || Real*4 || K_cmb || 100 GHz foregrounds<br />
|-<br />
|HFI_143 || Real*4 || K_cmb || 143 GHz foregrounds<br />
|-<br />
|HFI_217 || Real*4 || K_cmb || 217 GHz foregrounds<br />
|-<br />
|HFI_353 || Real*4 || K_cmb || 353 GHz foregrounds<br />
|-<br />
|HFI_545 || Real*4 || MJy/sr || 545 GHz foregrounds<br />
|-<br />
|HFI_857 || Real*4 || MJy/sr || 857 GHz foregrounds<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || uK_cmb || The CMB temperature map<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|}<br />
<br />
<br />
Notes:<br />
# The half-ring half-difference (HRHD) map is made by passing the half-ring frequency maps independently through the component separation pipeline, then computing half their difference. It approximates a noise realisation, and gives an indication of the uncertainties due to instrumental noise in the corresponding CMB map. <br />
# The confidence mask indicates where the CMB map is considered valid. <br />
# NILC and SMICA CMB maps have been inpainted in the Galactic plane and around some bright sources with a constrained realisation of the signal. The inpainted area covers approximately 3% of the sky. This column is not present in the SEVEM product file.<br />
# The subtraction of the CMB from the sky maps in order to produce the foregrounds map is done after convolving the CMB map to the resolution of the given frequency.<br />
<br />
===Cautionary notes===<br />
<br />
# The half-ring CMB maps are produced by the pipelines with parameters/weights fixed to the values obtained from the full maps. Therefore the CMB HRHD maps do not capture all of the uncertainties due to foreground modelling on large angular scales.<br />
# The HRHD maps for the HFI frequency channels underestimate the noise power spectrum at high l by typically a few percent. This is caused by correlations induced in the pre-processing to remove cosmic ray hits. The CMB is mostly constrained by the HFI channels at high l, and so the CMB HRHD maps will inherit this deficiency in power.<br />
# The beam transfer functions do not account for uncertainties in the beams of the frequency channel maps.<br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper <cite>#planck2013-p06</cite> {{P2013|12}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper <cite>#planck2013-p06</cite> {{p2013|12}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
<br />
None. <br />
<br />
===File names===<br />
<br />
* Low frequency component at N$_\rm{side}$ 256: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
<br />
* Mask: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
<br />
====Low frequency foreground component====<br />
<br />
=====Low frequency component at N$_\rm{side}$ 256=====<br />
<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<math>_{CMB}</math>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
Below an example of the header. <br />
<!--pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 16 / width of table in bytes<br />
NAXIS2 = 786432 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'uK_CMB ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT2 = 'uK_CMB ' / physical unit of field<br />
TTYPE3 = 'Beta ' / label for field 3<br />
TFORM3 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT3 = 'none ' / physical unit of field<br />
TTYPE4 = 'B_stdev ' / label for field 4<br />
TFORM4 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT4 = 'none ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-13T13:26:14' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'QXaaRVZTQVaZQVYZ' / HDU checksum updated 2013-02-13T13:26:14<br />
DATASUM = '2752450756' / data unit checksum updated 2013-02-13T13:26:14<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 256 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 786431 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity is normalized at 30GHz<br />
COMMENT The intensity was estimated during mixing matrix estimation<br />
COMMENT Object:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_stddev.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
=====Low frequency component at N$_\rm{side}$ 2048=====<br />
<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<math>_{CMB}</math>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<math>_{CMB}</math> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
Below an example of the header of the first and second extension respectively. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 32 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT1 = 'uK_CMB ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT2 = 'uK_CMB ' / physical unit of field<br />
TTYPE3 = 'I_hr1 ' / label for field 3<br />
TFORM3 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT3 = 'uK_CMB ' / physical unit of field<br />
TTYPE4 = 'I_hr2 ' / label for field 4<br />
TFORM4 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT4 = 'uK_CMB ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-15T17:12:04' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'dlA5ei24di94di94' / HDU checksum updated 2013-02-15T17:12:13<br />
DATASUM = '3117718572' / data unit checksum updated 2013-02-15T17:12:13<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity was computed after mixibg matrix application<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_lowfreq.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_lowfreq_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_lowfreq.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_lowfreq.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre><br />
<br />
<pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 1501 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'BeamWF ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'BeamWF '<br />
DATE = '2013-02-15T17:12:17' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '74GA849274E97499' / HDU checksum updated 2013-02-15T17:12:17<br />
DATASUM = '3098248385' / data unit checksum updated 2013-02-15T17:12:17<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
MAX-LPOL= 1500 / Maximum L multipole<br />
POLAR = T / Polarization included (True/False)<br />
BCROSS = T / Magnetic cross terms included (True/False)<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity was computed after mixing matrix application<br />
COMMENT<br />
COMMENT Objects used:<br />
COMMENT<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_beams/dx9_delta_v1_7b_lowfreq_beam.fits<br />
COMMENT<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
====Thermal dust====<br />
<br />
=====Thermal dust component at N$_\rm{side}$=256=====<br />
<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<math>_{CMB}</math> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
Below an example of the header. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 24 / width of table in bytes<br />
NAXIS2 = 786432 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 6 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'MJy/sr ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT2 = 'MJy/sr ' / physical unit of field<br />
TTYPE3 = 'Em ' / label for field 3<br />
TFORM3 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT3 = 'uK_CMB ' / physical unit of field<br />
TTYPE4 = 'Em_stdev' / label for field 4<br />
TFORM4 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT4 = 'none ' / physical unit of field<br />
TTYPE5 = 'T ' / label for field 5<br />
TFORM5 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT5 = 'uK_CMB ' / physical unit of field<br />
TTYPE6 = 'T_stdev ' / label for field 6<br />
TFORM6 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT6 = 'uK_CMB ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-13T13:31:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '9OAOJO7N9OANGO7N' / HDU checksum updated 2013-02-13T13:31:15<br />
DATASUM = '4139938263' / data unit checksum updated 2013-02-13T13:31:15<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 256 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 786431 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_dust-commrul_0256_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity is normalized at 353 GHz<br />
COMMENT Object:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_stddev.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
=====Thermal dust component at N$_\rm{side}$=2048=====<br />
<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
Below an example of the header of the first and second extension respectively. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 32 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT1 = 'MJy/sr ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT2 = 'MJy/sr ' / physical unit of field<br />
TTYPE3 = 'I_hr1 ' / label for field 3<br />
TFORM3 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT3 = 'MJy/sr ' / physical unit of field<br />
TTYPE4 = 'I_hr2 ' / label for field 4<br />
TFORM4 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT4 = 'MJy/sr ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-16T10:23:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '6k8A7i826i896i89' / HDU checksum updated 2013-02-16T10:23:32<br />
DATASUM = '3817117839' / data unit checksum updated 2013-02-16T10:23:32<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_dust-commrul_2048_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_dust_flux.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_dust_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_dust_flux.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_dust_flux.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre><br />
<br />
<pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 3001 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'BeamWF ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'BeamWF '<br />
DATE = '2013-02-16T10:23:34' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'FBGWI9EWFAEWF7EW' / HDU checksum updated 2013-02-16T10:23:34<br />
DATASUM = '4096860189' / data unit checksum updated 2013-02-16T10:23:34<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
MAX-LPOL= 3000 / Maximum L multipole<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Beam window function used in the Component separation process<br />
COMMENT<br />
COMMENT Objects used:<br />
COMMENT<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_beams/dx9_delta_v1_7b_dust_beam.fits<br />
COMMENT<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
====Sky mask====<br />
<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
Below an example of the header. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'Mask ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-16T21:07:43' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '5fQAAeQ45eQAAeQ3' / HDU checksum updated 2013-02-16T21:07:44<br />
DATASUM = '1075621420' / data unit checksum updated 2013-02-16T21:07:44<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
OBJECT = 'FULLSKY ' / Sky coverage, either FULLSKY or PARTIAL<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Mask-rulerminimal_2048.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_masks/deltadx9_ruler_mask_total_minimal.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
== Dust optical depth map and model ==<br />
<br />
Thermal emission from interstellar dust is captured by Planck-HFI over the whole sky, at all frequencies from 100 to 857 GHz. This emission is well modelled by a modified black body in the far-infrared to millimeter range. It is produced by the biggest interstellar dust grain that are in thermal equilibrium with the radiation field from stars. The grains emission properties in the sub-millimeter are therefore directly linked to their absorption properties in the UV-visible range. By modelling the thermal dust emission in the sub-millimeter, a map of dust reddening in the visible can then be constructed. <br />
<br />
; Model of thermal dust emission<br />
<br />
The model of the thermal dust emission is based on a modify black body fit to the data $I_\nu$<br />
<br />
$I_\nu = A\, B_\nu(T)\, \nu^\beta$<br />
<br />
where B_nu(T) is the Planck function for dust equilibirum temperature T, A is the amplitude of the MBB and beta the dust spectral index. The dust optical depth at frequency nu is<br />
<br />
$\tau_\nu = I_\nu / B_\nu(T) = A\, \nu^\beta$<br />
<br />
The dust parameters provided are $T$, beta and $\tau_{353}$. They were obtained by fitting the Planck data at 353, 545 and 857 GHz together with the IRAS (IRIS) 100 micron data. All maps (in Healpix N$_\rm{side}$=2048) were smoothed to a common resolution of 5 arcmin. The CMB anisotropies, clearly visible at 353 GHz, were removed from all the HFI maps using the SMICA map. An offset was removed from each map to obtained a meaningful Galactic zero level, using a correlation with the LAB 21 cm data in diffuse areas of the sky ($N_{HI} < 2\times10^{20} cm^{-2}$). Because the dust emission is so well correlated between frequencies in the Rayleigh-Jeans part of the dust spectrum, the zero level of the 545 and 353 GHz were improved by correlating with the 857 GHz over a larger mask ($N_{HI} < 3\times10^{20} cm^{-2}$). Faint residual dipole structures, identified in the 353 and 545 GHz maps, were removed prior to the fit.<br />
<br />
The MBB fit was performed using a chi-square minimization, assuming errors for each data point that include instrumental noise, calibration uncertainties (on both the dust emission and the CMB anisotropies) and uncertainties on the zero level. Because of the known degeneracy between $T$ and $\beta$ in the presence of noise, we produced a model of dust emission using data smoothed to 35 arcmin; at such resolution no systematic bias of the parameters is observed. The map of the spectral index $\beta$ at 35 arcmin was than used to fit the data for $T$ and $\tau_{353}$ at 5 arcmin. <br />
<br />
; The $E(B-V)$ map <br />
For the production of the $E(B-V)$ map, we used Planck and IRAS data from which point sources in diffuse areas were removed to avoid contamination by galaxies. In the hypothesis of constant dust emission cross-section, the optical depth map $\tau_{353}$ is proportional to dust column density. It can then be used to estimate E(B-V), also proportional to dust column density in the hypothesis of a constant differential absorption cross-section between the B and V bands. Given those assumptions, $ E(B-V) = q\, \tau_{353}$.<br />
<br />
To estimate the calibration factor q, we followed a method similar to <cite>#mortsell2013</cite> based on SDSS reddening measurements ($E(g-r)$ which corresponds closely to $E(B-V)$) of 77 429 Quasars <cite>#schneider2007</cite>. The interstellar HI column densities covered on the lines of sight of this sample ranges from $0.5$ to $10\times10^{20}\,cm^{-2}$. Therefore this sample allows to estimate q in the diffuse ISM where dust properties are expected to vary less than in denser clouds where coagulation and grain growth might modify dust emission and absorption cross sections. <br />
<br />
; Dust optical depth products<br />
<br />
The characteristics of the dust model maps are the following.<br />
* Dust optical depth at 353 GHz : N$_\rm{side}$=2048, fwhm=5 arcmin, no units<br />
* Dust reddening E(B-V) : N$_\rm{side}$=2048, fwhm=5 arcmin, units=magnitude, obtained with data from which point sources were removed.<br />
* Dust temperature : N$_\rm{side}$ 2048, fwhm=5 arcmin, units=Kelvin<br />
* Dust spectral index : N$_\rm{side}$=2048, fwhm=35 arcmin, no units<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Dust opacity file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
| TAU353 || Real*4 || none || The opacity at 353GHz<br />
|-<br />
| TAU353ERR || Real*4 || none || Error in the opacity<br />
|-<br />
| EBV || Real*4 || mag || E(B-V)<br />
|-<br />
| EBV_ERR || Real*4 || mag || Error in E(B-V)<br />
|-<br />
|T_HF || Real*4 || K || Temperature for the high frequency correction<br />
|-<br />
|T_HF_ERR || Real*4 || K || Error on the temperature<br />
|-<br />
| BETAHF || Real*4 || none || Beta for the high frequency correction<br />
|-<br />
| BETAHFERR || Real*4 || none || Error on beta<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
| AST-COMP || String || DUST-OPA|| Astrophysical compoment name<br />
|-<br />
| PIXTYPE || String || HEALPIX ||<br />
|-<br />
| COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
| ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
| NSIDE || Int || 2048 || Healpix N$_\rm{side}$ for LFI and HFI, respectively<br />
|-<br />
| FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
| LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|}<br />
<br />
== CO emission maps ==<br />
<br />
CO rotational transition line emission is present in all HFI bands but for the 143 GHz channel. It is especially significant in the 100, 217 and 353 GHz channels (due to the 115 (1-0), 230 (2-1) and 345 GHz (3-2) CO transitions). This emission comes essentially from the Galactic interstellar medium and is mainly located at low and intermediate Galactic latitudes. Three approaches (summarised below) have been used to extract CO velocity-integrated emission maps from HFI maps and to make three types of CO products. An introduction is given in [[Science#CO_maps|Section]] and a full description of these products is given in <cite>#planck2013-p03a</cite>.<br />
* Type 1 product: it is based on a single channel approach using the fact that each CO line has a slightly different transmission in each bolometer at a given frequency channel. These transmissions can be evaluated from bandpass measurements that were performed on the ground or empirically determined from the sky using existing ground-based CO surveys. From these, the J=1-0, J=2-1 and J=3-2 CO lines can be extracted independently. As this approach is based on individual bolometer maps of a single channel, the resulting Signal-to-Noise ratio (SNR) is relatively low. The benefit, however, is that these maps do not suffer from contamination from other HFI channels (as is the case for the other approaches) and are more reliable, especially in the Galactic Plane.<br />
<br />
* Type 2 product: this product is obtained using a multi frequency approach. Three frequency channel maps are combined to extract the J=1-0 (using the 100, 143 and 353 GHz channels) and J=2-1 (using the 143, 217 and 353 GHz channels) CO maps. Because frequency channels are combined, the spectral behaviour of other foregrounds influences the result. The two type 2 CO maps produced in this way have a higher SNR than the type 1 maps at the cost of a larger possible residual contamination from other diffuse foregrounds.<br />
<br />
* Type 3 product: using prior information on CO line ratios and a multi-frequency component separation method, we construct a combined CO emission map with the largest possible SNR. This type 3 product can be used as a sensitive finder chart for low-intensity diffuse CO emission over the whole sky.<br />
<br />
The released Type 1 CO maps have been produced using the MILCA-b algorithm, Type 2 maps using a specific implementation of the Commander algorithm, and the Type 3 map using the full Commander-Ruler component separation pipeline (see [[Astrophysical_component_maps#Maps_of_astrophysical_foregrounds|above]]).<br />
<br />
Characteristics of the released maps are the following. We provide Healpix maps with N$_\rm{side}$=2048. For one transition, the CO velocity-integrated line signal map is given in K_RJ.km/s units. A conversion factor from this unit to the native unit of HFI maps (K_CMB) is provided in the header of the data files and in the RIMO. Four maps are given per transition and per type:<br />
* The signal map<br />
* The standard deviation map (same unit as the signal), <br />
* A null test noise map (same unit as the signal) with similar statistical properties. It is made out of half the difference of half-ring maps.<br />
* A mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.<br />
<br />
All products of a given type belong to a single file.<br />
Type 1 products have the native HFI resolution i.e. approximately 10, 5 and 5 arcminutes for the CO 1-0, 2-1, 3-2 transitions respectively.<br />
Type 2 products have a 15 arcminute resolution<br />
The Type 3 product has a 5.5 arcminute resolution.<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-1 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map<br />
|-<br />
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity<br />
|-<br />
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable<br />
|-<br />
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map<br />
|-<br />
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity<br />
|-<br />
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable<br />
|-<br />
|I32 || Real*4 || K_RJ km/sec || The CO(3-2) intensity map<br />
|-<br />
|E32 || Real*4 || K_RJ km/sec || Uncertainty in the CO(3-2) intensity<br />
|-<br />
|N32 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M32 || Byte || none || Region over which the CO(3-2) intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || string || CO-TYPE2 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix N$_\rm{side}$ for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 3-2 || Real*4 || value || Factor to convert CO(3-2) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-2 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map<br />
|-<br />
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity<br />
|-<br />
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable<br />
|-<br />
|-<br />
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map<br />
|-<br />
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity<br />
|-<br />
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CO-TYPE2 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-3 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|INTEN || Real*4 || K_RJ km/sec || The CO intensity map<br />
|-<br />
|ERR || Real*4 || K_RJ km/sec || Uncertainty in the intensity<br />
|-<br />
|NUL || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|MASK || Byte || none || Region over which the intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CO-TYPE1 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV || Real*4 || value || Factor to convert to Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
== References ==<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Lviberthttps://wiki.cosmos.esa.int/planckpla/index.php?title=CMB_and_astrophysical_component_maps&diff=7319CMB and astrophysical component maps2013-03-19T14:49:44Z<p>Lvibert: some cleanups for the description of NIULC and SMICA</p>
<hr />
<div>== Overview ==<br />
<br />
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of the product and how it is obtained, followed by a description of the FITS file containing the data and associated information.<br />
All the details can be found in <cite>#planck2013-p06</cite>.<br />
<br />
==CMB maps==<br />
<br />
Four pipelines have been used to produce maps of the CMB: Commander-Ruler, NILC, SEVEM and SMICA. The last three have been delivered as Legacy Archive products.<br />
<br />
The front-runner CMB map is the SMICA one. This product is labeled as "Main product" in the Planck Legacy Archive Java interface while the two others (NILC, SEVEM) are labeled as "Additional product".<br />
<br />
The component separation pipelines are described in the [[Astrophysical_component_separation#CMB_and_foreground_separation|CMB and foreground separation]] section and also in Section 3 and Appendices A-D of <cite>#planck2013-p06</cite> {{P2013|12}} and references therein.<br />
<br />
===Product description ===<br />
<br />
; SMICA<br />
<br />
* Principle:<br />
SMICA produces a CMB map by linearly combining all Planck<br />
input channels (from 30 to 857 GHz) with weights which vary with the<br />
multipole. It includes multipoles up to <math>\ell = 4000</math>.<br />
<br />
* Resolution (effective beam):<br />
The SMICA map has an effective beam window function of 5 arc-minutes,<br />
deconvolved from the pixel window. It means that, ideally, one would<br />
have <math>C_\ell(map) = C_\ell(sky) * B_{(5')}^2</math>, where<br />
<math>C_\ell(map)</math> is the angular spectrum of the map, where<br />
<math>C_\ell(sky)</math> is the angular spectrum of the CMB and<br />
<math>B_{(5')}</math> is a 5-arcminute Gaussian beam function.<br />
<br />
* Confidence mask:<br />
a confidence mask is provided which excludes some<br />
parts of the Galactic plane, some very bright areas and the masked<br />
point sources.<br />
<br />
* Undefined pixels:<br />
The SMICA map has valid pixels over 97% of the<br />
sky: a binary mask describing the valid pixels is provided (as the 4th<br />
column of the FITS file). The 3% invalid pixels are not set to zero<br />
(or to some NaN value): their values result from the pre-processing<br />
step in which this area is filled-in by a smooth field in order to<br />
avoid spectral leakage. <br />
<br />
<br />
<br />
; NILC<br />
<br />
* Principle: <br />
The Needlet-ILC (hereafter NILC) CMB map is constructed<br />
from all Planck channels from 44 to 857 GHz and includes multipoles up<br />
to <math>\ell = 3200</math>. It is obtained by applying the Internal<br />
Linear Combination (ILC) technique in needlet space, that is, with<br />
combination weights which are allowed to vary over the sky and over<br />
the whole multipole range.<br />
<br />
* Confidence mask:<br />
a confidence mask is provided which excludes some<br />
parts of the Galactic plane, some very bright areas and the masked<br />
point sources.<br />
<br />
* Undefined pixels:<br />
The NILC data structure contains an "INPMASK" '''which should be ignored'''.<br />
<br />
<br />
; SEVEM<br />
<br />
The aim of SEVEM is to produce clean CMB maps at one or several frequencies by using a procedure based on template fitting. The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. The method has been successfully applied to Planck simulations Leach et al., 2008 <cite>#leach2008</cite> and to WMAP polarisation data Fernandez-Cobos et al., 2012 <cite>xx</cite>. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust.<br />
<br />
<br />
===Production process===<br />
<br />
; SMICA<br />
<br />
The actual implementation of SMICA includes the following steps:<br />
; Inputs<br />
: All nine Planck frequency channels from 30 to 857 GHz, harmonically transformed up to <math>\ell = 4000 </math>.<br />
; Fit<br />
: In practice, the SMICA fit,i.e.,the minimization of Eq. (4) in the [[Astrophysical component separation#SMICA|SMICA]] description section, is conducted in three successive steps: We first estimate the CMB spectral law by fitting all model parameters over a clean fraction of sky in the range <math> 100 ≤ \ell ≤ 680</math> and retaining the best fit value for vector <math> \mathbf{a}</math>. In the second step, we estimate the foreground emissivity by fixing a to its value from the previous step and fitting all the other parameters over a large fraction of sky in the range <math> 4 ≤ \ell ≤ 150</math> and retaining the best fit values for the matrix <math> \mathbf{A}</math>. In the last step, we fit all power spectrum parameters; that is, we fix <math>\mathbf{a}</math> and <math>\mathbf{A}</math> to their previously found values and fit for each <math> C_\ell </math> and <math>\mathbf{P}_\ell </math> at each <math>\ell</math>. <br />
; Beams<br />
: The discussion thus far assumes that all input maps have the same resolution and effective beam. Since the observed maps actually vary in resolution, we process the input maps in the following way. To the <math>i</math>-th input map with effective beam <math>b_i(\ell)</math> and sampled on an HEALPix grid with <math>N^i_{side}</math>, the CMB sky multipole <math>s_{\ell m}</math> actually contributes <math>s_{\ell m}a_i b_i(\ell) p_i(\ell)</math>, where <math>p_i(\ell)</math> is the pixel window function for the grid at <math>N^i_{side}</math>. Seeking a final CMB map at 5-arcmin resolution, the highest resolution of Planck, we work with input spherical harmonics re-beamed to 5 arcmins, <math>\mathbf{\tilde{x}}_{\ell m} </math>; that is, SMICA operates on vectors with entries <math>x ̃^i_{\ell m} = x^i_{\ell m} b_5(\ell) / b_i(\ell) / p_i(\ell)</math>, where <math>b_5(\ell)</math> is a 5 arcmin Gaussian beam function. By construction, SMICA then produces an CMB map with an effective Gaussian beam of 5 arcmin (without the pixel window function).<br />
; Pre-processing<br />
: We start by fitting point sources with SNR > 5 in the PCCS catalogue in each input map. If the fit is successful, the fitted point source is removed from the map; otherwise it is masked and the hole in-painted. This is done at all frequencies but 545 and 857 GHz, where all point sources with SNR > 7.5 are masked and in-painted. <br />
; Masking and in-painting<br />
: In practice, SMICA uses a small Galactic mask leaving 97% of the sky. We deliver a full-sky CMB map in which the masked pixels (Galactic and point-source) are replaced by a constrained Gaussian realization.<br />
; Binning<br />
: In our implementation, we use binned spectra.<br />
; High <math>\ell</math><br />
: Since there is little point trying to model the spectral covariance at high multipoles, because the sample estimate is sufficient, SMICA implements a simple harmonic ILC at <math>\ell > 1500</math>; that is, it applies the filter (Eq. (2) in the [[Astrophysical component separation#SMICA|SMICA]] description section) with <math>\mathbf{R}_\ell = \mathbf{\hat{R}}_\ell</math>.<br />
<br />
Viewed as a filter, SMICA can be summarized by the weights <math>\mathbf{w}_\ell</math> applied to each input map as a function of multipole. In this sense, SMICA is strictly equivalent to co-adding the input maps after convolution by specific axi-symmetric kernels directly related to the corresponding entry of <math>\mathbf{w}_\ell</math>. The SMICA weights used here are shown in the figure below for input maps in units of K<math>_\rm{RJ}</math>. They show, in particular, the (expected) progressive attenuation of the lowest resolution channels with increasing multipole.<br />
<br />
[[File:smica.jpg|thumb|center|600px|'''Weights <math>w_\ell</math> given by SMICA to the input maps, after they are re-beamed to 5 arcmin and expressed in K<math>_\rm{RJ}</math>), as a function of multipole.''']]<br />
<br />
<br />
; NILC<br />
<br />
The ability linearly to combine input maps varying over the sky and over multipoles is called ‘localisation’. In the needlet framework, harmonic localisation is achieved using a set of bandpass filters defining ‘scales’ and spatial localization is achieved, at each scale, by defining zones over the sky. The harmonic localisation used here uses 9 spectral bands covering multipoles up to <math>\ell</math> = 3200 (see figure below). The spatial localisation depends on the scale: at the coarsest scale, which include the multipoles of lowest degree, we use a single zone (no localization) while at the finest scales (which include the highest degree multipoles), the sky is partitioned in up to 20 zones (again, see figure below).<br />
<br />
<center><br />
<gallery perrow=2 widths=300px heights=180px><br />
File:Nilc1.jpg | Spectral window functions defining nine ''needlet scales''<br />
File:Nilc2.jpg | The 2-zone partition<br />
File:Nilc3.jpg | The 4-zone partition<br />
File:Nilc4.jpg | The 20-zone partition.<br />
</gallery><br />
'''Spectral localization for NILC using with nine spectral window functions defining nine ‘needlet scales’ (top left panel). The scale-dependent spatial localization partitions the sky in 1 zone (for scale 1), 2 zones (for scale 2), 4 zones (for scale 3), or 20 zones (for scales 5, 6, 7, 8, 9).'''<br />
</center><br />
<br />
The NILC method amounts to applying an ILC in each zone of each scale, allowing the ILC weights to adapt naturally to the varying strength of the contaminants as a function of direction and multipole. A complete description of the basic NILC method can be found in Delabrouille et al. (2009) <cite>#delabrouille2009</cite>. In this work, however, we have implemented an important difference for the processing of the coarsest scale.<br />
<br />
The actual processing differs from the above scenario in several respects: pre-processing of point sources, dealing with frequency-dependent beams, and dealing with statistical issues (the ILC bias) in the coarsest scale.<br />
* ''Pre-processing of point sources''. Identical to the SMICA pre-processing.<br />
* ''Masking and inpainting''. The NILC CMB map is actually produced in a two step process. In a first step, the NILC weights are computed from needlet statistics evaluated using a Galactic mask which covers about 98% of the sky (and is apodiwed at 1 degree). In a second step, those NILC weights on are applied to needlet coefficients computed over the whole sky (the point sources having been subtracted or fitted at the pre-processing stage), yielding a NILC CMB estimate over the whole sky, except for the point source mask. In a final step, those masked pixels are replaced by the values of a constrained Gaussian realization.<br />
* ''Beam control and transfer function''. As in the SMICA processing (see that section), the input maps are represented by their spherical harmonic coefficients. By internally rebeaming to a 5 arcmin resolution and by the unbiasedness property of the ILC, the resulting CMB map is automatically synthesized with an effective Gaussian beam of 5 arcmin.<br />
* ''ILC bias and spectral statistics for the coarsest scale''. The coarsest scale of the NILC filter is not localized. Therefore, the NILC map at the coarsest scale is equivalent to a plain pixel-based ILC which is known to be quite susceptible to an ‘ILC bias’ due to chance correlations between the CMB and foregrounds. In order to mitigate that effect, the covariance matrix which determines the ILC coefficients at the coarsest scale is not computed as a pixel average but is rather estimated in the spectral domain with a spectral weight which equalizes the power of the CMB modes (based on a fiducial spectrum).<br />
* ''Using SMICA recalibration''. In our current rendering, the NILC uses for the CMB emission law the values determined by SMICA.<br />
<br />
<br />
; SEVEM<br />
<br />
The templates are internal, i.e., they are constructed from Planck data, avoiding the need for external data sets, which usually complicates the analyses and may introduce inconsistencies. In the cleaning process, no assumptions about the foregrounds or noise levels are needed, rendering the technique very robust. The fitting can be done in real or wavelet space (using a fast wavelet adapted to the HEALPix pixelization; Casaponsa et al. 2011 <cite>#Casaponsa2011</cite>) to properly deal with incomplete sky coverage. By expediency, however, we fill in the small number of unobserved pixels at each channel with the mean value of its neighbouring pixels before applying SEVEM.<br />
<br />
We construct our templates by subtracting two close Planck frequency channel maps, after first smoothing them to a common resolution to ensure that the CMB signal is properly removed. A linear combination of the templates <math>t_j</math> is then subtracted from (hitherto unused) map d to produce a clean CMB map at that frequency. This is done either in real or in wavelet space (i.e., scale by scale) at each position on the sky:<br />
<br />
:<math> \label{eq:eq4}<br />
T_c(\mathbf{x}, ν) = d(\mathbf{x}, ν) − \sum_{j=1}^{n_t} α_j t(\mathbf{x})<br />
</math><br />
<br />
where <math>n_t</math> is the number of templates. If the cleaning is performed in real space, the <math>α_j</math> coefficients are obtained by minimising the variance of the clean map <math>T_c</math> outside a given mask. When working in wavelet space, the cleaning is done in the same way at each wavelet scale independently (i.e., the linear coefficients depend on the scale). Although we exclude very contaminated regions during the minimization, the subtraction is performed for all pixels and, therefore, the cleaned maps cover the full-sky (although we expect that foreground residuals are present in the excluded areas).<br />
<br />
An additional level of flexibility can also be considered: the linear coefficients can be the same for all the sky, or several regions with different sets of coefficients can be considered. The regions are then combined in a smooth way, by weighting the pixels at the boundaries, to avoid discontinuities in the clean maps.<br />
Since the method is linear, we may easily propagate the noise properties to the final CMB map. Moreover, it is very fast and permits the generation of thousands of simulations to character- ize the statistical properties of the outputs, a critical need for many cosmological applications. The final CMB map retains the angular resolution of the original frequency map.<br />
<br />
There are several possible configurations of SEVEM with regard to the number of frequency maps which are cleaned or the number of templates that are used in the fitting. Note that the production of clean maps at different frequencies is of great interest in order to test the robustness of the results. Therefore, to define the best strategy, one needs to find a compromise between the number of maps that can be cleaned independently and the number of templates that can be constructed.<br />
<br />
In particular, we have cleaned the 143 GHz and 217 GHz maps using four templates constructed as the difference of the following Planck channels (smoothed to a common resolution): (30-44), (44-70), (545-353) and (857-545). For simplicity, the three maps have been cleaned in real space, since there was not a significant improvement when using wavelets (especially at high latitude). In order to take into account the different spectral behaviour of the foregrounds at low and high galactic latitudes, we have considered two independent regions of the sky, for which we have used a different set of coefficients. The first region corresponds to the 3 per cent brightest Galactic emission, whereas the second region is defined by the remaining 97 per cent of the sky. For the first region, the coefficients are actually estimated over the whole sky (we find that this is more optimal than perform the minimisation only on the 3 per cent brightest region, where the CMB emission is very sub-dominant) while for the second region, we exclude the 3 per cent brightest region of the sky, point sources detected at any frequency and those pixels which have not been observed at all channels.<br />
Our final CMB map has then been constructed by combining the 143 and 217 GHz maps by weighting the maps in harmonic space taking into account the noise level, the resolution and a rough estimation of the foreground residuals of each map (obtained from realistic simulations). This final map has a resolution corresponding to a Gaussian beam of fwhm=5 arcminutes.<br />
<br />
Moreover, additional CMB clean maps (at frequencies between 44 and 353 GHz) have also been produced using different combinations of templates for some of the analyses carried out in <cite>#planck2013-p09</cite> {{P2013|23}} and <cite>#planck2013-p14</cite> {{P2013|19}}. In particular, clean maps from 44 to 353 GHz have been used for the stacking analysis presented in <cite>#planck2013-p14</cite>, while frequencies from 70 to 217 GHz were used for consistency tests in <cite>#planck2013-p09</cite>.<br />
<br />
The method has been successfully applied to Planck simulations <cite>#leach2008</cite> and to WMAP polarisation data <cite>#Fernandez-Cobos2012</cite>.<br />
<br />
===Inputs===<br />
<br />
The input maps are the sky temperature maps described in the [[Frequency Maps | Sky temperature maps]] section. <br />
<br />
; SMICA<br />
<br />
SMICA uses all nine Planck frequency channels from 30 to 857 GHz. SMICA uses a pre-processing step in which point sources are subtracted or masked as described above.<br />
<br />
; NILC<br />
<br />
NILC uses eight frequency channels from 44 to 857 GHz and the same pre-processing step as SMICA.<br />
<br />
; SEVEM <br />
<br />
SEVEM uses all nine Planck frequency channel maps. The 30 - 70 GHz and 353 - 857 GHz maps are used to construct templates by taking the differences (30 - 44) GHz, (44 - 70) GHz, (545 - 353) GHz and (857 - 545) GHz, after smoothing to a common resolution. The 100, 143 and 217 GHz maps are cleaned using the templates.<br />
<br />
<br />
===File names and structure===<br />
<br />
The FITS files corresponding to the three CMB products are the following:<br />
<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-nilc_2048_R1.11.fits|link=COM_CompMap_CMB-nilc_2048_R1.11.fits}}<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-sevem_2048_R1.11.fits|link=COM_CompMap_CMB-sevem_2048_R1.11.fits}}<br />
* {{PLASingleFile|fileType=map|name=COM_CompMap_CMB-smica_2048_R1.11.fits|link=COM_CompMap_CMB-smica_2048_R1.11.fits}}<br />
<br />
and the CMB they contain is shows below.<br />
<br />
<center><br />
<gallery perrow=3 widths=260px heights=170px> <br />
File: CMB-smica.png | SMICA<br />
File: CMB-nilc.png | NILC<br />
File: CMB-sevem.png | SEVEM<br />
</gallery></center><br />
<br />
<br />
The files contains a minimal primary extension with no data and four data extensions which are described in the table below:<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''CMB map file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | Ext. 1. EXTNAME = ''COMP-MAP'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK_cmb || The CMB temperature map<br />
|-<br />
|NOISE || Real*4 || uK_cmb || Estimated noise map (Note 1)<br />
|-<br />
|VALMASK|| Byte || none || Validity, or confidence mask (note 2)<br />
|-<br />
|INPMASK || Byte || none || Inpainted mask (Optional - see Note 3) <br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CMB || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 2. EXTNAME = ''FGDS-LFI'' (BINTABLE) - Note 4<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|LFI_030 || Real*4 || K_cmb || 30 GHz foregrounds<br />
|-<br />
|LFI_044 || Real*4 || K_cmb || 44 GHz foregrounds<br />
|-<br />
|LFI_070 || Real*4 || K_cmb || 70 GHz foregrounds<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 3. EXTNAME = ''FGDS-HFI'' (BINTABLE) - Note 4<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|HFI_100 || Real*4 || K_cmb || 100 GHz foregrounds<br />
|-<br />
|HFI_143 || Real*4 || K_cmb || 143 GHz foregrounds<br />
|-<br />
|HFI_217 || Real*4 || K_cmb || 217 GHz foregrounds<br />
|-<br />
|HFI_353 || Real*4 || K_cmb || 353 GHz foregrounds<br />
|-<br />
|HFI_545 || Real*4 || MJy/sr || 545 GHz foregrounds<br />
|-<br />
|HFI_857 || Real*4 || MJy/sr || 857 GHz foregrounds<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|- bgcolor="ffdead" <br />
!colspan="4" | Ext. 4. EXTNAME = ''BEAM_WF'' (BINTABLE)<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BEAM_WF || Real*4 || uK_cmb || The CMB temperature map<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|LMIN || Int || value || First multipole of beam WF<br />
|-<br />
|LMAX || Int || value || Lsst multipole of beam WF<br />
|-<br />
|METHOD || String ||name || Cleaning method (SMICA/NILC/SEVEM)<br />
|-<br />
|}<br />
<br />
<br />
Notes:<br />
# The half-ring half-difference (HRHD) map is made by passing the half-ring frequency maps independently through the component separation pipeline, then computing half their difference. It approximates a noise realisation, and gives an indication of the uncertainties due to instrumental noise in the corresponding CMB map. <br />
# The confidence mask indicates where the CMB map is considered valid. <br />
# NILC and SMICA CMB maps have been inpainted in the Galactic plane and around some bright sources with a constrained realisation of the signal. The inpainted area covers approximately 3% of the sky. This column is not present in the SEVEM product file.<br />
# The subtraction of the CMB from the sky maps in order to produce the foregrounds map is done after convolving the CMB map to the resolution of the given frequency.<br />
<br />
===Cautionary notes===<br />
<br />
# The half-ring CMB maps are produced by the pipelines with parameters/weights fixed to the values obtained from the full maps. Therefore the CMB HRHD maps do not capture all of the uncertainties due to foreground modelling on large angular scales.<br />
# The HRHD maps for the HFI frequency channels underestimate the noise power spectrum at high l by typically a few percent. This is caused by correlations induced in the pre-processing to remove cosmic ray hits. The CMB is mostly constrained by the HFI channels at high l, and so the CMB HRHD maps will inherit this deficiency in power.<br />
# The beam transfer functions do not account for uncertainties in the beams of the frequency channel maps.<br />
<br />
== Astrophysical foregrounds from parametric component separation ==<br />
<br />
We describe diffuse foreground products for the Planck 2013 release. See Planck Component Separation paper <cite>#planck2013-p06</cite> {{P2013|12}} for a detailed description and astrophysical discussion of those.<br />
<br />
===Product description===<br />
<br />
; Low frequency foreground component<br />
: The products below contain the result of the fitting for one foreground component at low frequencies in Planck bands,along with its spectral behavior parametrized by a power law spectral index. Amplitude and spectral indeces are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on both. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is also provided as a secondary Extension in the N$_\rm{side}$ 2048 product.<br />
<br />
; Thermal dust<br />
: The products below contain the result of the fitting for one foreground component at high frequencies in Planck bands, along with its spectral behavior parametrized by temperature and emissivity. Amplitude, temperature and emissivity are evaluated at N$_\rm{side}$ 256 (see below in the production process), along with standard deviation from sampling and instrumental noise on all of them. An amplitude solution at N$_\rm{side}$=2048 is also given, along with standard deviation from sampling and instrumental noise as well as solutions on halfrings. The beam profile associated to this component is provided. <br />
<br />
; Sky mask<br />
: The delivered mask is defined as the sky region where the fitting procedure was conducted and the solutions presented here were obtained. It is made by masking a region where the Galactic emission is too intense to perform the fitting, plus the masking of brightest point sources.<br />
<br />
===Production process===<br />
<br />
CODE: COMMANDER-RULER. The code exploits a parametrization of CMB and main diffuse foreground observables. The naive resolution of input <br />
frequency channels is reduced to N$_\rm{side}$=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution <br />
by using Markov Chain Monte Carlo analysis using Gibbs sampling. The foreground parameters make the foreground mixing matrix which is <br />
applied to the data at full resolution in order to obtain the provided products at N$_\rm{side}$=2048. In the Planck Component Separation paper <cite>#planck2013-p06</cite> {{p2013|12}}additional material is discussed, specifically concerning the sky region where the solutions are reliable, in terms of chi2 maps.<br />
<br />
===Inputs===<br />
<br />
Nominal frequency maps at 30, 44, 70, 100, 143, 217, 353 GHz ({{PLAFreqMaps|inst=LFI|freq=30|period=Nominal|link=LFI 30 GHz frequency maps}}, {{PLAMaps|inst=LFI|freq=44|period=Nominal|link=LFI 44 GHz frequency maps}} and {{PLAMaps|inst=LFI|freq=70|period=Nominal|link=LFI 70 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=100|period=Nominal|zodi=uncorr|link=HFI 100 GHz frequency maps}}, {{PLAMaps|inst=HFI|freq=143|period=Nominal|zodi=uncorr|link=HFI 143 GHz frequency maps}},{{PLAMaps|inst=HFI|freq=217|period=Nominal|zodi=uncorr|link=HFI 217 GHz frequency maps}} and {{PLAMaps|inst=HFI|freq=353|period=Nominal|zodi=uncorr|link=HFI 353 GHz frequency maps}}) and their II column corresponding to the noise covariance matrix. <br />
Halfrings at the same frequencies. Beam window functions as reported in the [[The RIMO#Beam Window Functions|LFI and HFI RIMO]].<br />
<br />
===Related products===<br />
<br />
None. <br />
<br />
===File names===<br />
<br />
* Low frequency component at N$_\rm{side}$ 256: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits}}<br />
* Low frequency component at N$_\rm{side}$ 2048: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits|link=COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 256: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_0256_R1.00.fits|link=COM_CompMap_dust-commrul_0256_R1.00.fits}}<br />
* Thermal dust at N$_\rm{side}$ 2048: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commrul_2048_R1.00.fits|link=COM_CompMap_dust-commrul_2048_R1.00.fits}}<br />
<br />
* Mask: <br />
: {{PLASingleFile|fileType=map|name=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits|link=COM_CompMap_Mask-rulerminimal_2048_R1.00.fits}}<br />
<br />
===Meta Data===<br />
<br />
====Low frequency foreground component====<br />
<br />
=====Low frequency component at N$_\rm{side}$ 256=====<br />
<br />
File name: COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || uK<math>_{CMB}</math>|| Intensity <br />
|-<br />
|I_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation of intensity <br />
|-<br />
|Beta || Real*4 || || effective spectral index <br />
|-<br />
|B_stdev || Real*4 || || standard deviation on the effective spectral index <br />
|}<br />
<br />
; Notes:<br />
: Comment: The Intensity is normalized at 30 GHz<br />
: Comment: The intensity was estimated during mixing matrix estimation<br />
<br />
Below an example of the header. <br />
<!--pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 16 / width of table in bytes<br />
NAXIS2 = 786432 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'uK_CMB ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT2 = 'uK_CMB ' / physical unit of field<br />
TTYPE3 = 'Beta ' / label for field 3<br />
TFORM3 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT3 = 'none ' / physical unit of field<br />
TTYPE4 = 'B_stdev ' / label for field 4<br />
TFORM4 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT4 = 'none ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-13T13:26:14' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'QXaaRVZTQVaZQVYZ' / HDU checksum updated 2013-02-13T13:26:14<br />
DATASUM = '2752450756' / data unit checksum updated 2013-02-13T13:26:14<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 256 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 786431 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Lfreqfor-commrul_0256_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity is normalized at 30GHz<br />
COMMENT The intensity was estimated during mixing matrix estimation<br />
COMMENT Object:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_amp_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_synch_beta_stddev.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
=====Low frequency component at N$_\rm{side}$ 2048=====<br />
<br />
: File name: COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || uK<math>_{CMB}</math>|| Intensity <br />
|-<br />
|I_stdev || Real*8 || uK<math>_{CMB}</math> || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || uK<math>_{CMB}</math> || Intensity on half ring 2 <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity was computed after mixing matrix application<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
Below an example of the header of the first and second extension respectively. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 32 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT1 = 'uK_CMB ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT2 = 'uK_CMB ' / physical unit of field<br />
TTYPE3 = 'I_hr1 ' / label for field 3<br />
TFORM3 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT3 = 'uK_CMB ' / physical unit of field<br />
TTYPE4 = 'I_hr2 ' / label for field 4<br />
TFORM4 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT4 = 'uK_CMB ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-15T17:12:04' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'dlA5ei24di94di94' / HDU checksum updated 2013-02-15T17:12:13<br />
DATASUM = '3117718572' / data unit checksum updated 2013-02-15T17:12:13<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Lfreqfor-commrul_2048_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity was computed after mixibg matrix application<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_lowfreq.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_lowfreq_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_lowfreq.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_lowfreq.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre><br />
<br />
<pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 1501 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'BeamWF ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'BeamWF '<br />
DATE = '2013-02-15T17:12:17' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '74GA849274E97499' / HDU checksum updated 2013-02-15T17:12:17<br />
DATASUM = '3098248385' / data unit checksum updated 2013-02-15T17:12:17<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
MAX-LPOL= 1500 / Maximum L multipole<br />
POLAR = T / Polarization included (True/False)<br />
BCROSS = T / Magnetic cross terms included (True/False)<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity was computed after mixing matrix application<br />
COMMENT<br />
COMMENT Objects used:<br />
COMMENT<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_beams/dx9_delta_v1_7b_lowfreq_beam.fits<br />
COMMENT<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
====Thermal dust====<br />
<br />
=====Thermal dust component at N$_\rm{side}$=256=====<br />
<br />
: File name: COM_CompMap_dust-commrul_0256_R1.00.fits<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*4 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*4 || MJy/sr || standard deviation of intensity <br />
|-<br />
|Em || Real*4 || || emissivity <br />
|-<br />
|Em_stdev || Real*4 || || standard deviation on emissivity <br />
|-<br />
|T || Real*4 || uK<math>_{CMB}</math> || temperature <br />
|-<br />
|T_stdev || Real*4 || uK<math>_{CMB}</math> || standard deviation on temerature <br />
|}<br />
<br />
; Notes:<br />
: Comment: The intensity is normalized at 353 GHz<br />
<br />
Below an example of the header. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 24 / width of table in bytes<br />
NAXIS2 = 786432 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 6 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'MJy/sr ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT2 = 'MJy/sr ' / physical unit of field<br />
TTYPE3 = 'Em ' / label for field 3<br />
TFORM3 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT3 = 'uK_CMB ' / physical unit of field<br />
TTYPE4 = 'Em_stdev' / label for field 4<br />
TFORM4 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT4 = 'none ' / physical unit of field<br />
TTYPE5 = 'T ' / label for field 5<br />
TFORM5 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT5 = 'uK_CMB ' / physical unit of field<br />
TTYPE6 = 'T_stdev ' / label for field 6<br />
TFORM6 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT6 = 'uK_CMB ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-13T13:31:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '9OAOJO7N9OANGO7N' / HDU checksum updated 2013-02-13T13:31:15<br />
DATASUM = '4139938263' / data unit checksum updated 2013-02-13T13:31:15<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 256 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 786431 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_dust-commrul_0256_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT The intensity is normalized at 353 GHz<br />
COMMENT Object:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_amp_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_em_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_mean.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9delta_v1_dust_T_stddev.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
=====Thermal dust component at N$_\rm{side}$=2048=====<br />
<br />
File name: COM_CompMap_dust-commrul_2048_R1.00.fits<br />
<br />
<br />
: '''Name HDU -- COMP-MAP'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I || Real*8 || MJy/sr || Intensity <br />
|-<br />
|I_stdev || Real*8 || MJy/sr || standard deviation of intensity <br />
|-<br />
|I_hr1 || Real*8 || MJy/sr || Intensity on half ring 1 <br />
|-<br />
|I_hr2 || Real*8 || MJy/sr || Intensity on half ring 2 <br />
|}<br />
<br />
<br />
: '''Name HDU -- BeamWF'''<br />
<br />
The Fits second extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|BeamWF || Real*4 || || beam profile <br />
|}<br />
<br />
; Notes:<br />
: Comment: Beam window function used in the Component separation process<br />
<br />
Below an example of the header of the first and second extension respectively. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 32 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 4 / number of fields in each row<br />
TTYPE1 = 'I ' / label for field 1<br />
TFORM1 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT1 = 'MJy/sr ' / physical unit of field<br />
TTYPE2 = 'I_stdev ' / label for field 2<br />
TFORM2 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT2 = 'MJy/sr ' / physical unit of field<br />
TTYPE3 = 'I_hr1 ' / label for field 3<br />
TFORM3 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT3 = 'MJy/sr ' / physical unit of field<br />
TTYPE4 = 'I_hr2 ' / label for field 4<br />
TFORM4 = 'D ' / data format of field: 8-byte DOUBLE<br />
TUNIT4 = 'MJy/sr ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-16T10:23:15' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '6k8A7i826i896i89' / HDU checksum updated 2013-02-16T10:23:32<br />
DATASUM = '3817117839' / data unit checksum updated 2013-02-16T10:23:32<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_dust-commrul_2048_R1.00.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_avrg_dust_flux.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_stddev/dx9_delta_v1_7b_dust_stddev.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr1_avrg_dust_flux.fits<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/commander-ru<br />
COMMENT ler/delta_dx9/planck/dx9_delta_v1_7b_hr2_avrg_dust_flux.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre><br />
<br />
<pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 3001 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'BeamWF ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'BeamWF '<br />
DATE = '2013-02-16T10:23:34' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= 'FBGWI9EWFAEWF7EW' / HDU checksum updated 2013-02-16T10:23:34<br />
DATASUM = '4096860189' / data unit checksum updated 2013-02-16T10:23:34<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
MAX-LPOL= 3000 / Maximum L multipole<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Beam window function used in the Component separation process<br />
COMMENT<br />
COMMENT Objects used:<br />
COMMENT<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_beams/dx9_delta_v1_7b_dust_beam.fits<br />
COMMENT<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
====Sky mask====<br />
<br />
File name: COM_CompMap_Mask-rulerminimal_2048.fits<br />
<br />
; '''Name HDU -- COMP-MASK'''<br />
<br />
The Fits extension is composed by the columns described below:<br />
{| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"<br />
|+ FITS header<br />
|-<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|Mask || Real*4 || || Mask <br />
|}<br />
<br />
Below an example of the header. <br />
<!-- pre><br />
XTENSION= 'BINTABLE' / binary table extension<br />
BITPIX = 8 / 8-bit bytes<br />
NAXIS = 2 / 2-dimensional binary table<br />
NAXIS1 = 4 / width of table in bytes<br />
NAXIS2 = 50331648 / number of rows in table<br />
PCOUNT = 0 / size of special data area<br />
GCOUNT = 1 / one data group (required keyword)<br />
TFIELDS = 1 / number of fields in each row<br />
TTYPE1 = 'Mask ' / label for field 1<br />
TFORM1 = 'E ' / data format of field: 4-byte REAL<br />
TUNIT1 = 'none ' / physical unit of field<br />
EXTNAME = 'COMP-MAP'<br />
DATE = '2013-02-16T21:07:43' / file creation date (YYYY-MM-DDThh:mm:ss UT)<br />
CHECKSUM= '5fQAAeQ45eQAAeQ3' / HDU checksum updated 2013-02-16T21:07:44<br />
DATASUM = '1075621420' / data unit checksum updated 2013-02-16T21:07:44<br />
COMMENT<br />
COMMENT *** Planck params ***<br />
COMMENT<br />
PIXTYPE = 'HEALPIX ' / HEALPIX pixelisation<br />
ORDERING= 'NESTED ' / Pixel ordering scheme, either RING or NESTED<br />
NSIDE = 2048 / Resolution parameter for HEALPIX<br />
FIRSTPIX= 0 / First pixel # (0 based)<br />
LASTPIX = 50331647 / Last pixel # (0 based)<br />
INDXSCHM= 'IMPLICIT' / Indexing: IMPLICIT or EXPLICIT<br />
OBJECT = 'FULLSKY ' / Sky coverage, either FULLSKY or PARTIAL<br />
BAD_DATA= -1.6375E+30<br />
COORDSYS= 'GALACTIC'<br />
FILENAME= 'COM_CompMap_Mask-rulerminimal_2048.fits'<br />
COMMENT ---------------------------------------------------------------------<br />
COMMENT Objects used:<br />
COMMENT /sci_planck/lfi_dpc_test/ashdown/repository/compsep_outputs/CR-temporary<br />
COMMENT /dx9delta_masks/deltadx9_ruler_mask_total_minimal.fits<br />
COMMENT ---------------------------------------------------------------------<br />
END<br />
</pre --><br />
<br />
== Dust optical depth map and model ==<br />
<br />
Thermal emission from interstellar dust is captured by Planck-HFI over the whole sky, at all frequencies from 100 to 857 GHz. This emission is well modelled by a modified black body in the far-infrared to millimeter range. It is produced by the biggest interstellar dust grain that are in thermal equilibrium with the radiation field from stars. The grains emission properties in the sub-millimeter are therefore directly linked to their absorption properties in the UV-visible range. By modelling the thermal dust emission in the sub-millimeter, a map of dust reddening in the visible can then be constructed. <br />
<br />
; Model of thermal dust emission<br />
<br />
The model of the thermal dust emission is based on a modify black body fit to the data $I_\nu$<br />
<br />
$I_\nu = A\, B_\nu(T)\, \nu^\beta$<br />
<br />
where B_nu(T) is the Planck function for dust equilibirum temperature T, A is the amplitude of the MBB and beta the dust spectral index. The dust optical depth at frequency nu is<br />
<br />
$\tau_\nu = I_\nu / B_\nu(T) = A\, \nu^\beta$<br />
<br />
The dust parameters provided are $T$, beta and $\tau_{353}$. They were obtained by fitting the Planck data at 353, 545 and 857 GHz together with the IRAS (IRIS) 100 micron data. All maps (in Healpix N$_\rm{side}$=2048) were smoothed to a common resolution of 5 arcmin. The CMB anisotropies, clearly visible at 353 GHz, were removed from all the HFI maps using the SMICA map. An offset was removed from each map to obtained a meaningful Galactic zero level, using a correlation with the LAB 21 cm data in diffuse areas of the sky ($N_{HI} < 2\times10^{20} cm^{-2}$). Because the dust emission is so well correlated between frequencies in the Rayleigh-Jeans part of the dust spectrum, the zero level of the 545 and 353 GHz were improved by correlating with the 857 GHz over a larger mask ($N_{HI} < 3\times10^{20} cm^{-2}$). Faint residual dipole structures, identified in the 353 and 545 GHz maps, were removed prior to the fit.<br />
<br />
The MBB fit was performed using a chi-square minimization, assuming errors for each data point that include instrumental noise, calibration uncertainties (on both the dust emission and the CMB anisotropies) and uncertainties on the zero level. Because of the known degeneracy between $T$ and $\beta$ in the presence of noise, we produced a model of dust emission using data smoothed to 35 arcmin; at such resolution no systematic bias of the parameters is observed. The map of the spectral index $\beta$ at 35 arcmin was than used to fit the data for $T$ and $\tau_{353}$ at 5 arcmin. <br />
<br />
; The $E(B-V)$ map <br />
For the production of the $E(B-V)$ map, we used Planck and IRAS data from which point sources in diffuse areas were removed to avoid contamination by galaxies. In the hypothesis of constant dust emission cross-section, the optical depth map $\tau_{353}$ is proportional to dust column density. It can then be used to estimate E(B-V), also proportional to dust column density in the hypothesis of a constant differential absorption cross-section between the B and V bands. Given those assumptions, $ E(B-V) = q\, \tau_{353}$.<br />
<br />
To estimate the calibration factor q, we followed a method similar to <cite>#mortsell2013</cite> based on SDSS reddening measurements ($E(g-r)$ which corresponds closely to $E(B-V)$) of 77 429 Quasars <cite>#schneider2007</cite>. The interstellar HI column densities covered on the lines of sight of this sample ranges from $0.5$ to $10\times10^{20}\,cm^{-2}$. Therefore this sample allows to estimate q in the diffuse ISM where dust properties are expected to vary less than in denser clouds where coagulation and grain growth might modify dust emission and absorption cross sections. <br />
<br />
; Dust optical depth products<br />
<br />
The characteristics of the dust model maps are the following.<br />
* Dust optical depth at 353 GHz : N$_\rm{side}$=2048, fwhm=5 arcmin, no units<br />
* Dust reddening E(B-V) : N$_\rm{side}$=2048, fwhm=5 arcmin, units=magnitude, obtained with data from which point sources were removed.<br />
* Dust temperature : N$_\rm{side}$ 2048, fwhm=5 arcmin, units=Kelvin<br />
* Dust spectral index : N$_\rm{side}$=2048, fwhm=35 arcmin, no units<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Dust opacity file data structure'''<br />
|- bgcolor="ffdead" <br />
! colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
| TAU353 || Real*4 || none || The opacity at 353GHz<br />
|-<br />
| TAU353ERR || Real*4 || none || Error in the opacity<br />
|-<br />
| EBV || Real*4 || mag || E(B-V)<br />
|-<br />
| EBV_ERR || Real*4 || mag || Error in E(B-V)<br />
|-<br />
|T_HF || Real*4 || K || Temperature for the high frequency correction<br />
|-<br />
|T_HF_ERR || Real*4 || K || Error on the temperature<br />
|-<br />
| BETAHF || Real*4 || none || Beta for the high frequency correction<br />
|-<br />
| BETAHFERR || Real*4 || none || Error on beta<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
| AST-COMP || String || DUST-OPA|| Astrophysical compoment name<br />
|-<br />
| PIXTYPE || String || HEALPIX ||<br />
|-<br />
| COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
| ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
| NSIDE || Int || 2048 || Healpix N$_\rm{side}$ for LFI and HFI, respectively<br />
|-<br />
| FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
| LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|}<br />
<br />
== CO emission maps ==<br />
<br />
CO rotational transition line emission is present in all HFI bands but for the 143 GHz channel. It is especially significant in the 100, 217 and 353 GHz channels (due to the 115 (1-0), 230 (2-1) and 345 GHz (3-2) CO transitions). This emission comes essentially from the Galactic interstellar medium and is mainly located at low and intermediate Galactic latitudes. Three approaches (summarised below) have been used to extract CO velocity-integrated emission maps from HFI maps and to make three types of CO products. An introduction is given in [[Science#CO_maps|Section]] and a full description of these products is given in <cite>#planck2013-p03a</cite>.<br />
* Type 1 product: it is based on a single channel approach using the fact that each CO line has a slightly different transmission in each bolometer at a given frequency channel. These transmissions can be evaluated from bandpass measurements that were performed on the ground or empirically determined from the sky using existing ground-based CO surveys. From these, the J=1-0, J=2-1 and J=3-2 CO lines can be extracted independently. As this approach is based on individual bolometer maps of a single channel, the resulting Signal-to-Noise ratio (SNR) is relatively low. The benefit, however, is that these maps do not suffer from contamination from other HFI channels (as is the case for the other approaches) and are more reliable, especially in the Galactic Plane.<br />
<br />
* Type 2 product: this product is obtained using a multi frequency approach. Three frequency channel maps are combined to extract the J=1-0 (using the 100, 143 and 353 GHz channels) and J=2-1 (using the 143, 217 and 353 GHz channels) CO maps. Because frequency channels are combined, the spectral behaviour of other foregrounds influences the result. The two type 2 CO maps produced in this way have a higher SNR than the type 1 maps at the cost of a larger possible residual contamination from other diffuse foregrounds.<br />
<br />
* Type 3 product: using prior information on CO line ratios and a multi-frequency component separation method, we construct a combined CO emission map with the largest possible SNR. This type 3 product can be used as a sensitive finder chart for low-intensity diffuse CO emission over the whole sky.<br />
<br />
The released Type 1 CO maps have been produced using the MILCA-b algorithm, Type 2 maps using a specific implementation of the Commander algorithm, and the Type 3 map using the full Commander-Ruler component separation pipeline (see [[Astrophysical_component_maps#Maps_of_astrophysical_foregrounds|above]]).<br />
<br />
Characteristics of the released maps are the following. We provide Healpix maps with N$_\rm{side}$=2048. For one transition, the CO velocity-integrated line signal map is given in K_RJ.km/s units. A conversion factor from this unit to the native unit of HFI maps (K_CMB) is provided in the header of the data files and in the RIMO. Four maps are given per transition and per type:<br />
* The signal map<br />
* The standard deviation map (same unit as the signal), <br />
* A null test noise map (same unit as the signal) with similar statistical properties. It is made out of half the difference of half-ring maps.<br />
* A mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.<br />
<br />
All products of a given type belong to a single file.<br />
Type 1 products have the native HFI resolution i.e. approximately 10, 5 and 5 arcminutes for the CO 1-0, 2-1, 3-2 transitions respectively.<br />
Type 2 products have a 15 arcminute resolution<br />
The Type 3 product has a 5.5 arcminute resolution.<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-1 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map<br />
|-<br />
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity<br />
|-<br />
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable<br />
|-<br />
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map<br />
|-<br />
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity<br />
|-<br />
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable<br />
|-<br />
|I32 || Real*4 || K_RJ km/sec || The CO(3-2) intensity map<br />
|-<br />
|E32 || Real*4 || K_RJ km/sec || Uncertainty in the CO(3-2) intensity<br />
|-<br />
|N32 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M32 || Byte || none || Region over which the CO(3-2) intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || string || CO-TYPE2 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix N$_\rm{side}$ for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 3-2 || Real*4 || value || Factor to convert CO(3-2) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-2 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map<br />
|-<br />
|E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity<br />
|-<br />
|N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable<br />
|-<br />
|-<br />
|I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map<br />
|-<br />
|E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity<br />
|-<br />
|N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CO-TYPE2 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s)) <br />
|-<br />
|CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''Type-3 CO map file data structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'COMP-MAP' <br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|INTEN || Real*4 || K_RJ km/sec || The CO intensity map<br />
|-<br />
|ERR || Real*4 || K_RJ km/sec || Uncertainty in the intensity<br />
|-<br />
|NUL || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps<br />
|-<br />
|MASK || Byte || none || Region over which the intensity is considered reliable<br />
|-<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|AST-COMP || String || CO-TYPE1 || Astrophysical compoment name<br />
|-<br />
|PIXTYPE || String || HEALPIX ||<br />
|-<br />
|COORDSYS || String || GALACTIC ||Coordinate system <br />
|-<br />
|ORDERING || String || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|CNV || Real*4 || value || Factor to convert to Kcmb (units Kcmb/(Krj*km/s)) <br />
|}<br />
<br />
== References ==<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
<br />
<br />
[[Category:Mission products|007]]</div>Lvibert