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=Map-Making and photometric calibration=
+
{{DISPLAYTITLE:Mapmaking and photometric calibration}}
 
 
 
== Introduction ==
 
== Introduction ==
  
This page will give an overview of the map-making and photometric calibration procedures used by the HFI DPC to build detector and frequency maps.  
+
This section will give an overview of the mapmaking and photometric calibration procedures used by the HFI DPC to build detector and frequency maps for the 2015 data release.  They are described in {{PlanckPapers|planck2014-a09}}.
This processing and its performances are described in the <span style="color:red">[[XXXXXX|the HFI DPC Paper]]</span> and the <span style="color:red">[[XXXXXX|the HFI DPC Calibration co-Paper]]</span>
+
These have common elements with the tools used for the 2013 release that are described in {{PlanckPapers|planck2013-p03}} and {{PlanckPapers|planck2013-p03b}}.  
[which will be completed prior to this page].
 
  
To build HFI maps, we use the destriping approximation, in which noise is assumed to decompose into two components : white noise plus low frequency drifts. Using the sky redundancy, the low frequency drifts are modelled as one constant, or offset, per pointing period. To speed up the ulterior processing we first build intermediate products, by taking advantage of redundancies : we average signal and detector orientation on healpix pixels visited during  
+
To build HFI maps, we use the destriping approximation, in which noise is assumed to decompose into two components, namely white noise plus low frequency drifts. Using the sky redundancy, the low frequency drifts are modelled as one constant, or offset, per pointing period. To speed up the subsequent processing we first build intermediate products, by taking advantage of redundancies.  We average signal and detector orientation on HEALPix pixels visited during  
each fixed pointing period, which we call hereafter 'ring'. This intermediate product is called HPR for healpix pixel ring. They have been constructed using the same map resolution as the final HFI products (correspondontg to nside=2048).  
+
each fixed pointing period, which we call hereafter a "ring."  The detector pointing is corrected for slow drifts and aberration (displacement on the sky induced by the satellite's motion). This intermediate product is called HPR for HEALPix pixel ring." These have been constructed using the same map resolution as the final HFI products (corresponding to <i>N</i><sub>side</sub>=2048).  
This new dataset is used as input in the following steps.  
+
This new data set is used as input for the following steps.
  
 
== Photometric calibration ==
 
== Photometric calibration ==
  
=== dipole calibration (100 to 353 GHz) ===
+
=== Dipole calibration (100 to 353 GHz) ===
  
For the 2013 data release, the calibrator for the CMB frequency was the Solar dipole, as measured by the WMAP team (G. Hinshaw et al., Astrophys.J.Suppl.180:225-245,2009).  
+
For the 2015 data release, the HFI CMB channels were calibrated using the orbital dipole modulation. This time-variable anisotropy results from the motion of the spacecraft in the solar system, which is precisely known. Thus it provides an absolute calibrator for orbital CMB missions. Its measurement is now used to calibrate HFI data, thanks to the improvements in the time stability of the data
We use a two components template fitting procedure, performed for each detector independently, to determine ring by ring an estimation of the dipole gain.
+
brought by the ADC nonlinearity corrections and a better characterization of the time response of the detectors.  
The two fitted components are the Solar dipole and a sky template. We used the PSM for thermal dust emission at the detector's frequency as a first approximation of the sky template in pur early release. Using the HFI channel map as a template brings negligible change in the averaged gain, but reduces the systematic ring-to-ring dispersion of our estimation.  We average these estimations over a subset of rings in the first survey (2000 to 6000) in which the dipole's amplitude is high enough with respect to that of the sky template, to get a single dipole gain per detector.
 
  
Several pieces of evidence led us to the conclusion that out bolometers presented apparent gain variation with time, after comparing the 3rd scan of the sky with the first one. This was later (mid-2012) explained by inequalities in the steps of the analog-to-digital converters (ADC) used in each bolometer's electronic chain. These devices had to  be characterized using warm data after the end of the HFI observations. This process is still on-going (01/2012).
+
Residual time response slow components are modelled as a dipole shifted by 90&deg; in phase, whose amplitude is fitted bolometer per bolometer. To mitigate residual systematics, we perform a simultaneous fit of the detectors gains on the orbital dipole. This amounts to solving the nonlinear equation
 +
<math> \displaystyle{d\ =\ g_i.(S+D) + O_i + n},
 +
\label{nlequat}</math>
  
In the mean time we used an empiric correction, looking for a gain estimation and an offset per ring. This amounts to solve the non-linear equation :
+
where <i>d</i> is the detector measurement, <i>D</i> the total dipole component, <i>n</i> the (white) noise, and <i>S</i> the sky signal, <i>g</i> the detector gain, <i>O</i> the offset (for ring number <i>i</i>) are the unknowns to be determined.  
<math> \displaystyle{d\ =\  g_i.S + O_i + n}
+
This is done by linearizing the above equation to look for gains and sky variations, and iterating by updating the approximate sky and gains.  
\label{nlequat}</math>
 
  
where d is s the detector measurement, both S the sky signal, g the detector gain, O the offset (for ring no i) are the unknowns to be determined, and n the noise.
 
We linearized this equation starting from the constant gain approximation, to get a measurement of the apparent time-varying gains for each bolometer independently. The limitations of this process are intrinsic signal variability from one observation to the other, like polarization or intra-pixel gradient. This procedure was thus only used for the 100 to 217 GHz detectors, for which the dipole signal is brighter and  galactic signal (and polarization). A mask was used to removed the inner part of the Galactic plane.
 
 
  
 
=== Higher frequency calibration (545 and 857 GHz) ===
 
=== Higher frequency calibration (545 and 857 GHz) ===
  
We therefore finally derived the sub-mm channels' calibration for the 2013 Planck data release from the comparison of measurements of the Neptune and Uranus fluxes (with aperture photometry) with  their expectations from the Moreno et al model of their atmospheres' emission. This procedure is justified, since for both planets, at the  lower frequencies (100-353 Ghz), the fluxes we recover are in agreement within ~ +/-5\% with what is expected from the planet spectral model, and the HFI detector's band-passes.
+
We derived the sub-mm channels' calibration for the 2015 Planck data release from comparison of measurements of the Neptune and Uranus flux densities (using aperture photometry) with  their expectations from the Moreno et al. model of their atmospheric emission. This procedure is justified, since for both planets, at the  lower frequencies (100-353 GHz), the flux densities we recover are in agreement within approximately &plusmn;5% of what is expected from the planet spectral model, given the HFI detector bandpasses.
 
 
We determined zero-level for the released maps, by imposing that their average in regions where, according to HI template, dust emission is zero, be equal to that of the CIB model of Bethermin et al.
 
  
 +
=== Zero levels === 
 +
We determined zero-levels for the released maps in selected regions of the sky where dust emission is low and well-correlated with HI. We may thus estimate and subtract dust emission using the HI template, and CMB using a Planck component-separated template. The remaining astrophysical zero level should be that of the CIB. By imposing that the level we find is equal to that of the CIB model of B&eacute;thermin et al., we thereby set the zero level of our maps.
  
== Building of Maps ==  
+
== Building of maps ==  
  
Using the photometric calibration parameters, we build maps in two steps :  
+
Using the photometric calibration parameters, we build maps in two steps:  
  
* we determine the destriping offsets using the full mission data
+
* we determine the destriping offsets using the full mission data for all detectors of a given frequency;
* we build the maps, using these offsets, by inverting the  photometric equation :
+
* we build the maps, using these offsets, by inverting the  photometric equation
  
<math> \displaystyle{d_i  = g(I^p+\eta [Q^p cos(2\psi_i) + U^p sin(2\psi_i)]) + n}
+
<math> \displaystyle{d_i  = g(I^p+\eta [Q^p cos(2\psi_i) + U^p sin(2\psi_i)]) + n}.
 
\label{photeq}</math>
 
\label{photeq}</math>
where d is the destriped and calibrated signal at the HPR level. Detector's data are combined with an inverse noise weights derived from each detector's NEP. Q and U maps are build whenever possible. We propagate the white noise by building the 3x3 (or 1x1 if only I is reconstructed) covariance matrices in each pixel.  
+
 
 +
Here <i>d</i> is the destriped and calibrated signal at the HPR level. The detector data are combined with inverse noise weights derived from each detector's NEP. <i>Q</i>, and <i>U</i> maps are built whenever possible. We propagate the white noise by building the 3&times;3 (or 1&times;1 if only <i>I</i> is reconstructed) covariance matrices in each pixel.  
 
At each frequency we build maps combining all detectors and independent detector sets.  
 
At each frequency we build maps combining all detectors and independent detector sets.  
We use the offsets build for the full mission for building maps for each scan survey and for the nominal mission duration.  
+
We use the offsets built for the full mission for constructing maps for each scan survey, year (combination of Surveys 1 and 2 or 3 and 4, respectively), and for the full, nominal mission duration and its two halves.  
We also build maps from the two independent halves of each rings. Altogether, more than 6000 maps are built at each release.  
+
We also build maps from the two independent halves of each ring. Altogether, more than 8000 maps are built at each release.  
  
 +
HPR and maps are built in Galactic coordinates.
  
 
== Noise properties ==
 
== Noise properties ==
  
Map noise properties can be evaluated using several methods, thanks to the high level of observation redundancies.  
+
Map noise properties can be evaluated using several methods, thanks to the high level of observational redundancy.  
We can use the maps built from the difference between the first and second half of each rings, or compare individual sky scans, of detector sets with each other.  
+
We can use the maps built from the differences between the first and second halves of each ring, or compare individual sky scans, years, half-mission or independent detector sets with each other
 +
Some of these tests are described in {{PlanckPapers|planck2014-a09}}.
  
Low resolution (nside = 8, 16, 32 ?) pixel-to-pixel noise covariance matrices are build using an analytic approach from the measured noise power spectra.
+
Low resolution (<i>N</i><sub>side</sub> = 8, 16) pixel-to-pixel noise covariance matrices are built from the measured noise power spectra using an analytic approach.
  
== Zodi correction ==
+
== Zodiacal light correction ==
  
At the highest Planck frequencies, Zodiacal emission is visible in a survey difference map:
+
At the highest Planck frequencies, zodiacal light emission is visible in a survey difference map, shown below.
  
[[File:857GHz_I_S2mS1.png|600px|857 GHz Survey 2 - Survey 1 Difference]]
+
[[File:Z857SurveyJackknifeWiZodi.png|500px|thumb|center|2013 Release 857-GHz Survey 2 - Survey 1 difference.]]
  
This map is a difference between the 857 GHz Survey 2 map and the 857 GHz Survey 1 map. This difference effectively removes Galactic and other emissions which originate far from Planck. As the Solar elongation is different for measurements of the same point on the sky for the two surveys, we see Zodiacal emission, while all emission from further sources is removed. The zodiacal emission follows the Ecliptic plane, which starts at the lower left of the image, then crosses the center of the plot towards the upper right. Note that the "arcs" at the top and bottom of the image are images of the Galactic center in the Far Sidelobes, which are discussed in the section below. Note also that the image above is from an early processing and will be updated.  
+
This map is a difference between the 857-GHz Survey 2 map and the 857-GHz Survey 1 map. This difference effectively removes Galactic and other emission that originates far from Planck. As the Solar elongation is different for measurements of the same point on the sky for the two surveys, we see zodiacal light emission, while all emission from further sources is removed. The zodiacal light emission follows the Ecliptic plane, which starts at the lower left of the image, then crosses the centre of the plot towards the upper right. Note that the "arcs" at the top and bottom of the image are images of the Galactic centre in the far sidelobes, which are discussed in the section below. Similar plots for other HFI frequencies, for maps both before and after zodiacal light removal, are shown [[beforeAndAfterSurveyDifferences|here]].
  
Zodiacal Emission is removed from the 353, 545 and 857 GHz channels. It is described in <span style="color:red">[[XXXXXX|the HFI DPC Paper]]</span>, but a synopsis of the procedure is as follows:
+
For the 2015 Planck release, zodiacal light emission is removed from all HFI channels. The general procedure is described in {{PlanckPapers|planck2013-p03}}, but a synopsis of the procedure is as follows.
* During each survey, a large fraction of the sky has observations which all fall within a week of each other. That is, during a single survey, most pixels are observed during a short, well-defined period. The contribution from Zodiacal Emission to the total brightness seen, then, is well defined.  
+
* During each survey, a large fraction of the sky has observations that all fall within a week of each other. That is, during a single survey, most pixels are observed during a short, well-defined period. The contribution from zodiacal light emission to the total brightness seen is then well defined.  
* We use the the COBE model of the Zodiacal Light to make predictions for this Zodiacal emission for those pixels observed over a span of one week or less, and use GRASP models of the beams to predict the emission from the Galaxy given our sidelobes.  
+
* We use the the COBE model of the zodiacal light to make predictions for this emission for those pixels observed over a span of one week or less. The templates from the COBE model are shown [[COBEZodiModelTemplates|here]].
* We fit the survey difference maps with these model templates to estimate the emissivity of each Zodi component and sidelobe at the Planck wavelengths. The results of these fits at each frequency are shown [[zodiFreqFits|here]].  
+
* We fit the survey difference maps with these model templates to estimate the emissivity of each zodiacal light component at the Planck wavelengths. The results of these fits at each frequency are given in {{PlanckPapers|planck2014-a09}}.
* We reconstruct each ring of the the full mission using the combination of the COBE geometric model with the emissivities determined above and the sidelobe models.  
+
* We reconstruct each ring of the the full mission using the combination of the COBE geometric model with the emissivities determined above.  
 
* We remove the reconstruction above from each ring of data.  
 
* We remove the reconstruction above from each ring of data.  
* We then make maps as described previously in this section. Maps with and without, as well as the differences between the two, are shown [[withAndWithoutRemoval|here]]. The survey differences before and after this removal are shown with and without Zodical emission removal [[beforeAndAfterSurveyDifferences|here]]. The power spectra of what is removed from each map is shown [[zodiCorrectionSpectra|here]].
+
* We then make maps as described previously in this section.
 +
 
 +
== Far SideLobes (FSL)==
  
== Far Sidelobes ==
+
Contrary to the 2013 Planck release, far sidelobes were not removed from the HFI data for the 2015 Planck release.
 +
The change of the gain due to the neglect of the far sidelobes is calculated by fitting the dipole to full timeline simulations of the dipole convolved with the FSL. The correction factors applied to the data are 0.09 % at 100 GHz, 0.05 % at 143 GHz, 0.04 % at 217 GHz and negligible at 353 GHz. Corrections were not made at 545 and 857 GHz (see {{PlanckPapers|planck2014-a09}} for details).
  
The far sidelobe correction for the highest frequency HFI channels is described in [[Map-making#Zodi correction|the section above]]. Note that this correction is done only for the 857 and 545 GHz channels, as it is not seen at longer wavelengths. As for the Zodical emission correction, it is not important for the CMB.
+
== CO maps ==
  
We have made estimates of the contamination of the far sidelobes at 143 GHz by taking the 143 GHz map, adding the dipole, and passing it through our simulator, using a GRASP calculation of the far sidelobes for the 143-1a detector as the beam. The resulting maps is shown here:
+
Carbon monoxide rotational transition line emission is present in all HFI bands except for the 143-GHz
[[File:FSLMap.png|600px|Estimated Spurious Far Sidelobe Signal]]
+
channel. It is especially significant in the 100, 217, and 353 GHz channels (due to the 115GHz
 +
(1-0), 230GHz (2-1) and 345GHz (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 (summarized below) have been used to extract CO velocity-integrated
 +
emission maps from HFI data and to generate the CO products. See
 +
{{PlanckPapers|planck2013-p03a}} and {{PlanckPapers|planck2014-a12}} for a full description.
  
While there is one small region that might reach 20 micro-K (this happens when the secondary spillover overlaps with the Galactic center), most of the map is quite quiet. This is evidenced by the power spectrum of the above map, which is quite small.
+
*"Type 1" product: this is based on a single channel approach, using the fact that each CO
[[File:FSLCl.png|300px|Estimated Spurious Far Sidelobe Power Spectrum]]
+
line has a slightly different transmission in each bolometer at a given frequency channel.
 +
From this, the <i>J</i>=1-0, <i>J</i>=2-1, and <i>J</i>=3-2 CO lines can be extracted independently. Since this
 +
approach is based on individual bolometer maps of a single channel, the resulting
 +
S/N 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.  
  
== CO Correction ==
+
*"Type 2" product: this product is obtained using a multi-frequency approach. Three
 +
frequency channel maps are combined to extract the <i>J</i>=1-0 (using the 100, 143, and 353
 +
GHz channels) and <i>J</i>=2-1 (using the 143, 217, and 353 GHz channels) CO maps. Since
 +
frequency maps are combined, the spectral behaviour of other foregrounds influences
 +
the result. The two Type 2 CO maps produced in this way have a higher S/N than the
 +
Type 1 maps, at the cost of a larger residual contamination from other diffuse foregrounds.
  
This is described in the <span style="color:red">[[XXXXXX|the CO Paper]]</span>. The CO maps are produced by a combination of bolometer maps or frequency maps. This is summarized [[http://www.sciops.esa.int/wikiSI/planckpla/index.php?title=Science&instance=Planck_PLA_ES#CO_maps |here]]
+
*"Type 3" product: no Type 3 product (as defined in 2013) has been produced for the
 +
2015 release. Instead, this has been is superseded by a high-resolution CO(2-1) map (FWHM=7.5')
 +
produced by the Commander component separation pipeline. Note that low
 +
resolution (FWHM=1&deg;) CO maps of the three lines have also been produced using
 +
Commander. See section 5 of {{PlanckPapers|planck2014-a12}} for a complete description.
 +
 
 +

The 2015 Type 1 and Type 2 CO maps have been produced using the same procedure as
 +
for the 2013 results. Very similar to their 2013 counterparts, the 2015 maps benefit from
 +
an increased S/N due to the use of the full, rather than nominal, mission data.
 +

Characteristics of the released maps are the following. We provide HEALPix maps with
 +
<i>N</i><sub>side</sub>=2048. For one transition, the CO velocity-integrated line signal map is given in
 +
K<sub>RJ</sub> km s<sup>-1</sup> units. A conversion factor from this unit to the native unit of HFI maps (K<sub>CMB</sub>)
 +
is provided in the header of the data files and in the RIMO. Four maps are given per
 +
transition and per type:
 +
* the signal map;
 +
* the standard deviation map (same units as the signal);
 +
* a null-test noise map (same units as the signal) with similar statistical properties, which is made out of half the difference of half-ring maps;
 +
* a mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.
 +
 +
All products of a given type belong to a single file. Type 1 products have the native HFI
 +
resolution. i.e.. approximately 10, 5, and 5 arcmin for the CO 1-0, 2-1, and 3-2 transitions,
 +
respectively. Type 2 products have a 15 arcmin resolution.
 +

We refer the reader to section 5 of {{PlanckPapers|planck2014-a12}} for a
 +
description and characteristics of the Commander CO products.
  
 
== Map validation ==
 
== Map validation ==
  
 +
Several validations of HFI maps are described in {{PlanckPapers|planck2014-a08}}  and in {{PlanckPapers|planck2014-a09}}.
 +
 +
Further checks are presented in the likelihood, parameters, component separation, and Commander papers.
 +
 +
== References ==
 +
<References />
 +
  
[[Category:Data processing]]
+
[[Category:HFI data processing|004]]

Latest revision as of 12:56, 7 July 2015

Introduction[edit]

This section will give an overview of the mapmaking and photometric calibration procedures used by the HFI DPC to build detector and frequency maps for the 2015 data release. They are described in Planck-2015-A08[1]. These have common elements with the tools used for the 2013 release that are described in Planck-2013-VI[2] and Planck-2013-VIII[3].

To build HFI maps, we use the destriping approximation, in which noise is assumed to decompose into two components, namely white noise plus low frequency drifts. Using the sky redundancy, the low frequency drifts are modelled as one constant, or offset, per pointing period. To speed up the subsequent processing we first build intermediate products, by taking advantage of redundancies. We average signal and detector orientation on HEALPix pixels visited during each fixed pointing period, which we call hereafter a "ring." The detector pointing is corrected for slow drifts and aberration (displacement on the sky induced by the satellite's motion). This intermediate product is called HPR for HEALPix pixel ring." These have been constructed using the same map resolution as the final HFI products (corresponding to Nside=2048). This new data set is used as input for the following steps.

Photometric calibration[edit]

Dipole calibration (100 to 353 GHz)[edit]

For the 2015 data release, the HFI CMB channels were calibrated using the orbital dipole modulation. This time-variable anisotropy results from the motion of the spacecraft in the solar system, which is precisely known. Thus it provides an absolute calibrator for orbital CMB missions. Its measurement is now used to calibrate HFI data, thanks to the improvements in the time stability of the data brought by the ADC nonlinearity corrections and a better characterization of the time response of the detectors.

Residual time response slow components are modelled as a dipole shifted by 90° in phase, whose amplitude is fitted bolometer per bolometer. To mitigate residual systematics, we perform a simultaneous fit of the detectors gains on the orbital dipole. This amounts to solving the nonlinear equation [math] \displaystyle{d\ =\ g_i.(S+D) + O_i + n}, \label{nlequat}[/math]

where d is the detector measurement, D the total dipole component, n the (white) noise, and S the sky signal, g the detector gain, O the offset (for ring number i) are the unknowns to be determined. This is done by linearizing the above equation to look for gains and sky variations, and iterating by updating the approximate sky and gains.


Higher frequency calibration (545 and 857 GHz)[edit]

We derived the sub-mm channels' calibration for the 2015 Planck data release from comparison of measurements of the Neptune and Uranus flux densities (using aperture photometry) with their expectations from the Moreno et al. model of their atmospheric emission. This procedure is justified, since for both planets, at the lower frequencies (100-353 GHz), the flux densities we recover are in agreement within approximately ±5% of what is expected from the planet spectral model, given the HFI detector bandpasses.

Zero levels[edit]

We determined zero-levels for the released maps in selected regions of the sky where dust emission is low and well-correlated with HI. We may thus estimate and subtract dust emission using the HI template, and CMB using a Planck component-separated template. The remaining astrophysical zero level should be that of the CIB. By imposing that the level we find is equal to that of the CIB model of Béthermin et al., we thereby set the zero level of our maps.

Building of maps[edit]

Using the photometric calibration parameters, we build maps in two steps:

  • we determine the destriping offsets using the full mission data for all detectors of a given frequency;
  • we build the maps, using these offsets, by inverting the photometric equation

[math] \displaystyle{d_i = g(I^p+\eta [Q^p cos(2\psi_i) + U^p sin(2\psi_i)]) + n}. \label{photeq}[/math]

Here d is the destriped and calibrated signal at the HPR level. The detector data are combined with inverse noise weights derived from each detector's NEP. Q, and U maps are built whenever possible. We propagate the white noise by building the 3×3 (or 1×1 if only I is reconstructed) covariance matrices in each pixel. At each frequency we build maps combining all detectors and independent detector sets. We use the offsets built for the full mission for constructing maps for each scan survey, year (combination of Surveys 1 and 2 or 3 and 4, respectively), and for the full, nominal mission duration and its two halves. We also build maps from the two independent halves of each ring. Altogether, more than 8000 maps are built at each release.

HPR and maps are built in Galactic coordinates.

Noise properties[edit]

Map noise properties can be evaluated using several methods, thanks to the high level of observational redundancy. We can use the maps built from the differences between the first and second halves of each ring, or compare individual sky scans, years, half-mission or independent detector sets with each other. Some of these tests are described in Planck-2015-A08[1].

Low resolution (Nside = 8, 16) pixel-to-pixel noise covariance matrices are built from the measured noise power spectra using an analytic approach.

Zodiacal light correction[edit]

At the highest Planck frequencies, zodiacal light emission is visible in a survey difference map, shown below.

2013 Release 857-GHz Survey 2 - Survey 1 difference.

This map is a difference between the 857-GHz Survey 2 map and the 857-GHz Survey 1 map. This difference effectively removes Galactic and other emission that originates far from Planck. As the Solar elongation is different for measurements of the same point on the sky for the two surveys, we see zodiacal light emission, while all emission from further sources is removed. The zodiacal light emission follows the Ecliptic plane, which starts at the lower left of the image, then crosses the centre of the plot towards the upper right. Note that the "arcs" at the top and bottom of the image are images of the Galactic centre in the far sidelobes, which are discussed in the section below. Similar plots for other HFI frequencies, for maps both before and after zodiacal light removal, are shown here.

For the 2015 Planck release, zodiacal light emission is removed from all HFI channels. The general procedure is described in Planck-2013-VI[2], but a synopsis of the procedure is as follows.

  • During each survey, a large fraction of the sky has observations that all fall within a week of each other. That is, during a single survey, most pixels are observed during a short, well-defined period. The contribution from zodiacal light emission to the total brightness seen is then well defined.
  • We use the the COBE model of the zodiacal light to make predictions for this emission for those pixels observed over a span of one week or less. The templates from the COBE model are shown here.
  • We fit the survey difference maps with these model templates to estimate the emissivity of each zodiacal light component at the Planck wavelengths. The results of these fits at each frequency are given in Planck-2015-A08[1].
  • We reconstruct each ring of the the full mission using the combination of the COBE geometric model with the emissivities determined above.
  • We remove the reconstruction above from each ring of data.
  • We then make maps as described previously in this section.

Far SideLobes (FSL)[edit]

Contrary to the 2013 Planck release, far sidelobes were not removed from the HFI data for the 2015 Planck release. The change of the gain due to the neglect of the far sidelobes is calculated by fitting the dipole to full timeline simulations of the dipole convolved with the FSL. The correction factors applied to the data are 0.09 % at 100 GHz, 0.05 % at 143 GHz, 0.04 % at 217 GHz and negligible at 353 GHz. Corrections were not made at 545 and 857 GHz (see Planck-2015-A08[1] for details).

CO maps[edit]

Carbon monoxide rotational transition line emission is present in all HFI bands except for the 143-GHz channel. It is especially significant in the 100, 217, and 353 GHz channels (due to the 115GHz (1-0), 230GHz (2-1) and 345GHz (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 (summarized below) have been used to extract CO velocity-integrated emission maps from HFI data and to generate the CO products. See Planck-2013-XIII[4] and Planck-2015-A10[5] for a full description.

  • "Type 1" product: this 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. From this, the J=1-0, J=2-1, and J=3-2 CO lines can be extracted independently. Since this approach is based on individual bolometer maps of a single channel, the resulting S/N 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.

  • "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. Since frequency maps are combined, the spectral behaviour of other foregrounds influences the result. The two Type 2 CO maps produced in this way have a higher S/N than the Type 1 maps, at the cost of a larger residual contamination from other diffuse foregrounds.

  • "Type 3" product: no Type 3 product (as defined in 2013) has been produced for the

2015 release. Instead, this has been is superseded by a high-resolution CO(2-1) map (FWHM=7.5') produced by the Commander component separation pipeline. Note that low resolution (FWHM=1°) CO maps of the three lines have also been produced using Commander. See section 5 of Planck-2015-A10[5] for a complete description.


The 2015 Type 1 and Type 2 CO maps have been produced using the same procedure as for the 2013 results. Very similar to their 2013 counterparts, the 2015 maps benefit from an increased S/N due to the use of the full, rather than nominal, mission data. 
Characteristics of the released maps are the following. We provide HEALPix maps with Nside=2048. For one transition, the CO velocity-integrated line signal map is given in KRJ km s-1 units. A conversion factor from this unit to the native unit of HFI maps (KCMB) is provided in the header of the data files and in the RIMO. Four maps are given per transition and per type:

  • the signal map;
  • the standard deviation map (same units as the signal);
  • a null-test noise map (same units as the signal) with similar statistical properties, which is made out of half the difference of half-ring maps;
  • a mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.


 All products of a given type belong to a single file. Type 1 products have the native HFI resolution. i.e.. approximately 10, 5, and 5 arcmin for the CO 1-0, 2-1, and 3-2 transitions, respectively. Type 2 products have a 15 arcmin resolution. 
We refer the reader to section 5 of Planck-2015-A10[5] for a description and characteristics of the Commander CO products.

Map validation[edit]

Several validations of HFI maps are described in Planck-2015-A07[6] and in Planck-2015-A08[1].

Further checks are presented in the likelihood, parameters, component separation, and Commander papers.

References[edit]

(Planck) High Frequency Instrument

Data Processing Center

(Hierarchical Equal Area isoLatitude Pixelation of a sphere, <ref name="Template:Gorski2005">HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere, K. M. Górski, E. Hivon, A. J. Banday, B. D. Wandelt, F. K. Hansen, M. Reinecke, M. Bartelmann, ApJ, 622, 759-771, (2005).

[LFI meaning]: absolute calibration refers to the 0th order calibration for each channel, 1 single number, while the relative calibration refers to the component of the calibration that varies pointing period by pointing period.

Cosmic Microwave background

analog to digital converter

Noise Equivalent Power

Full-Width-at-Half-Maximum

reduced IMO