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| − | = Astrophysical Components= | + | = 2018 Astrophysical Components= |
| | | | |
| | == Overview == | | == Overview == |
| | 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 each product and how it is obtained, followed by a description of the FITS file containing the data and associated information. | | 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 each product and how it is obtained, followed by a description of the FITS file containing the data and associated information. |
| − | All the details can be found in {{PlanckPapers|planck2014-a12}}, {{PlanckPapers|planck2016-l04}} and {PlanckPapers|planck20}}. | + | All the details can be found in {{PlanckPapers|planck2016-l04}} and {{PlanckPapers|planck2016-l08}}. |
| | | | |
| − | == Astrophysical foregrounds from Commander == | + | == Commander-derived astrophysical foreground maps == |
| | As discussed in detail in {{PlanckPapers|planck2016-l04}}, the main Planck 2018 frequency sky maps have significantly lower systematic errors than earlier versions. At the same time, these maps are also associated with a significant limitation, in that no robust single detector or detector set maps are available. As described in {{PlanckPapers|planck2016-l03}}, such maps do not contain the full signal content of the true sky. As a result, only full frequency maps are distributed and used in the 2018 analysis. | | As discussed in detail in {{PlanckPapers|planck2016-l04}}, the main Planck 2018 frequency sky maps have significantly lower systematic errors than earlier versions. At the same time, these maps are also associated with a significant limitation, in that no robust single detector or detector set maps are available. As described in {{PlanckPapers|planck2016-l03}}, such maps do not contain the full signal content of the true sky. As a result, only full frequency maps are distributed and used in the 2018 analysis. |
| | | | |
| | For polarization analysis, this is not a significant issue, and the 2018 polarization foreground products therefore supersede the 2015 release in all respects. However, for temperature analysis the lack of single-detector maps strongly limits the ability to extract CO line emission from the data set, and it is also not possible to exclude known detector outliers; see {{PlanckPapers|planck2014-a12}} for details. For these reasons, we consider the parametric foreground products from 2015 to represent a more accurate description of the true sky than the corresponding 2018 version. '''As a result, we do not release parametric temperature foreground products from the 2018 data set, but rather recommend continued usage of the 2015 temperature model. For polarization, we recommend usage of the 2018 model.''' | | For polarization analysis, this is not a significant issue, and the 2018 polarization foreground products therefore supersede the 2015 release in all respects. However, for temperature analysis the lack of single-detector maps strongly limits the ability to extract CO line emission from the data set, and it is also not possible to exclude known detector outliers; see {{PlanckPapers|planck2014-a12}} for details. For these reasons, we consider the parametric foreground products from 2015 to represent a more accurate description of the true sky than the corresponding 2018 version. '''As a result, we do not release parametric temperature foreground products from the 2018 data set, but rather recommend continued usage of the 2015 temperature model. For polarization, we recommend usage of the 2018 model.''' |
| | | | |
| − | ===Low-resolution temperature products===
| |
| | | | |
| − | : The Planck 2015 astrophysical component separation analysis in temperature combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors.
| + | Two Commander-based polarization foreground products are provided for the Planck 2018 releaes, namely synchrotron and thermal dust emission. For synchrotron emission, a spatially constant spectral index of β=-3.1 is adopted. For thermal dust emission, the dust temperature is fixed to that derived from the corresponding 2018 intensity analysis, while the spectral index is fitted directly from the polarization measurements, smoothed to 3 degrees FWHM. For both synchrotron and thermal dust emission, we provide results derived from both the full-mission data set, and from the half-mission and odd-even splits. |
| − | | |
| − | ====Inputs====
| |
| − | | |
| − | The following data products are used for the low-resolution analysis:
| |
| − | * Full-mission 30 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=30|period=Full|link=LFI 30 GHz frequency maps}}
| |
| − | * Full-mission 44 GHz frequency map, {{PLAFreqMaps|inst=LFI|freq=44|period=Full|link=LFI 44 GHz frequency maps}}
| |
| − | * Full-mission 70 GHz ds1 (18+23), ds2 (19+22), and ds3 (20+21) detector-set maps
| |
| − | * Full-mission 100 GHz ds1 and ds2 detector set maps
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| − | * Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
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| − | * Full-mission 217 GHz detector 1, 2, 3 and 4 maps
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| − | * Full-mission 353 GHz detector set ds2 and detector 1 maps
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| − | * Full-mission 545 GHz detector 2 and 4 maps
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| − | * Full-mission 857 GHz detector 2 map
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| − | * Beam-symmetrized 9-year WMAP K-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
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| − | * Beam-symmetrized 9-year WMAP Ka-band map [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
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| − | * Default 9-year WMAP Q1 and Q2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
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| − | * Default 9-year WMAP V1 and V2 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
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| − | * Default 9-year WMAP W1, W2, W3, and W4 differencing assembly maps [http://lambda.gsfc.nasa.gov/product/map/dr5/skymap_info.cfm (Lambda)]
| |
| − | * Re-processed 408 MHz survey map, Remazeilles et al. (2014) [http://lambda.gsfc.nasa.gov/product/foreground/2014_haslam_408_info.cfm (Lambda)]
| |
| − | All maps are smoothed to a common resolution of 1 degree FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256.
| |
| − | | |
| − | ====Outputs====
| |
| − | | |
| − | =====Synchrotron emission=====
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| − | | |
| − | <!--<center>
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| − | <gallery style="padding:0 0 0 0;" perrow=3 widths=800px heights=500px>
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| − | File:commander_synch_amp.png | '''Commander low-resolution synchrotron amplitude'''
| |
| − | </gallery>
| |
| − | </center>-->
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Synchrotron-commander_0256_R2.00.fits|link=COM_CompMap_Synchrotron-commander_0256_R2.00.fits}}
| |
| − | : Reference frequency: 408 MHz
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| − | : Nside = 256
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| − | : Angular resolution = 60 arcmin
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| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ HDU -- COMP-MAP-Synchrotron
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML || Real*4 || uK_RJ || Amplitude posterior maximum
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| − | |-
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| − | |I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean
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| − | |-
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| − | |I_RMS || Real*4 || uK_RJ || Amplitude posterior rms
| |
| − | |}
| |
| − | | |
| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ Extension 1 -- SYNC-TEMP
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |nu || Real*4 || Hz || Frequency
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| − | |-
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| − | |intensity || Real*4 || W/Hz/m2/sr || GALPROP z10LMPD_SUNfE spectrum
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| − | |}
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| − | | |
| − | =====Free-free emission=====
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}}
| |
| − | : Reference frequency: NA
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| − | : Nside = 256
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| − | : Angular resolution = 60 arcmin
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| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ HDU -- COMP-MAP-freefree
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |EM_ML || Real*4 || cm^-6 pc || Emission measure posterior maximum
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| − | |-
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| − | |EM_MEAN || Real*4 || cm^-6 pc || Emission measure posterior mean
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| − | |-
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| − | |EM_RMS || Real*4 || cm^-6 pc || Emission measure posterior rms
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| − | |-
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| − | |TEMP_ML || Real*4 || K || Electron temperature posterior maximum
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| − | |-
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| − | |TEMP_MEAN || Real*4 || K || Electron temperature posterior mean
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| − | |-
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| − | |TEMP_RMS || Real*4 || K || Electron temperature posterior rms
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| − | |}
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| − | | |
| − | | |
| − | =====Spinning dust emission=====
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}}
| |
| − | : Nside = 256
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| − | : Angular resolution = 60 arcmin
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| − | | |
| − | Note: The spinning dust component has two independent constituents, each corresponding to one spdust2 component, but with different peak frequencies. The two components are stored in the two first FITS extensions, and the template frequency spectrum is stored in the third extension.
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| − | | |
| − | : Reference frequency: 22.8 GHz
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| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ HDU -- COMP-MAP-AME1
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML || Real*4 || uK_RJ || Primary amplitude posterior maximum
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| − | |-
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| − | |I_MEAN || Real*4 || uK_RJ || Primary amplitude posterior mean
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| − | |-
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| − | |I_RMS || Real*4 || uK_RJ || Primary amplitude posterior rms
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| − | |-
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| − | |FREQ_ML || Real*4 || GHz || Primary peak frequency posterior maximum
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| − | |-
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| − | |FREQ_MEAN || Real*4 || GHz || Primary peak frequency posterior mean
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| − | |-
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| − | |FREQ_RMS || Real*4 || GHz || Primary peak frequency posterior rms
| |
| − | |}
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| − | | |
| − | : Reference frequency: 41.0 GHz
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| − | : Peak frequency: 33.35 GHz
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| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ Extension 1 -- COMP-MAP-AME2
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML || Real*4 || uK_RJ || Secondary amplitude posterior maximum
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| − | |-
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| − | |I_MEAN || Real*4 || uK_RJ || Secondary amplitude posterior mean
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| − | |-
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| − | |I_RMS || Real*4 || uK_RJ || Secondary amplitude posterior rms
| |
| − | |}
| |
| − | | |
| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ Extension 2 -- SPINNING-DUST-TEMP
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |nu || Real*4 || GHz || Frequency
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| − | |-
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| − | |j_nu/nH || Real*4 || Jy sr-1 cm2/H || spdust2 spectrum
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| − | |}
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| − | | |
| − | =====CO line emission=====
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}}
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| − | : Nside = 256
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| − | : Angular resolution = 60 arcmin
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| − | | |
| − | Note: The CO line emission component has three independent objects, corresponding to the J1->0, 2->1 and 3->2 lines, stored in separate extensions.
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| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ HDU -- COMP-MAP-co10
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior maximum
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| − | |-
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| − | |I_MEAN || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior mean
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| − | |-
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| − | |I_RMS || Real*4 || K_RJ km/s || CO(1-0) amplitude posterior rms
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| − | |}
| |
| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ Extension 1 -- COMP-MAP-co21
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior maximum
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| − | |-
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| − | |I_MEAN || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior mean
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| − | |-
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| − | |I_RMS || Real*4 || K_RJ km/s || CO(2-1) amplitude posterior rms
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| − | |}
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| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ Extension 2 -- COMP-MAP-co32
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior maximum
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| − | |-
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| − | |I_MEAN || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior mean
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| − | |-
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| − | |I_RMS || Real*4 || K_RJ km/s || CO(3-2) amplitude posterior rms
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| − | |}
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| − | | |
| − | =====94/100 GHz line emission=====
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-commander_0256_R2.00.fits}}
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| − | : Nside = 256
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| − | : Angular resolution = 60 arcmin
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| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ HDU -- COMP-MAP-xline
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML || Real*4 || uK_cmb || Amplitude posterior maximum
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| − | |-
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| − | |I_MEAN || Real*4 || uK_cmb || Amplitude posterior mean
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| − | |-
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| − | |I_RMS || Real*4 || uK_cmb || Amplitude posterior rms
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| − | |}
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| − | | |
| − | Note: The amplitude of this component is normalized according to the 100-ds1 detector set map, ie., it is the amplitude as measured by this detector combination.
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| − | | |
| − | =====Thermal dust emission=====
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}}
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| − | : Nside = 256
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| − | : Angular resolution = 60 arcmin
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| − | | |
| − | : Reference frequency: 545 GHz
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| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ HDU -- COMP-MAP-dust
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML || Real*4 || uK_RJ || Amplitude posterior maximum
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| − | |-
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| − | |I_MEAN || Real*4 || uK_RJ || Amplitude posterior mean
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| − | |-
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| − | |I_RMS || Real*4 || uK_RJ || Amplitude posterior rms
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| − | |-
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| − | |TEMP_ML || Real*4 || K || Dust temperature posterior maximum
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| − | |-
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| − | |TEMP_MEAN || Real*4 || K || Dust temperature posterior mean
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| − | |-
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| − | |TEMP_RMS || Real*4 || K || Dust temperature posterior rms
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| − | |-
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| − | |BETA_ML || Real*4 || NA || Emissivity index posterior maximum
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| − | |-
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| − | |BETA_MEAN || Real*4 || NA || Emissivity index posterior mean
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| − | |-
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| − | |BETA_RMS || Real*4 || NA || Emissivity index posterior rms
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| − | |}
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| − | | |
| − | =====Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters=====
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SZ-commander_0256_R2.00.fits|link=COM_CompMap_SZ-commander_0256_R2.00.fits}}
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| − | : Nside = 256
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| − | : Angular resolution = 60 arcmin
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| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
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| − | |+ HDU -- COMP-MAP-SZ
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| − | |-
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| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |Y_ML || Real*4 || y_SZ || Y parameter posterior maximum
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| − | |-
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| − | |Y_MEAN || Real*4 || y_SZ || Y parameter posterior mean
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| − | |-
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| − | |Y_RMS || Real*4 || y_SZ || Y parameter posterior rms
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| − | |}
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| − | | |
| − | ===High-resolution temperature products===
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| − | | |
| − | High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz.
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| − | | |
| − | ====Inputs====
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| − | | |
| − | The following data products are used for the low-resolution analysis:
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| − | * Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
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| − | * Full-mission 217 GHz detector 1, 2, 3 and 4 maps
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| − | * Full-mission 353 GHz detector set ds2 and detector 1 maps
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| − | * Full-mission 545 GHz detector 2 and 4 maps
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| − | * Full-mission 857 GHz detector 2 map
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| − | All maps are smoothed to a common resolution of 7.5 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=2048.
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| − | | |
| − | ====Outputs====
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| − | | |
| − | =====CO J2->1 emission=====
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO21-commander_2048_R2.00.fits|link=COM_CompMap_CO21-commander_2048_R2.00.fits}}
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| − | : Nside = 2048
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| − | : Angular resolution = 7.5 arcmin
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| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ HDU -- COMP-MAP-CO21
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| − | |-
| |
| − | |- bgcolor="ffdead"
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| − | ! Column Name || Data Type || Units || Description
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| − | |-
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| − | |I_ML_FULL || Real*4 || K_RJ km/s || Full-mission amplitude posterior maximum
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| − | |-
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| − | |I_ML_HM1 || Real*4 || K_RJ km/s || First half-mission amplitude posterior maximum
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| − | |-
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| − | |I_ML_HM2 || Real*4 || K_RJ km/s || Second half-mission amplitude posterior maximum
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| − | |-
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| − | |I_ML_HR1 || Real*4 || K_RJ km/s || First half-ring amplitude posterior maximum
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| − | |-
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| − | |I_ML_HR2 || Real*4 || K_RJ km/s || Second half-ring amplitude posterior maximum
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| − | |-
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| − | |I_ML_YR1 || Real*4 || K_RJ km/s || "First year" amplitude posterior maximum
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| − | |-
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| − | |I_ML_YR2 || Real*4 || K_RJ km/s || "Second year" amplitude posterior maximum
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| − | |}
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| − | | |
| − | | |
| − | =====Thermal dust emission=====
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| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_ThermalDust-commander_2048_R2.00.fits|link=COM_CompMap_ThermalDust-commander_2048_R2.00.fits}}
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| − | : Nside = 2048
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| − | : Angular resolution = 7.5 arcmin
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| − | | |
| − | : Reference frequency: 545 GHz
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| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ HDU -- COMP-MAP-dust
| |
| − | |-
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Column Name || Data Type || Units || Description
| |
| − | |-
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| − | |I_ML_FULL || Real*4 || uK_RJ || Full-mission amplitude posterior maximum
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| − | |-
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| − | |I_ML_HM1 || Real*4 || uK_RJ || First half-mission amplitude posterior maximum
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| − | |-
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| − | |I_ML_HM2 || Real*4 || uK_RJ || Second half-mission amplitude posterior maximum
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| − | |-
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| − | |I_ML_HR1 || Real*4 || uK_RJ || First half-ring amplitude posterior maximum
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| − | |-
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| − | |I_ML_HR2 || Real*4 || uK_RJ || Second half-ring amplitude posterior maximum
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| − | |-
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| − | |I_ML_YR1 || Real*4 || uK_RJ || "First year" amplitude posterior maximum
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| − | |-
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| − | |I_ML_YR2 || Real*4 || uK_RJ || "Second year" amplitude posterior maximum
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| − | |-
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| − | |BETA_ML_FULL || Real*4 || NA || Full-mission emissivity index posterior maximum
| |
| − | |-
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| − | |BETA_ML_HM1 || Real*4 || NA || First half-mission emissivity index posterior maximum
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| − | |-
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| − | |BETA_ML_HM2 || Real*4 || NA || Second half-mission emissivity index posterior maximum
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| − | |-
| |
| − | |BETA_ML_HR1 || Real*4 || NA || First half-ring emissivity index posterior maximum
| |
| − | |-
| |
| − | |BETA_ML_HR2 || Real*4 || NA || Second half-ring emissivity index posterior maximum
| |
| − | |-
| |
| − | |BETA_ML_YR1 || Real*4 || NA || "First year" emissivity index posterior maximum
| |
| − | |-
| |
| − | |BETA_ML_YR2 || Real*4 || NA || "Second year" emissivity index posterior maximum
| |
| − | |-
| |
| − | |}
| |
| − | | |
| − | ===2018 polarization products===
| |
| − | | |
| − | Two Commander-based polarization foreground products are provided, namely synchrotron and thermal dust emission. For synchrotron emission, a spatially constant spectral index of %beta=-3.1 is adopted. For thermal dust emission, the dust temperature is fixed to that derived from the corresponding 2018 intensity analysis, while the spectral index is fitted directly from the polarization measurements, smoothed to 3 degrees FWHM. For both synchrotron and thermal dust emission, we provide results derived from both the full-mission data set, and from the half-mission and odd-even splits. | |
| | | | |
| | In addition to the real observations, we also provide 300 end-to-end noise simulations processed through the algorithm with the same spectral parameters as derived from the data for each of the data splits. The filenames of these simulations have the following format: | | In addition to the real observations, we also provide 300 end-to-end noise simulations processed through the algorithm with the same spectral parameters as derived from the data for each of the data splits. The filenames of these simulations have the following format: |
| Line 405: |
Line 52: |
| | =====Thermal dust emission===== | | =====Thermal dust emission===== |
| | | | |
| − | : Full-mission file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_full.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_full.fits}} | + | : Full-mission file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_full.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_full.fits}} |
| − | : First half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm1.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_hm1.fits}} | + | : First half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm1.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm1.fits}} |
| − | : Second half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm2.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_hm2.fits}} | + | : Second half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm2.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_hm2.fits}} |
| − | : Odd ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe1.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_oe1.fits}} | + | : Odd ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe1.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe1.fits}} |
| − | : Even ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe2.fits|link=COM_CompMap_QU_synchrotron-commander_2048_R3.00_oe2.fits}} | + | : Even ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe2.fits|link=COM_CompMap_QU_thermaldust-commander_2048_R3.00_oe2.fits}} |
| | : Nside = 2048 | | : Nside = 2048 |
| | : Angular resolution = 5 arcmin | | : Angular resolution = 5 arcmin |
| Line 422: |
Line 69: |
| | |Q_STOKES || Real*4 || uK_RJ || Full-mission Stokes Q posterior maximum | | |Q_STOKES || Real*4 || uK_RJ || Full-mission Stokes Q posterior maximum |
| | |- | | |- |
| − | |U_STOKES || Real*4 || uK_RJ || Full-mission Stokes U posterior maximum | + | |U_STOKES || Real*4 || uK_RJ || Full-mission Stokes U posterior maximum |
| | + | |- |
| | + | |BETA || Real*4 || || Spectral index (full mission only) |
| | |} | | |} |
| | | | |
| − | == Astrophysical foregrounds from the Planck 2018 observations with SMICA == | + | == SMICA-derived astrophysical foreground maps == |
| | | | |
| − | Two SMICA-based polarization foreground products are provided, namely synchrotron and thermal dust emission. These are derived using the usual SMICA spectral matching algorithm, but tuned specifically for foreground reconstruction. Specifically, three assumptions are imposed on the solution: 1) CMB is neglected from the analysis; 2) synchrotron emission is assumed negligible at 353 GHz; and 3) thermal dust emission is assumed negligible at 30 GHz. Otherwise, no additional constraints are imposed on either the angular power spectrum or the spectral energy density of the two components. For both synchrotron and thermal dust emission, we provide results derived from both the full-mission data set, and from the half-mission and odd-even splits. | + | Two SMICA-based polarization foreground products are provided, namely synchrotron and thermal dust emission. These are derived using the usual SMICA spectral matching method, tuned specifically for the reconstruction of two polarized foregrounds. Specifically, three coherent components (plus noise) are fitted at the spectral level with the first one constrained to have CMB emissivity. No assumptions are made regarding the other two components: they are not assumed to have a specific emissivity or angular spectrum, nor are they assumed to be uncorrelated. This leaves a degenerate model but that degeneracy can be entirely fixed after the spectral fit by assuming that synchrotron emission is negligible at 353 GHz and that thermal dust emission is negligible at 30 GHz. For both synchrotron and thermal dust emission, we provide results derived from both the full-mission data set, and from the half-mission and odd-even splits. |
| | | | |
| | In addition to the real observations, we also provide 300 end-to-end noise simulations processed through the algorithm with the same spectral parameters as derived from the data for each of the data splits. The filenames of these simulations have the following format: | | In addition to the real observations, we also provide 300 end-to-end noise simulations processed through the algorithm with the same spectral parameters as derived from the data for each of the data splits. The filenames of these simulations have the following format: |
| Line 467: |
Line 116: |
| | =====Thermal dust emission===== | | =====Thermal dust emission===== |
| | | | |
| − | : Full-mission file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_full.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_full.fits}} | + | : Full-mission file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_full.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_full.fits}} |
| − | : First half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm1.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_hm1.fits}} | + | : First half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm1.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm1.fits}} |
| − | : Second half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm2.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_hm2.fits}} | + | : Second half-mission split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm2.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_hm2.fits}} |
| − | : Odd ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe1.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_oe1.fits}} | + | : Odd ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe1.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe1.fits}} |
| − | : Even ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe2.fits|link=COM_CompMap_QU_synchrotron-smica_2048_R3.00_oe2.fits}} | + | : Even ring split file name: {{PLASingleFile|fileType=map|name=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe2.fits|link=COM_CompMap_QU_thermaldust-smica_2048_R3.00_oe2.fits}} |
| | : Nside = 2048 | | : Nside = 2048 |
| | : Angular resolution = 12 arcmin | | : Angular resolution = 12 arcmin |
| Line 487: |
Line 136: |
| | |} | | |} |
| | | | |
| − | == CO emission maps == | + | ==GNILC thermal dust maps== |
| − | | |
| − | CO 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 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. A full description of how these products were generated is given in {{PlanckPapers|planck2013-p03a}} and {{PlanckPapers|planck2014-a12}}.
| |
| − | | |
| − | * 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. The improvement relative to the 2013 release comes from the combined effect of the ADC correction, the VLTC correction, and the improved calibration scheme. As a result, the noise level is ~30% lower in the new products, and the maps are much better behaved at high latitudes.
| |
| − | | |
| − | * 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.
| |
| − | * Type 3 product: to generate this product, fixed CO line ratios are assumed and a high-resolution parametric foreground model is fit. In 2013 this product was generated using the Commander-Ruler technique. In 2015, this technique is superseded by the high-resolution Commander-only, used to produce the J=2-1 map presented in [https://wiki.cosmos.esa.int/planckpla2015/index.php/CMB_and_astrophysical_component_maps#CO_J2-.3E1_emission] and described in Section 5.4 of {{PlanckPapers|planck2014-a12}}.
| |
| − | | |
| − | Type 1 and 2 maps have been produced using the MILCA algorithm. Commander has been used to produce low resolution CO J=1-0,2-1,3-2 maps ([[CMB_and_astrophysical_component_maps#CO_line_emission|here]]) and high resolution CO J=2-1 maps ([[CMB_and_astrophysical_component_maps#CO_J2-.3E1_emission|here]]).
| |
| − | | |
| − | A summary of all the 2015 CO maps can be found in Table 9 from {{PlanckPapers|planck2014-a12}}, also shown here:
| |
| − | | |
| − | [[File:Planck_2015_A10_Fig9_CO_maps.png]]
| |
| − | | |
| − | | |
| − | 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 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:
| |
| − | * The signal map
| |
| − | * The standard deviation map (same unit as the signal),
| |
| − | * 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.
| |
| − | * A mask map (0 or 1) giving the regions (1) where the CO measurement is not reliable because of some severe identified foreground contamination.
| |
| − | | |
| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=HFI_CompMap_CO-Type1_2048_R2.00.fits|link=HFI_CompMap_CO-Type1_2048_R2.00.fits}}
| |
| − | : Nside = 2048
| |
| − | | |
| − | | |
| − | | |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
| |
| − | |+ '''Type-1 CO map file data structure'''
| |
| − | |- bgcolor="ffdead"
| |
| − | !colspan="4" | 1. EXTNAME = 'COMP-MAP'
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Column Name || Data Type || Units || Description
| |
| − | |-
| |
| − | |INTEN10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map
| |
| − | |-
| |
| − | |ERR10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity
| |
| − | |-
| |
| − | |NULL10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
| |
| − | |-
| |
| − | |MASK10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable
| |
| − | |-
| |
| − | |INTEN21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map
| |
| − | |-
| |
| − | |ERR21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity
| |
| − | |-
| |
| − | |NULL21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
| |
| − | |-
| |
| − | |MASK21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable
| |
| − | |-
| |
| − | |INTEN32 || Real*4 || K_RJ km/sec || The CO(3-2) intensity map
| |
| − | |-
| |
| − | |ERR32 || Real*4 || K_RJ km/sec || Uncertainty in the CO(3-2) intensity
| |
| − | |-
| |
| − | |NULL32 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
| |
| − | |-
| |
| − | |MASK32 || Byte || none || Region over which the CO(3-2) intensity is considered reliable
| |
| − | |-
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Keyword || Data Type || Value || Description
| |
| − | |-
| |
| − | |AST-COMP || string || CO-TYPE1 || Astrophysical compoment name
| |
| − | |-
| |
| − | |PIXTYPE || String || HEALPIX ||
| |
| − | |-
| |
| − | |COORDSYS || String || GALACTIC ||Coordinate system
| |
| − | |-
| |
| − | |ORDERING || String || NESTED || Healpix ordering
| |
| − | |-
| |
| − | |NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively
| |
| − | |-
| |
| − | |FIRSTPIX || Int*4 || 0 || First pixel number
| |
| − | |-
| |
| − | |LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively
| |
| − | |-
| |
| − | |CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s))
| |
| − | |-
| |
| − | |CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s))
| |
| − | |-
| |
| − | |CNV 3-2 || Real*4 || value || Factor to convert CO(3-2) intensityto Kcmb (units Kcmb/(Krj*km/s))
| |
| − | |}
| |
| − | | |
| − | | |
| − | | |
| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=HFI_CompMap_CO-Type2_2048_R2.00.fits|link=HFI_CompMap_CO-Type2_2048_R2.00.fits}}
| |
| − | : Nside = 2048
| |
| − | | |
| − | | |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
| |
| − | |+ '''Type-2 CO map file data structure'''
| |
| − | |- bgcolor="ffdead"
| |
| − | !colspan="4" | 1. EXTNAME = 'COMP-MAP'
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Column Name || Data Type || Units || Description
| |
| − | |-
| |
| − | |I10 || Real*4 || K_RJ km/sec || The CO(1-0) intensity map
| |
| − | |-
| |
| − | |E10 || Real*4 || K_RJ km/sec || Uncertainty in the CO(1-0) intensity
| |
| − | |-
| |
| − | |N10 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
| |
| − | |-
| |
| − | |M10 || Byte || none || Region over which the CO(1-0) intensity is considered reliable
| |
| − | |-
| |
| − | |-
| |
| − | |I21 || Real*4 || K_RJ km/sec || The CO(2-1) intensity map
| |
| − | |-
| |
| − | |E21 || Real*4 || K_RJ km/sec || Uncertainty in the CO(2-1) intensity
| |
| − | |-
| |
| − | |N21 || Real*4 || K_RJ km/sec || Map built from the half-ring difference maps
| |
| − | |-
| |
| − | |M21 || Byte || none || Region over which the CO(2-1) intensity is considered reliable
| |
| − | |-
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Keyword || Data Type || Value || Description
| |
| − | |-
| |
| − | |AST-COMP || String || CO-TYPE2 || Astrophysical compoment name
| |
| − | |-
| |
| − | |PIXTYPE || String || HEALPIX ||
| |
| − | |-
| |
| − | |COORDSYS || String || GALACTIC ||Coordinate system
| |
| − | |-
| |
| − | |ORDERING || String || NESTED || Healpix ordering
| |
| − | |-
| |
| − | |NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively
| |
| − | |-
| |
| − | |FIRSTPIX || Int*4 || 0 || First pixel number
| |
| − | |-
| |
| − | |LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively
| |
| − | |-
| |
| − | |CNV 1-0 || Real*4 || value || Factor to convert CO(1-0) intensity to Kcmb (units Kcmb/(Krj*km/s))
| |
| − | |-
| |
| − | |CNV 2-1 || Real*4 || value || Factor to convert CO(2-1) intensityto Kcmb (units Kcmb/(Krj*km/s))
| |
| − | |}
| |
| − | | |
| − | | |
| − | == Modelling of the thermal dust emission with the Draine and Li dust model ==
| |
| − | | |
| − | The Planck, IRAS, and WISE infrared observations were fit with the dust model presented by Draine & Li in 2007 (DL07).
| |
| − | The input maps, the DL07 model, and the fitting procedure and results are presented in {{PlanckPapers|planck2014-XXIX}}.
| |
| − | Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.
| |
| − | | |
| − | ===Inputs===
| |
| − | | |
| − | The following data have been fit:
| |
| − | | |
| − | * WISE 12 micron map
| |
| − | * IRAS 60 micron map
| |
| − | * IRAS 100 micron map
| |
| − | * Full-mission 353 GHz PR2 map
| |
| − | * Full-mission 545 GHz PR2 map
| |
| − | * Full-mission 857 GHz PR2 map
| |
| − | | |
| − | The CIB monopole, the CMB anisotropries and the zodiacal light were subtracted to obtain dust emission maps from the sky emission maps.
| |
| − | All maps were smoothed to a common angular resolution of 5'.
| |
| − | | |
| − | ===Model Parameters===
| |
| − | | |
| − | For each pixel of the inputs maps, we have fitted four parameters of the DL07 model:
| |
| − | | |
| − | * the dust mass surface density, Sigma_Mdust,
| |
| − | * the dust mass fraction in small PAH grains, q_PAH,
| |
| − | * the fraction of the total luminosity from dust heated by intense radiation fields, f_PDR,
| |
| − | * the starlight intensity heating the bulk of the dust, U_min.
| |
| − | | |
| − | The parameter maps and their uncertainties are gathered in one file. This file also includes the
| |
| − | chi2 of the fit per degree of freedom.
| |
| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits}}
| |
| − | : Nside = 2048
| |
| − | : Angular resolution = 5 arcmin
| |
| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ HDU -- COMP-MAP-Dust-DL07-Parameters
| |
| − | |-
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Column Name || Data Type || Units || Description
| |
| − | |-
| |
| − | |Sigma_Mdust || Real*4 || Solar masses/kpc^2 || Dust mass surface density
| |
| − | |-
| |
| − | |Sigma_Mdust_unc || Real*4 || Solar masses/kpc^2 || Uncertainty (1 sigma) on Sigma_Mdust
| |
| − | |-
| |
| − | |q_PAH || Real*4 || dimensionless || Dust mass fraction in small PAH grains
| |
| − | |-
| |
| − | |q_PAH_unc || Real*4 || dimensionless || Uncertainty (1 sigma) on q_PAH
| |
| − | |-
| |
| − | |f_PDR || Real*4 || dimensionless || Fraction of the total luminosity from dust heated by intense radiation fields
| |
| − | |-
| |
| − | |f_PDR_unc || Real*4 || dimensionless || Uncertainty (1 sigma) on f_PDR
| |
| − | |-
| |
| − | |U_min || Real*4 || dimensionless || Starlight intensity heating the bulk of the dust
| |
| − | |-
| |
| − | |U_min_unc || Real*4 || dimensionless || Uncertainty (1 sigma) on U_min
| |
| − | |-
| |
| − | |Chi2_DOF || Real*4 || dimensionless || Chi2 of the fit per degree of freedom
| |
| − | |}
| |
| − | | |
| − | ===Visible extinction maps===
| |
| − | | |
| − | We provide two exinctions maps at the visible V band: the value from the model (Av_DL) and the
| |
| − | renormalized one (Av_RQ) that matches extinction estimates for quasars (QSOs) derived from the Sloan digital sky survey (SDSS) data.
| |
| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits}}
| |
| − | : Nside = 2048
| |
| − | : Angular resolution = 5 arcmin
| |
| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ HDU -- COMP-MAP-Dust-DL07-AvMaps
| |
| − | |-
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Column Name || Data Type || Units || Description
| |
| − | |-
| |
| − | |Av_DL || Real*4 || magnitude || Extinction in the V band from the DL model
| |
| − | |-
| |
| − | |Av_DL_unc || Real*4 || magnitude || Uncertainty (1 sigma) on Av_DL
| |
| − | |-
| |
| − | |Av_RQ || Real*4 || magnitude || Extinction in the V band renormalized to match estimates from QSO SDSS observations
| |
| − | |-
| |
| − | |Av_RQ_unc || Real*4 || magnitude || Uncertainty (1 sigma) on Av_RQ
| |
| − | |}
| |
| − | | |
| − | ===Model Fluxes===
| |
| − | | |
| − | We provide the model predicted fluxes in the following file.
| |
| − | | |
| − | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits|link=COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits}}
| |
| − | : Nside = 2048
| |
| − | : Angular resolution = 5 arcmin
| |
| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ HDU -- COMP-MAP-Dust-DL07-ModelFluxes
| |
| − | |-
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Column Name || Data Type || Units || Description
| |
| − | |-
| |
| − | |Planck_857 || Real*4 || MJy/sr || Model flux in the Planck 857 GHz band
| |
| − | |-
| |
| − | |Planck_545 || Real*4 || MJy/sr || Model flux in the Planck 545 GHz band
| |
| − | |-
| |
| − | |Planck_353 || Real*4 || MJy/sr || Model flux in the Planck 353 GHz band
| |
| − | |-
| |
| − | |WISE_12 || Real*4 || MJy/sr || Model flux in the WISE 12 micron band
| |
| − | |-
| |
| − | |IRAS_60 || Real*4 || MJy/sr || Model flux in the IRAS 60 micron band
| |
| − | |-
| |
| − | |IRAS_100 || Real*4 || MJy/sr || Model flux in the IRAS 100 micron band
| |
| − | |}
| |
| − | | |
| − | | |
| − | | |
| − | == Thermal dust and CIB all-sky maps from GNILC component separation ==
| |
| − | We describe diffuse foreground products for the Planck 2015 and 2018 releases produced with the GNILC component separation method. See the Planck paper {{PlanckPapers|planck2016-XLVIII}} and {{PlanckPapers|planck2016-l04}} for a detailed discussion on these products.
| |
| − | | |
| − | ===Method===
| |
| − | | |
| − | : The basic idea behind the Generalized Needlet Internal Linear Combination (GNILC) component-separation method ([http://adsabs.harvard.edu/abs/2011MNRAS.418..467R Remazeilles et al, MNRAS 2011]) is to disentangle specific components of emission not on the sole basis of the spectral (frequency) information but also on the basis of their distinct spatial information (angular power spectrum). The GNILC method has been applied to Planck data in order to disentangle Galactic dust emission and Cosmic Infrared Background (CIB) anisotropies. Both components have a similar spectral signature but a distinct angular power spectrum (spatial signature). The spatial information used by GNILC is under the form of priors for the angular power spectra of the CIB, the CMB, and the instrumental noise. No assumption is made on the Galactic signal, neither spectral or spatial. In that sense, GNILC is a blind component-separation method. GNILC operates on a needlet (spherical wavelet) frame, therefore adapting the component separation to the local conditions of contamination both over the sky and over the angular scales.
| |
| − | | |
| − | : Intensity products are provided both from the 2015 and 2018 data releases, while polarization products are only provided from the 2018 data set. For analyses that only involve intensity alone, we recommend usage of the 2015 GNILC products, as these are considered more robust than the corresponding 2018 products. However, for analyses that require intensity products in order to characterize polarization measurements (such as estimation of polarization fraction), we recommend usage of the 2018 GNILC intensity products, in order to ensure that effective bandpasses are identical within a given analysis.
| |
| − | | |
| − | ===Data===
| |
| − | | |
| − | : The data used by GNILC for the analysis are the Planck data release 2 (PR2) and release 3 (PR3) frequency maps from 30 to 857 GHz, and a 100 micron hybrid map combined from the SFD map ([http://adsabs.harvard.edu/abs/1998ApJ...500..525S Schlegel et al, ApJ 1998]) at large angular scales (> 30') and the IRIS map ([http://adsabs.harvard.edu/abs/2005ApJS..157..302M Miville-Deschênes et al, ApJS 2005]) at small angular scales (< 30'). This special 100 micron map can be obtained in the External Maps section of the PLA.
| |
| − | | |
| − | ===Pre-processing===
| |
| − | | |
| − | : The point-sources with a signal-to-noise ratio, S/N > 5, in each individual frequency map (30 to 857 GHz, and 100 micron) have been pre-processed by a minimum curvature surface inpainting technique ([http://adsabs.harvard.edu/abs/2015MNRAS.451.4311R Remazeilles et al, MNRAS 2015]) prior to performing component separation with GNILC.
| |
| − | | |
| − | ===GNILC thermal dust and CIB products===
| |
| − | | |
| − | The result of GNILC component separation are thermal dust and CIB maps at 353, 545, and 857 GHz. In addition, by fitting a modified blackbody model to the GNILC thermal dust products at 353, 545, 857, and 100 micron, we have created all-sky maps of the dust optical depth, dust temperature, and dust emmissivity index. Note that the thermal dust maps have a variable angular resolution over the sky with an effective beam FWHM varying from 21.8' to 5'. The dust beam FWHM map is also released as a product.
| |
| − | | |
| − | ====2015 thermal dust maps====
| |
| − | | |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ HDU -- COMP-MAP-DUST
| |
| − | |-
| |
| − | |- bgcolor="ffdead"
| |
| − | ! File Name || Nside || Units || Reference frequency || Angular resolution || Description
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F353_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F353_2048_R2.00.fits}} || 2048 || MJy/sr || 353 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust amplitude at 353 GHz
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F545_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F545_2048_R2.00.fits}} || 2048 || MJy/sr || 545 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust amplitude at 545 GHz
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F857_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F857_2048_R2.00.fits}} || 2048 || MJy/sr || 857 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust amplitude at 857 GHz
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.00.fits}}|| 2048 || NA || 353 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust optical depth at 353 GHz
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.00.fits}} || 2048 || NA || NA || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust emissivity index
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.00.fits}} || 2048 || K || NA || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust temperature
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Radiance_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Radiance_2048_R2.00.fits}} || 2048 || W/m<sup>2</sup>/sr || NA || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust radiance
| |
| − | |-
| |
| − | |[http://pla.esac.esa.int/pla/aio/product-action?DOCUMENT_MAP.DOCUMENT_ID=COM_DocMap_Dust-GNILC-Beam-FWHM_R2.00.fits COM_DocMap_Dust-GNILC-Beam-FWHM_R2.00.fits] || 128 || Arcminute || NA || NA || Effective dust beam FWHM
| |
| − | |}
| |
| − | | |
| − | ====2018 thermal dust maps====
| |
| | | | |
| | The 2018 GNILC thermal dust products are provided as single files that include both intensity and polarization, 3x3 IQU noise covariance matrices per pixel, and as well as local smoothing scale for the variable resolution map. The structure of the data files is the following: | | The 2018 GNILC thermal dust products are provided as single files that include both intensity and polarization, 3x3 IQU noise covariance matrices per pixel, and as well as local smoothing scale for the variable resolution map. The structure of the data files is the following: |
| Line 821: |
Line 173: |
| | |- | | |- |
| | |} | | |} |
| − |
| |
| − |
| |
| − |
| |
| − | ====CIB maps====
| |
| − |
| |
| − |
| |
| − | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ HDU -- COMP-MAP-CIB
| |
| − | |-
| |
| − | |- bgcolor="ffdead"
| |
| − | ! File Name || Nside || Units || Reference frequency || Angular resolution || Description
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F353_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F353_2048_R2.00.fits}} || 2048 || MJy/sr || 353 GHz || 5 arcmin || CIB amplitude at 353 GHz
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F545_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F545_2048_R2.00.fits}} || 2048 || MJy/sr || 545 GHz || 5 arcmin || CIB amplitude at 545 GHz
| |
| − | |-
| |
| − | |{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F857_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F857_2048_R2.00.fits}} || 2048 || MJy/sr || 857 GHz || 5 arcmin || CIB amplitude at 857 GHz
| |
| − | |-
| |
| − | |}
| |
| − |
| |
| − | = Other maps that require special processing =
| |
| − |
| |
| − | == 2015 Lensing map ==
| |
| − |
| |
| − | We distribute the minimum-variance (MV) lensing potential estimate presented in {{PlanckPapers|planck2014-a17}} as part of the 2014 data release. This map represents an estimate of the CMB lensing potential on approximately 70% of the sky, and also forms the basis for the Planck 2014 lensing likelihood. It is produced using filtered temperature and polarization data from the SMICA DX11 CMB map; its construction is discussed in detail in {{PlanckPapers|planck2014-a11}}.
| |
| − |
| |
| − |
| |
| − | The estimate is contained in a single gzipped tarball named ''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R2.00.tgz|link=COM_CompMap_Lensing_2048_R2.00.tgz}}''. Its contents are described below. The convergence map "dat_klm.fits" that can be found in the tarball, has been categorized as COM_Lensing-Convergence-dat-klm_2048_R2.00.fits in the Lensing Products section of the archive.
| |
| − |
| |
| − |
| |
| − |
| |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
| |
| − | |+ ''' Contents of Lensing package '''
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Filename || Format || Description
| |
| − | |-
| |
| − | | dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm max}=2048</math> || Contains the estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math>.
| |
| − | |-
| |
| − | | mask.fits.gz || HEALPix FITS format map, with <math>N_{\rm side}=2048</math> || Contains the lens reconstruction analysis mask.
| |
| − | |-
| |
| − | | nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>N_L </math>, <math>C_L+N_L</math>) || The approximate noise <math>N_L</math> (and signal+noise, <math>C_L+N_L</math>) power spectrum of <math> \hat{\kappa}_{LM} </math>, for the fiducial cosmology used in {{PlanckPapers|planck2014-a15}}.
| |
| − | |}
| |
| − |
| |
| − | === Previous Releases: (2013) Lensing Maps ===
| |
| − |
| |
| − | <div class="toccolours mw-collapsible mw-collapsed" style="background-color: #EEE8AA;width:80%">
| |
| − | '''2013 Release of the lensing map'''
| |
| − | <div class="mw-collapsible-content">
| |
| − |
| |
| − | ''' Description '''
| |
| − |
| |
| − | Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of {{PlanckPapers|planck2013-p12}}. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.
| |
| − |
| |
| − | We distribute:
| |
| − |
| |
| − | ; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate <math>\hat{\phi}</math> with the lensing response function <math>R_L^{\phi\phi}</math>. This map has been band-limited between multipoles <math>10 \le L \le 2048</math>.
| |
| − | ; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. ''Note'': the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.
| |
| − | ; RLPP : This column contains the response function <math>R_L^{\phi\phi}</math>.
| |
| − | ; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, <math>N_L^{\phi\phi}</math>. The noise is highly coloured. There is a dependence of the noise power spectrum on the local noise level of the map, discussed in Appendix A of {{PlanckPapers|planck2013-p12}}. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.
| |
| − |
| |
| − | Also, the table below gives the lensing curl-mode power spectrum data used to produce Figure A2 of {{PlanckPapers|planck2013-p12}}:
| |
| − |
| |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center"
| |
| − | |+ ''''MV' curl reconstruction bandpowers from Fig A2 of {{PlanckPapers|planck2013-p12}} '''
| |
| − | |- bgcolor="ffdead"
| |
| − | ! <math>L</math><sub>min</sub> || <math>L</math><sub>max</sub> || <math>{\hat{C}_L}^{\psi\psi} (L(L+1))^2/(2\pi)</math> || <math> std({\hat{C}_L}^{\psi\psi}) (L(L+1))^2 /(2\pi)</math>
| |
| − | |-
| |
| − | | 2 || 7 || -13.6379 || 15.3409
| |
| − | |-
| |
| − | | 8 || 20 || 6.0184 || 4.8881
| |
| − | |-
| |
| − | | 21 || 39 || -1.0675 || 3.0940
| |
| − | |-
| |
| − | | 40 || 65 || 0.6135 || 1.8474
| |
| − | |-
| |
| − | | 66 || 100 || 1.5030 || 1.2696
| |
| − | |-
| |
| − | | 101 || 144 || 1.3760 || 0.9950
| |
| − | |-
| |
| − | | 145 || 198 || -1.2289 || 0.8286
| |
| − | |-
| |
| − | | 199 || 263 || 1.1910 || 0.7001
| |
| − | |-
| |
| − | | 264 || 338 || -0.6567 || 0.6197
| |
| − | |-
| |
| − | | 339 || 425 || -0.8201 || 0.5235
| |
| − | |-
| |
| − | | 426 || 525 || -0.7581 || 0.4850
| |
| − | |-
| |
| − | | 526 || 637 || -0.3201 || 0.5134
| |
| − | |-
| |
| − | | 638 || 762 || -0.1589 || 0.4073
| |
| − | |-
| |
| − | | 763 || 901 || -0.6451 || 0.4044
| |
| − | |-
| |
| − | | 902 || 1054 || 0.4910 || 0.3718
| |
| − | |-
| |
| − | | 1055 || 1221 || -0.2186 || 0.3702
| |
| − | |-
| |
| − | | 1222 || 1404 || -0.3295 || 0.4146
| |
| − | |-
| |
| − | | 1405 || 1602 || -0.3647 || 0.4703
| |
| − | |-
| |
| − | | 1603 || 1816 || -0.1060 || 0.5904
| |
| − | |-
| |
| − | | 1817 || 2020 || -0.7887 || 0.8507
| |
| − | |}
| |
| − |
| |
| − |
| |
| − | ''' Production process '''
| |
| − |
| |
| − | The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of {{PlanckPapers|planck2013-p12}}. The response function <math>R_L^{\phi\phi}</math> here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.
| |
| − |
| |
| − | '''Inputs'''
| |
| − |
| |
| − | This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.
| |
| − | The analysis mask is constructed from a combination of thresholding in the 857GHz map (to remove the regions which are most contaminated by Galactic dust) and the [[CMB_and_astrophysical_component_maps#CO_emission_maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is joined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs are given in {{PlanckPapers|planck2013-p12}}.
| |
| − |
| |
| − | '''File names and format'''
| |
| − |
| |
| − | A single file named
| |
| − | *''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R1.10.fits|link=COM_CompMap_Lensing_2048_R1.10.fits}}''
| |
| − | with two BINTABLE extensions containing the items described below.
| |
| − |
| |
| − | For illustration, we show in the figures below the maps of the Wiener-filtered CMB lensing potential in Galactic coordinates using orthographic projection. The reconstruction was bandpass filtered to <math>L \in [10, 2048]</math>. Note that the lensing reconstruction, while highly statistically significant, is still noise dominated for every individual mode, and is at best <math>S/N \simeq 0.7</math> around <math>L = 30</math>.
| |
| − |
| |
| − | <center>
| |
| − | <gallery perrow=3 widths=260px heights=170px>
| |
| − | File: analysis_lens_pub_map_orth_north_dat_p.png | Galactic north
| |
| − | File: analysis_lens_pub_map_orth_south_dat_p.png | Galactic south
| |
| − | </gallery></center>
| |
| − |
| |
| − |
| |
| − |
| |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
| |
| − | |+ '''FITS file structure'''
| |
| − | |- bgcolor="ffdead"
| |
| − | !colspan="4" | 1. EXTNAME = ''LENS-MAP''
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Column Name || Data Type || Units || Description
| |
| − | |-
| |
| − | |PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP
| |
| − | |-
| |
| − | |MASK || Int || none || Region over which the lensing potential is reconstructed
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Keyword || Data Type || Value || Description
| |
| − | |-
| |
| − | |PIXTYPE || string || HEALPIX || colspan="2"|
| |
| − | |-
| |
| − | |COORDSYS || string || GALACTIC || Coordinate system
| |
| − | |-
| |
| − | |ORDERING || string || NESTED || Healpix ordering
| |
| − | |-
| |
| − | |NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside
| |
| − | |-
| |
| − | |FIRSTPIX || Int*4 || 0 ||
| |
| − | |-
| |
| − | |LASTPIX || Int*4 || 50331647 ||
| |
| − | |- bgcolor="ffdead"
| |
| − | !colspan="4"| 2. EXTNAME = ''TransFun''
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Column Name || Data Type || Units || Description
| |
| − | |-
| |
| − | |RLPP || Real*4 || none || Response function
| |
| − | |-
| |
| − | |NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Keyword || Data Type || Value || Description
| |
| − | |-
| |
| − | |L_MIN || Int*4 || 0 || First multipole
| |
| − | |-
| |
| − | |L_MAX || Int*4 || 2048 || Last multipole
| |
| − | |}
| |
| − |
| |
| − | </div>
| |
| − | </div>
| |
| − |
| |
| − | == 2015 Lensing-induced <i>B</i>-mode map ==
| |
| − |
| |
| − | We distribute the Planck map of the lensing-induced <i>B</i>-modes presented in {{PlanckPapers|planck2015-XLI}}. The Stokes parameter maps of the lensing <i>B</i>-modes are produced by combining the lensing potential map extracted from the SMICA CMB temperature map with <i>E</i>-mode data from the SMICA CMB polarization maps. The SMICA temperature and polarization products are described in {{PlanckPapers|planck2014-a11}}. The lensing-induced <i>B</i>-mode polarization maps are used in cross-correlation with the SMICA CMB polarization maps to obtain a lensing <i>B</i>-mode power spectrum measurement from approximately 70% of the sky.
| |
| − |
| |
| − | We provide both raw products, which can be utilized to generate products adapted to one's specific needs in term of mask, filtering, etc., and "ready-to-use" products for cross-correlation study purposes.
| |
| − |
| |
| − | === Raw products ===
| |
| − |
| |
| − | We deliver the non-normalized lensing-induced Stokes parameter maps, labelled <math> \bar{Q}^{\rm{lens}} </math> and <math> \bar{U}^{\rm{lens}} </math>, which form the basis of the final lensing <i>B</i>-mode estimator defined in equation (6) of the paper. They are defined as
| |
| − |
| |
| − | <math> \begin{eqnarray}
| |
| − | \bar Q^{\rm{lens}}({\bf n}) &=& \widetilde Q^{E}({\bf n}) \cdot \nabla \widetilde \phi({\bf n}), \\
| |
| − | \bar U^{\rm{lens}}({\bf n}) &=& \widetilde U^{E}({\bf n}) \cdot \nabla \widetilde \phi({\bf n}),
| |
| − | \end{eqnarray} </math>
| |
| − |
| |
| − | where <math> \widetilde Q^{E} </math> and <math> \widetilde U^{E} </math> are the filtered pure <i>E</i>-mode polarization maps given in equation (5), and <math> \widetilde \phi</math> is the filtered lensing potential estimate.
| |
| − |
| |
| − | We also provide the normalization transfer function <math> \mathcal{B}_\ell </math> defined in equation (12), as well as the "B70" mask <math> M({\bf n}) </math> that retains 69% of the sky before
| |
| − | apodization, and its apodized version <math> \tilde{M}({\bf n}) </math>, which has an effective sky fraction <math> f_{\rm{sky}}^{\rm{eff}} = 65\% </math>.
| |
| − |
| |
| − | As an example of the utilization of these products, the lensing <i>B</i>-mode maps that are shown in figure 4 are generated from
| |
| − |
| |
| − | <math> Q^{\rm{lens}} \pm i U^{\rm{lens}} = \sum_{\ell m} \left( G_\ell \mathcal{B}_\ell^{-1} \int d{\bf n} {\, }_{\pm 2}Y_{\ell m}^*({\bf n}) \left(\bar{Q}^{\rm{lens}} \pm i \bar{U}^{\rm{lens}} \right) \right) {\, }_{\pm 2}Y_{\ell m}({\bf n}) </math>,
| |
| − |
| |
| − | where <math>G_\ell</math> is a Gaussian filter of 60 arcmin FWHM (introduced for highlighting large angular scales, although it can be removed or replaced by any other filter). This can be practically done by ingesting <math>\bar{Q}^{\rm{lens}} </math> and <math> \bar{U}^{\rm{lens}} </math> in the HEALPix "smoothing" routine, and using the product <math> G_\ell\mathcal{B}_\ell^{-1} </math> as an input filtering function.
| |
| − |
| |
| − | The lensing-induced Stokes parameter maps are provided without being masked for the user's convenience (in particular, it allows for various filtering to be tested). However, whenever they are utilized in view of obtaining scientific outcomes, they should be masked using the B70 mask, which is also provided.
| |
| − |
| |
| − | === Specific products ===
| |
| − |
| |
| − | We provide the lensing <i>B</i>-mode spherical harmonic coefficient estimate <math> B_{\ell m}^{\rm{lens}} </math> over approximately 70% of the sky.
| |
| − |
| |
| − | It can also be constructed using the raw products described above from
| |
| − |
| |
| − | <math> B_{\ell m}^{\rm{lens}} = f_{10 \rightarrow 2000} \, \mathcal{B}_\ell^{-1} \, \, {\, }_{\pm 2}\mathcal{Y} \left[ \tilde{M}({\bf n}) \left( \bar{Q}^{\rm{lens}}({\bf n}) \pm i \bar{U}^{\rm{lens}}({\bf n}) \right) \right] </math>,
| |
| − |
| |
| − | where <math> f_{10 \rightarrow 2000} </math> is a band-pass filter that retain the multipole range <math> 10 \le \ell \le 2000 </math>, and <math> {\, }_{\pm2}\mathcal{Y} </math> is a short-hand notation for transforming a map into spin-weighted spherical harmonic coefficients <math> {\, }_{+2}a_{\ell m}</math>, <math>{\, }_{-2}a_{\ell m} </math> and forming <math>1/(2i)\left({\, }_{+2}a_{\ell m} - {\, }_{-2}a_{\ell m}\right)</math>. This can be done using, e.g., the HEALPix "anafast" tool.
| |
| − |
| |
| − | The lensing <i>B</i>-mode power spectrum estimate <math> \hat{C}_\ell^{BB^{\rm{lens}}} </math> is obtained by forming the cross-correlation power spectrum of <math> B_{\ell m}^{\rm{lens}} </math> and the <i>B</i>-mode data from the SMICA polarization maps <math> B_{\ell m} </math>:
| |
| − |
| |
| − | <math> \hat{C}_\ell^{BB^{\rm{lens}}} = \frac{\left(f_{\rm{sky}}^{\rm{eff}}\right)^{-1}}{2 \ell +1} G_\ell^{-2} \sum_m B_{\ell m}^* B_{\ell m}^{\rm{lens}}</math>,
| |
| − |
| |
| − | where <math> G_\ell </math> is the 5 arcmin Gaussian beam that convolves the SMICA CMB maps.
| |
| − |
| |
| − |
| |
| − | The products are contained in a single gzipped tarball named [http://pla.esac.esa.int/pla/aio/product-action?COSMOLOGY.FILE_ID=COM_Lensing-Bmode_R2.01.tgz COM_Lensing-Bmode_R2.01.tgz]. Its contents are described below.
| |
| − |
| |
| − |
| |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
| |
| − | |+ ''' Contents of Lensing B-mode package '''
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Filename || Format || Description
| |
| − | |-
| |
| − | | bar_q_lens_map.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the non-normalized lensing-induced <i>Q</i> Stokes parameter map <math> \bar Q^{\rm{lens}}({\bf n}) </math>.
| |
| − | |-
| |
| − | | bar_u_lens_map.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the non-normalized lensing-induced <i>U</i> Stokes parameter map <math> \bar U^{\rm{lens}}({\bf n}) </math>.
| |
| − | |-
| |
| − | | mask.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || The B70 mask (apodized version).
| |
| − | |-
| |
| − | | mask_noapo.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || The B70 mask without apodization.
| |
| − | |-
| |
| − | | transfer_function_b_l.dat || ASCII text file, with columns = (<math>\ell</math>, <math> \mathcal{B}_\ell </math>) || The transfer function of the lensing B-mode estimator.
| |
| − | |-
| |
| − | | lensing_bmode_b_lm.fits || HEALPix FITS format alm, with <math> \ell_{\rm max} = 2000 </math> || Contains the lensing <i>B</i>-mode harmonic coefficients <math> B_{\ell m}^{\rm{lens}} </math>.
| |
| − | |-
| |
| − | | lensing_bmode_bandpowers.dat || ASCII text file, with columns = (<math>\ell_{\rm min}</math>, <math>\ell_{\rm b} </math>, <math>\ell_{\rm max} </math>, <math> \hat{C}_{\ell_{\rm b}}^{BB^{\rm{lens}}} </math>, <math> \Delta \hat{C}_{\ell_{\rm b}}^{BB^{\rm{lens}}} </math> ) || The lensing <i>B</i>-mode bandpower estimate on approximativily 70% of the sky and over the multipole range from 10 to 2000 shown in figure 10 of {{PlanckPapers|planck2015-XLI}} (for plotting purposes only).
| |
| − | |}
| |
| − |
| |
| − |
| |
| − | == 2015 Compton <i>y</i> parameter map ==
| |
| − |
| |
| − | We distribute here the Planck full mission Compton parameter maps (<i>y</i>-maps hereafter) obtained using the NILC and MILCA component-separation algorithms as described in {{PlanckPapers|planck2014-a28}}. We also provide the ILC weights per scale and per frequency that were used to produce these <i>y</i>-maps. IDL routines are also provided to allow the user to apply those weights. Compton parameters produced by keeping either the first or the second half of stable pointing periods are also provided; we call these the FIRST and LAST <i>y</i>-maps. Additionally we construct noise estimates of full mission Planck <i>y</i>-maps from the half difference of the FIRST and LAST <i>y</i>-maps. These estimates are used to construct standard deviation maps of the noise in the full mission Planck <i>y</i>-maps, which are also provided. To complement this we also provide the power spectra of the noise estimate maps after correcting for inhomogeneities using the standard deviation maps. We also deliver foreground masks including point-source and Galactic masks.
| |
| − |
| |
| − | <span style="color:#ff0000"> Update 04 Aug 2017:</span> The file containing the masks named ''COM_CompMap_Compton-SZMap-masks_2048_R2.00.fits'' has been updated with the file ''COM_CompMap_Compton-SZMap-masks_2048_R2.01.fits''. The difference between the two is that in the R2.00 version a region around the Galactic pole had been masked, while only the Galactic plane should be masked. This has been fixed in version R2.01. The full updated data set is contained in a single gzipped tarball named ''COM_CompMap_YSZ_R2.01.fits.tgz''. The R2.00 version of the mask is not available in the PLA anymore, but can be requested via the PLA Helpdesk.
| |
| − |
| |
| − | The contents of the full data set are described below.
| |
| − |
| |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
| |
| − | |+ ''' Contents of COM_CompMap_YSZ_R2.01.fits.tgz '''
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Filename || Format || Description
| |
| − | |-
| |
| − | | nilc_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math>N_{\rm side}=2048 </math>|| Contains the NILC full mission, FIRST and LAST <i>y</i>-maps.
| |
| − | |-
| |
| − | | milca_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the MILCA full mission, FIRST and LAST <i>y</i>-maps.
| |
| − | |-
| |
| − | | nilc_weights_BAND.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 128 </math>|| Contains the NILC ILC weights for the full mission <i>y</i>-map for band BAND 0 to 9. For each band we provide a weight map per frequency.
| |
| − | |-
| |
| − | | milca_FREQ_Csz.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the MILCA ILC weights for the full mission <i>y</i>-map for frequency FREQ (100, 143, 217, 353, 545, 857). For each frequency we provide a weight map per filter band.
| |
| − | |-
| |
| − | | nilc_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math>|| Contains the stddev map for the NILC full mission <i>y</i>-map.
| |
| − | |-
| |
| − | | milca_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the stddev maps for the MILCA full mission <i>y</i>-map.
| |
| − | |-
| |
| − | | nilc_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the NILC full mission <i>y</i>-map.
| |
| − | |-
| |
| − | | milca_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the MILCA full mission <i>y</i>-map.
| |
| − | |-
| |
| − | | masks.fits || HEALPix FITS format map, with <math> N_{\rm side} = 2048 </math> || Contains foreground masks.
| |
| − | |-
| |
| − | | nilc_bands.fits || ASCII table FITS format || Contains NILC wavelet bands in multipole space
| |
| − | |}
| |
| − |
| |
| − | == 2015 Integrated Sachs-Wolfe effect map ==
| |
| − |
| |
| − | We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in {{PlanckPapers|planck2014-a26}} as part of the 2015 data release. These map represents an estimate of the ISW anisotropies using different data sets:
| |
| − |
| |
| − | * SEVEM DX11 CMB map, together with all the large-scale structure tracers considered in the ISW paper, namely: NVSS, SDSS, WISE, and the Planck lensing map
| |
| − | * Using only the large-scale structure tracers mentioned above
| |
| − | * SEVEM DX11 CMB map, together with NVSS and the Planck lensing maps (since these two tracers capture most of the information, as compared to SDSS and WISE)
| |
| − |
| |
| − |
| |
| − | For all the three cases, the reconstruction is provided on approximately 85% of the sky, and they are produced using the LCB filter described in the Planck ISW paper (Section 5), described in detail in [http://cdsads.u-strasbg.fr/abs/2008ISTSP...2..747B| Barreiro et al. 2008] and [http://cdsads.u-strasbg.fr/doi/10.1093/mnras/stw415| Bonavera et al. 2016].
| |
| − |
| |
| − | These ISW maps, together with their corresponding uncertainties maps and masks, are given in a file named ''{{PLASingleFile|fileType=map|name=COM_CompMap_ISW_0064_R2.00.fits|link=COM_CompMap_ISW_0064_R2.00.fits}}''. Its contents are described below.
| |
| − |
| |
| − |
| |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
| |
| − | |+ ''' Contents of the ISW maps file: COM_CompMap_ISW_0064_R2.00.fits '''
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Extension || Format || Description || Used data sets
| |
| − | |-
| |
| − | | 0 || HEALPix FITS format map with three components, <math>N_{\rm side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map || SEVEM DX11 CMB + NVSS + SDSS + WISE + Planck lensing.
| |
| − | |-
| |
| − | | 1 || HEALPix FITS format map with three components, <math>N_{\rm side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map || NVSS + SDSS + WISE + Planck lensing.
| |
| − | |-
| |
| − | | 2 || HEALPix FITS format map with three components, <math>N_{\rm side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map || SEVEM DX11 CMB + NVSS + Planck lensing.
| |
| − | |}
| |
| − |
| |
| − | == 2015 Low-frequency foregrounds maps (Planck only & Planck+WMAP) ==
| |
| − | 1) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck only)
| |
| − |
| |
| − | Linear combination of Planck 28.4, 44.1, 143 and 353 GHz maps (all at 1 degree resolution), with weights listed in column w_2 of Table 1 in {{PlanckPapers|planck2014-a31}}. These weights exactly null the CMB, almost exactly null free-free emission, and null thermal dust emission to high accuracy except along the inner Galactic plane,where the brightness is uncertain by around 20% due to variation in the dust spectrum. The normalisation leaves a beta = -3 power law at the same amplitude as in the Planck 28.4 GHz map. (As presented in Fig. 3a of Planck 2015 Results XXV.)
| |
| − |
| |
| − | 2) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck + WMAP)
| |
| − | Linear combination of WMAP K, Ka, and Q band, and Planck 28.4, 44.1, 143 and 353 GHz maps (all at 1 degree resolution), with weights listed in column w_3 of Table 1 in {{PlanckPapers|planck2014-a31}}. These weights exactly null the CMB, almost exactly null free-free emission, and null thermal dust emission to high accuracy except along the inner Galactic plane, where the brightness is uncertain by around 20% due to variation in the dust spectrum. The normalisation leaves a beta = -3 power law at the same amplitude as in the Planck 28.4 GHz map. (As presented in Fig. 3b of {{PlanckPapers|planck2014-a31}}.)
| |
| | | | |
| | = Previous Releases: (2015) and (2013) Foreground Maps = | | = Previous Releases: (2015) and (2013) Foreground Maps = |
| Line 1,141: |
Line 180: |
| | <div class="mw-collapsible-content"> | | <div class="mw-collapsible-content"> |
| | | | |
| − | ''' Overview '''
| + | == Overview == |
| | 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 each product and how it is obtained, followed by a description of the FITS file containing the data and associated information. | | 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 each product and how it is obtained, followed by a description of the FITS file containing the data and associated information. |
| | All the details can be found in {{PlanckPapers|planck2014-a12}} and {PlanckPapers|planck20}}. | | All the details can be found in {{PlanckPapers|planck2014-a12}} and {PlanckPapers|planck20}}. |
| | | | |
| − | ''' Astrophysical foregrounds from parametric component separation '''
| + | == Astrophysical foregrounds from parametric component separation == |
| | We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}. | | We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}. |
| | | | |
| Line 1,174: |
Line 213: |
| | '''Outputs''' | | '''Outputs''' |
| | | | |
| − | '''Synchrotron emission'''
| + | ===Synchrotron emission=== |
| | | | |
| | <!--<center> | | <!--<center> |
| Line 1,212: |
Line 251: |
| | |} | | |} |
| | | | |
| − | '''Free-free emission'''
| + | |
| | + | ===Free-free emission=== |
| | | | |
| | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}} | | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_freefree-commander_0256_R2.00.fits|link=COM_CompMap_freefree-commander_0256_R2.00.fits}} |
| Line 1,239: |
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| | | | |
| | | | |
| − | '''Spinning dust emission'''
| + | ===Spinning dust emission=== |
| | | | |
| | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}} | | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_AME-commander_0256_R2.00.fits|link=COM_CompMap_AME-commander_0256_R2.00.fits}} |
| Line 1,294: |
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| | |} | | |} |
| | | | |
| − | '''CO line emission'''
| + | ===CO line emission=== |
| | | | |
| | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}} | | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_CO-commander_0256_R2.00.fits|link=COM_CompMap_CO-commander_0256_R2.00.fits}} |
| Line 1,341: |
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| | |} | | |} |
| | | | |
| − | '''94/100 GHz line emission'''
| + | ===94/100 GHz line emission=== |
| | | | |
| | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-commander_0256_R2.00.fits}} | | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_xline-commander_0256_R2.00.fits|link=COM_CompMap_xline-commander_0256_R2.00.fits}} |
| Line 1,362: |
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| | Note: The amplitude of this component is normalized according to the 100-ds1 detector set map, ie., it is the amplitude as measured by this detector combination. | | Note: The amplitude of this component is normalized according to the 100-ds1 detector set map, ie., it is the amplitude as measured by this detector combination. |
| | | | |
| − | '''Thermal dust emission'''
| + | ===Thermal dust emission=== |
| | | | |
| | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}} | | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_dust-commander_0256_R2.00.fits|link=COM_CompMap_dust-commander_0256_R2.00.fits}} |
| Line 1,394: |
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| | |} | | |} |
| | | | |
| − | '''Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters'''
| + | ===Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters=== |
| | | | |
| | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SZ-commander_0256_R2.00.fits|link=COM_CompMap_SZ-commander_0256_R2.00.fits}} | | : File name: {{PLASingleFile|fileType=map|name=COM_CompMap_SZ-commander_0256_R2.00.fits|link=COM_CompMap_SZ-commander_0256_R2.00.fits}} |
| Line 1,715: |
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| | | | |
| | | | |
| − | ''' Other Special maps '''
| |
| | | | |
| − | '''Introduction'''
| |
| | | | |
| − | This section describes the map-based products that required special processing.
| + | == Thermal dust and CIB all-sky maps from GNILC component separation == |
| | + | We describe diffuse foreground products for the Planck 2015 release produced with the GNILC component separation method. See the Planck paper {{PlanckPapers|planck2016-XLVIII}} for a detailed discussion on these products. |
| | | | |
| − | ''' 2015 lensing map '''
| + | ===Method=== |
| | | | |
| − | We distribute the minimum-variance (MV) lensing potential estimate presented in {{PlanckPapers|planck2014-a17}} as part of the 2014 data release. This map represents an estimate of the CMB lensing potential on approximately 70% of the sky, and also forms the basis for the Planck 2014 lensing likelihood. It is produced using filtered temperature and polarization data from the SMICA DX11 CMB map; its construction is discussed in detail in {{PlanckPapers|planck2014-a11}}.
| + | : The basic idea behind the Generalized Needlet Internal Linear Combination (GNILC) component-separation method ([http://adsabs.harvard.edu/abs/2011MNRAS.418..467R Remazeilles et al, MNRAS 2011]) is to disentangle specific components of emission not on the sole basis of the spectral (frequency) information but also on the basis of their distinct spatial information (angular power spectrum). The GNILC method has been applied to Planck data in order to disentangle Galactic dust emission and Cosmic Infrared Background (CIB) anisotropies. Both components have a similar spectral signature but a distinct angular power spectrum (spatial signature). The spatial information used by GNILC is under the form of priors for the angular power spectra of the CIB, the CMB, and the instrumental noise. No assumption is made on the Galactic signal, neither spectral or spatial. In that sense, GNILC is a blind component-separation method. GNILC operates on a needlet (spherical wavelet) frame, therefore adapting the component separation to the local conditions of contamination both over the sky and over the angular scales. |
| | | | |
| | + | ===Data=== |
| | | | |
| − | The estimate is contained in a single gzipped tarball named ''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R2.00.tgz|link=COM_CompMap_Lensing_2048_R2.00.tgz}}''. Its contents are described below. The convergence map "dat_klm.fits" that can be found in the tarball, has been categorized as COM_Lensing-Convergence-dat-klm_2048_R2.00.fits in the Lensing Products section of the archive. | + | : The data used by GNILC for the analysis are the Planck data release 2 (PR2) frequency maps from 30 to 857 GHz, and a 100 micron hybrid map combined from the SFD map ([http://adsabs.harvard.edu/abs/1998ApJ...500..525S Schlegel et al, ApJ 1998]) at large angular scales (> 30') and the IRIS map ([http://adsabs.harvard.edu/abs/2005ApJS..157..302M Miville-Deschênes et al, ApJS 2005]) at small angular scales (< 30'). This special 100 micron map can be obtained in the External Maps section of the PLA. |
| | | | |
| | + | ===Pre-processing=== |
| | | | |
| | + | : The point-sources with a signal-to-noise ratio, S/N > 5, in each individual frequency map (30 to 857 GHz, and 100 micron) have been pre-processed by a minimum curvature surface inpainting technique ([http://adsabs.harvard.edu/abs/2015MNRAS.451.4311R Remazeilles et al, MNRAS 2015]) prior to performing component separation with GNILC. |
| | | | |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"
| + | ===GNILC thermal dust and CIB products=== |
| − | |+ ''' Contents of Lensing package '''
| |
| − | |- bgcolor="ffdead"
| |
| − | ! Filename || Format || Description
| |
| − | |-
| |
| − | | dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm max}=2048</math> || Contains the estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math>.
| |
| − | |-
| |
| − | | mask.fits.gz || HEALPix FITS format map, with <math>N_{\rm side}=2048</math> || Contains the lens reconstruction analysis mask.
| |
| − | |-
| |
| − | | nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>N_L </math>, <math>C_L+N_L</math>) || The approximate noise <math>N_L</math> (and signal+noise, <math>C_L+N_L</math>) power spectrum of <math> \hat{\kappa}_{LM} </math>, for the fiducial cosmology used in {{PlanckPapers|planck2014-a15}}.
| |
| − | |}
| |
| | | | |
| − | ''' 2015 Compton <i>y</i> parameter map ''' | + | The result of GNILC component separation are thermal dust and CIB maps at 353, 545, and 857 GHz. In addition, by fitting a modified blackbody model to the GNILC thermal dust products at 353, 545, 857, and 100 micron, we have created all-sky maps of the dust optical depth, dust temperature, and dust emmissivity index. Note that the thermal dust maps have a variable angular resolution over the sky with an effective beam FWHM varying from 21.8' to 5'. The dust beam FWHM map is also released as a product. |
| | | | |
| − | We distribute here the Planck full mission Compton parameter maps (<i>y</i>-maps hereafter) obtained using the NILC and MILCA component-separation algorithms as described in {{PlanckPapers|planck2014-a28}}. We also provide the ILC weights per scale and per frequency that were used to produce these <i>y</i>-maps. IDL routines are also provided to allow the user to apply those weights. Compton parameters produced by keeping either the first or the second half of stable pointing periods are also provided; we call these the FIRST and LAST <i>y</i>-maps. Additionally we construct noise estimates of full mission Planck <i>y</i>-maps from the half difference of the FIRST and LAST <i>y</i>-maps. These estimates are used to construct standard deviation maps of the noise in the full mission Planck <i>y</i>-maps, which are also provided. To complement this we also provide the power spectra of the noise estimate maps after correcting for inhomogeneities using the standard deviation maps. We also deliver foreground masks including point-source and Galactic masks.
| + | ====Thermal dust maps==== |
| | | | |
| − | The full data set is contained in a single gzipped tarball named ''COM_CompMap_YSZ_R2.00.fits.tgz''. Its contents are described below.
| + | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center" |
| − | ''Temporarily the tarball file can be found in the Supplement Data area of the PLA (go to pla.esac.esa.int/pla, go to Subsection Supplementary Data and type "YSZ" in the search form)''
| + | |+ HDU -- COMP-MAP-DUST |
| − | | |
| − | | |
| − | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" | |
| − | |+ ''' Contents of COM_CompMap_YSZ_R2.00.fits.tgz} ''' | |
| − | |- bgcolor="ffdead"
| |
| − | ! Filename || Format || Description
| |
| | |- | | |- |
| − | | nilc_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math>N_{\rm side}=2048 </math>|| Contains the NILC full mission, FIRST and LAST <i>y</i>-maps. | + | |- bgcolor="ffdead" |
| | + | ! File Name || Nside || Units || Reference frequency || Angular resolution || Description |
| | |- | | |- |
| − | | milca_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the MILCA full mission, FIRST and LAST <i>y</i>-maps. | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F353_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F353_2048_R2.00.fits}} || 2048 || MJy/sr || 353 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust amplitude at 353 GHz |
| | |- | | |- |
| − | | nilc_weights_BAND.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 128 </math>|| Contains the NILC ILC weights for the full mission <i>y</i>-map for band BAND 0 to 9. For each band we provide a weight map per frequency. | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F545_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F545_2048_R2.00.fits}} || 2048 || MJy/sr || 545 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust amplitude at 545 GHz |
| | |- | | |- |
| − | | milca_FREQ_Csz.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the MILCA ILC weights for the full mission <i>y</i>-map for frequency FREQ (100, 143, 217, 353, 545, 857). For each frequency we provide a weight map per filter band. | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-F857_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-F857_2048_R2.00.fits}} || 2048 || MJy/sr || 857 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust amplitude at 857 GHz |
| | |- | | |- |
| − | | nilc_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math>|| Contains the stddev map for the NILC full mission <i>y</i>-map. | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Opacity_2048_R2.00.fits}}|| 2048 || NA || 353 GHz || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust optical depth at 353 GHz |
| | |- | | |- |
| − | | milca_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the stddev maps for the MILCA full mission <i>y</i>-map. | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Spectral-Index_2048_R2.00.fits}} || 2048 || NA || NA || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust emissivity index |
| | |- | | |- |
| − | | nilc_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the NILC full mission <i>y</i>-map. | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.01.fits|link=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.01.fits}} (version 2.01 includes the error map)<br>{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Model-Temperature_2048_R2.00.fits}} || 2048 || K || NA || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust temperature |
| | |- | | |- |
| − | | milca_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the MILCA full mission <i>y</i>-map. | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Radiance_2048_R2.00.fits|link=COM_CompMap_Dust-GNILC-Radiance_2048_R2.00.fits}} || 2048 || W/m<sup>2</sup>/sr || NA || {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || Thermal dust radiance |
| | |- | | |- |
| − | | masks.fits || HEALPix FITS format map, with <math> N_{\rm side} = 2048 </math> || Contains foreground masks. | + | | {{PLASingleFile|fileType=map|name=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits|link=COM_CompMap_Dust-GNILC-Beam-FWHM_0128_R2.00.fits}} || 128 || Arcminute || NA || NA || Effective dust beam FWHM |
| | |- | | |- |
| − | | nilc_bands.fits || ASCII table FITS format || Contains NILC wavelet bands in multipole space
| |
| | |} | | |} |
| | | | |
| − | ''' 2015 lensing-induced <i>B</i>-mode map '''
| + | ====CIB maps==== |
| | | | |
| − | We distribute the lensing-induced <i>B</i>-mode map presented in {{PlanckPapers|planck2015-XLI}}. The lensing <i>B</i>-mode Stokes parameter maps are produced by combining the lensing potential reconstruction from the SMICA CMB temperature map with <i>E</i>-mode data from the SMICA CMB polarization maps. The SMICA temperature and polarization products are described in {{PlanckPapers|planck2014-a11}}. The lensing-induced <i>B</i>-mode polarization maps are used in cross-correlation with the SMICA CMB polarization maps to obtain a lensing <i>B</i>-mode power spectrum measurement from approximately 70% of the sky, as described in {{PlanckPapers|planck2015-XLI}}.
| |
| | | | |
| − | We provide both raw products, which can be utilized to generate products adapted to one's specific needs in term of mask, filtering, etc., and "ready-to-use" products for cross-correlation study purposes.
| + | {| border="1" cellpadding="5" cellspacing="0" align="center" style="text-align:center" |
| | + | |+ HDU -- COMP-MAP-CIB |
| | + | |- |
| | + | |- bgcolor="ffdead" |
| | + | ! File Name || Nside || Units || Reference frequency || Angular resolution || Description |
| | + | |- |
| | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F353_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F353_2048_R2.00.fits}} || 2048 || MJy/sr || 353 GHz || 5 arcmin || CIB amplitude at 353 GHz |
| | + | |- |
| | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F545_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F545_2048_R2.00.fits}} || 2048 || MJy/sr || 545 GHz || 5 arcmin || CIB amplitude at 545 GHz |
| | + | |- |
| | + | |{{PLASingleFile|fileType=map|name=COM_CompMap_CIB-GNILC-F857_2048_R2.00.fits|link=COM_CompMap_CIB-GNILC-F857_2048_R2.00.fits}} || 2048 || MJy/sr || 857 GHz || 5 arcmin || CIB amplitude at 857 GHz |
| | + | |- |
| | + | |} |
| | | | |
| − | ''' Raw products '''
| |
| | | | |
| − | We deliver the non-normalized lensing-induced Stokes parameter maps, labelled <math> \bar{Q}^{\rm{lens}} </math> and <math> \bar{U}^{\rm{lens}} </math>, which form the basis of the final lensing <i>B</i>-mode estimator defined in equation (6) of {{PlanckPapers|planck2015-XLI}}. They are defined as
| + | == Other Special maps == |
| | | | |
| − | <math> \begin{eqnarray}
| + | ===Introduction=== |
| − | \bar Q^{\rm{lens}}({\bf n}) &=& \widetilde Q^{E}({\bf n}) \cdot \nabla \widetilde \phi({\bf n}), \\
| |
| − | \bar U^{\rm{lens}}({\bf n}) &=& \widetilde U^{E}({\bf n}) \cdot \nabla \widetilde \phi({\bf n}),
| |
| − | \end{eqnarray} </math>
| |
| | | | |
| − | where <math> \widetilde Q^{E} </math> and <math> \widetilde U^{E} </math> are the filtered pure <i>E</i>-mode polarization maps given in equation (5) of {{PlanckPapers|planck2015-XLI}}, and <math> \widetilde \phi</math> is the filtered lensing potential estimate.
| + | This section describes the map-based products that required special processing. |
| | | | |
| − | We also provide the normalization transfer function <math> \mathcal{B}_\ell </math> defined in equation (11) of {{PlanckPapers|planck2015-XLI}}, as well as the "L70" mask <math> M({\bf n}) </math> that retains 69% of the sky before
| |
| − | apodization, and its apodized version <math> \tilde{M}({\bf n}) </math>, which has an effective sky fraction <math> f_{\rm{sky}}^{\rm{eff}} = 65\% </math>.
| |
| | | | |
| − | As an example of the utilization of these products, the lensing <i>B</i>-mode maps that are shown in figure 4 of {{PlanckPapers|planck2015-XLI}} are generated from
| + | === 2015 Compton <i>y</i> parameter map === |
| − |
| |
| − | <math> Q^{\rm{lens}} \pm i U^{\rm{lens}} = \sum_{\ell m} \left( G_\ell \mathcal{B}_\ell^{-1} \int d{\bf n} {\, }_{\pm 2}Y_{\ell m}^*({\bf n}) \left(\bar{Q}^{\rm{lens}} \pm i \bar{U}^{\rm{lens}} \right) \right) {\, }_{\pm 2}Y_{\ell m}({\bf n}) </math>,
| |
| − |
| |
| − | where <math>G_\ell</math> is a Gaussian of 60 arcmin FWHM (introduced for highlighting large angular scales, although it can be removed or replaced by any other filter). This can be practically done by ingesting <math>\bar{Q}^{\rm{lens}} </math> and <math> \bar{U}^{\rm{lens}} </math> in the HEALPix "smoothing" routine, and using the product <math> G_\ell\mathcal{B}_\ell^{-1} </math> as an input filtering function.
| |
| | | | |
| − | ''' Specific products '''
| + | We distribute here the Planck full mission Compton parameter maps (<i>y</i>-maps hereafter) obtained using the NILC and MILCA component-separation algorithms as described in {{PlanckPapers|planck2014-a28}}. We also provide the ILC weights per scale and per frequency that were used to produce these <i>y</i>-maps. IDL routines are also provided to allow the user to apply those weights [[:File: milca_nilc_IDL_routines.zip]]. Compton parameters produced by keeping either the first or the second half of stable pointing periods are also provided; we call these the FIRST and LAST <i>y</i>-maps. Additionally we construct noise estimates of full mission Planck <i>y</i>-maps from the half difference of the FIRST and LAST <i>y</i>-maps. These estimates are used to construct standard deviation maps of the noise in the full mission Planck <i>y</i>-maps, which are also provided. To complement this we also provide the power spectra of the noise estimate maps after correcting for inhomogeneities using the standard deviation maps. We also deliver foreground masks including point-source and Galactic masks. |
| | | | |
| − | We provide the lensing <i>B</i>-mode spherical harmonic coefficient estimate <math> B_{\ell m}^{\rm{lens}} </math> over approximately 70% of the sky.
| + | <span style="color:#ff0000"> Update 04 Aug 2017:</span> The file containing the masks named ''COM_CompMap_Compton-SZMap-masks_2048_R2.00.fits'' has been updated with the file ''COM_CompMap_Compton-SZMap-masks_2048_R2.01.fits''. The difference between the two is that in the R2.00 version a region around the Galactic pole had been masked, while only the Galactic plane should be masked. This has been fixed in version R2.01. The full updated data set is contained in a single gzipped tarball named ''COM_CompMap_YSZ_R2.01.fits.tgz''. The R2.00 version of the mask is not available in the PLA anymore, but can be requested via the PLA Helpdesk. |
| | | | |
| − | It can also be constructed using the raw products described above from
| + | <span style="color:#ff0000"> Update 30 July 2018:</span> The angular power spectra homogeneous noise files nilc_homnoise_spect.fits and milca_homnoise_spect.fits in COM_CompMap_YSZ_R2.01.fits.tgz have been updated. A new version of the COM_CompMap_SZ_R2.02.fits.tgz package is available in the PLA. |
| − | | |
| − | <math> B_{\ell m}^{\rm{lens}} = f_{10 \rightarrow 2000} \, \mathcal{B}_\ell^{-1} \, \, {\, }_{\pm 2}\mathcal{Y} \left[ \tilde{M}({\bf n}) \left( \bar{Q}^{\rm{lens}}({\bf n}) \pm i \bar{U}^{\rm{lens}}({\bf n}) \right) \right] </math>, | |
| − | | |
| − | where <math> f_{10 \rightarrow 2000} </math> is a function for producing band-powers over the range <math> 10 \le \ell \le 2000 </math>, and <math> {\, }_{\pm2}\mathcal{Y} </math> is a short-hand notation for transforming a map into spin-weighted spherical harmonic coefficients <math> {\, }_{+2}a_{\ell m}</math>, <math>{\, }_{-2}a_{\ell m} </math> and forming <math>1/(2i)\left({\, }_{+2}a_{\ell m} - {\, }_{-2}a_{\ell m}\right)</math>. This can be done using, e.g., the HEALPix "anafast" tool.
| |
| − | | |
| − | The lensing <i>B</i>-mode power spectrum estimate <math> \hat{C}_\ell^{BB^{\rm{lens}}} </math> discussed in {{PlanckPapers|planck2015-XLI}} is obtained by forming the cross-correlation power spectrum of <math> B_{\ell m}^{\rm{lens}} </math> and the <i>B</i>-mode data from the SMICA polarization maps <math> B_{\ell m} </math>:
| |
| − |
| |
| − | <math> \hat{C}_\ell^{BB^{\rm{lens}}} = \frac{\left(f_{\rm{sky}}^{\rm{eff}}\right)^{-1}}{2 \ell +1} G_\ell^{-2} \sum_m B_{\ell m}^* B_{\ell m}^{\rm{lens}}</math>,
| |
| − | | |
| − | where <math> G_\ell </math> is the 5 arcmin Gaussian beam that convolves the SMICA CMB maps.
| |
| − | | |
| − | | |
| − | The products are contained in a single gzipped tarball named ''{{PLASingleFile|fileType=map|name=COM_Lensing-Bmode_R2.00.tgz|link=COM_Lensing-Bmode_R2.00.tgz}}''. Its contents are described below.
| |
| | | | |
| | + | The contents of the full data set are described below. |
| | | | |
| | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" | | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" |
| − | |+ ''' Contents of Lensing B-mode package ''' | + | |+ ''' Contents of COM_CompMap_YSZ_R2.02.fits.tgz ''' |
| | |- bgcolor="ffdead" | | |- bgcolor="ffdead" |
| | ! Filename || Format || Description | | ! Filename || Format || Description |
| | |- | | |- |
| − | | bar_q_lens_map.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the non-normalized lensing-induced <i>Q</i> Stokes parameter map <math> \bar Q^{\rm{lens}}({\bf n}) </math>. | + | | nilc_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math>N_{\rm side}=2048 </math>|| Contains the NILC full mission, FIRST and LAST <i>y</i>-maps. |
| | |- | | |- |
| − | | bar_u_lens_map.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the non-normalized lensing-induced <i>U</i> Stokes parameter map <math> \bar U^{\rm{lens}}({\bf n}) </math>. | + | | milca_ymaps.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the MILCA full mission, FIRST and LAST <i>y</i>-maps. |
| | |- | | |- |
| − | | mask.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || The L70 mask. | + | | nilc_weights_BAND.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 128 </math>|| Contains the NILC ILC weights for the full mission <i>y</i>-map for band BAND 0 to 9. For each band we provide a weight map per frequency. |
| | + | |- |
| | + | | milca_FREQ_Csz.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the MILCA ILC weights for the full mission <i>y</i>-map for frequency FREQ (100, 143, 217, 353, 545, 857). For each frequency we provide a weight map per filter band. |
| | + | |- |
| | + | | nilc_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math>|| Contains the stddev map for the NILC full mission <i>y</i>-map. |
| | + | |- |
| | + | | milca_stddev.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || Contains the stddev maps for the MILCA full mission <i>y</i>-map. |
| | |- | | |- |
| − | | mask_noapo.fits || HEALPix FITS format map in Galactic coordinates with <math> N_{\rm side} = 2048 </math> || The L70 mask without apodization. | + | | nilc_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the NILC full mission <i>y</i>-map. |
| | |- | | |- |
| − | | transfer_function_b_l.dat || ASCII text file, with columns = (<math>\ell</math>, <math> \mathcal{B}_\ell </math>) || The transfer function. | + | | milca_homnoise_spect.fits || ASCII table FITS format || Contains the angular power spectrum of the homogeneous noise in the MILCA full mission <i>y</i>-map. |
| | |- | | |- |
| − | | lensing_bmode_b_lm.fits || HEALPix FITS format alm, with <math> \ell_{\rm max} = 2000 </math> || Contains the lensing <i>B</i>-mode harmonic coefficients <math> B_{\ell m}^{\rm{lens}} </math>. | + | | masks.fits || HEALPix FITS format map, with <math> N_{\rm side} = 2048 </math> || Contains foreground masks. |
| | |- | | |- |
| − | | lensing_bmode_bandpowers.dat || ASCII text file, with columns = (<math>\ell_{\rm min}</math>, <math>\ell_{\rm b} </math>, <math>\ell_{\rm max} </math>, <math> \hat{C}_{\ell_{\rm b}}^{BB^{\rm{lens}}} </math>, <math> \Delta \hat{C}_{\ell_{\rm b}}^{BB^{\rm{lens}}} </math> ) || The lensing <i>B</i>-mode bandpower estimate on approximativily 70% of the sky and over the multipole range from 10 to 2000 shown in figure 9 of {{PlanckPapers|planck2015-XLI}} (for plotting purposes only). | + | | nilc_bands.fits || ASCII table FITS format || Contains NILC wavelet bands in multipole space |
| | |} | | |} |
| | | | |
| − | ''' 2015 Integrated Sachs-Wolfe effect map '''
| + | === 2015 Integrated Sachs-Wolfe effect map === |
| | | | |
| | We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in {{PlanckPapers|planck2014-a26}} as part of the 2015 data release. These map represents an estimate of the ISW anisotropies using different data sets: | | We distribute estimates of the integrated Sachs-Wolfe (ISW) maps presented in {{PlanckPapers|planck2014-a26}} as part of the 2015 data release. These map represents an estimate of the ISW anisotropies using different data sets: |
| Line 1,849: |
Line 870: |
| | * Using only the large-scale structure tracers mentioned above | | * Using only the large-scale structure tracers mentioned above |
| | * SEVEM DX11 CMB map, together with NVSS and the Planck lensing maps (since these two tracers capture most of the information, as compared to SDSS and WISE) | | * SEVEM DX11 CMB map, together with NVSS and the Planck lensing maps (since these two tracers capture most of the information, as compared to SDSS and WISE) |
| − |
| |
| | | | |
| | For all the three cases, the reconstruction is provided on approximately 85% of the sky, and they are produced using the LCB filter described in the Planck ISW paper (Section 5), described in detail in [http://cdsads.u-strasbg.fr/abs/2008ISTSP...2..747B| Barreiro et al. 2008] and [http://cdsads.u-strasbg.fr/doi/10.1093/mnras/stw415| Bonavera et al. 2016]. | | For all the three cases, the reconstruction is provided on approximately 85% of the sky, and they are produced using the LCB filter described in the Planck ISW paper (Section 5), described in detail in [http://cdsads.u-strasbg.fr/abs/2008ISTSP...2..747B| Barreiro et al. 2008] and [http://cdsads.u-strasbg.fr/doi/10.1093/mnras/stw415| Bonavera et al. 2016]. |
| Line 1,867: |
Line 887: |
| | | 2 || HEALPix FITS format map with three components, <math>N_{\rm side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map || SEVEM DX11 CMB + NVSS + Planck lensing. | | | 2 || HEALPix FITS format map with three components, <math>N_{\rm side}=64</math>, Ordering='Nest' || Contains three components: i) ISW map [Kelvin], ii) Error map [Kelvin], iii) Mask map || SEVEM DX11 CMB + NVSS + Planck lensing. |
| | |} | | |} |
| | + | |
| | + | |
| | + | === 2015 Low-frequency foregrounds maps (Planck only & Planck+WMAP) === |
| | + | 1) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck only) |
| | + | |
| | + | Linear combination of Planck 28.4, 44.1, 143 and 353 GHz maps (all at 1 degree resolution), with weights listed in column w_2 of Table 1 in {{PlanckPapers|planck2014-a31}}. These weights exactly null the CMB, almost exactly null free-free emission, and null thermal dust emission to high accuracy except along the inner Galactic plane,where the brightness is uncertain by around 20% due to variation in the dust spectrum. The normalisation leaves a beta = -3 power law at the same amplitude as in the Planck 28.4 GHz map. (As presented in Fig. 3a of Planck 2015 Results XXV.) |
| | + | |
| | + | 2) CMB/free-free/Dust Nulled ILC at 28.4 GHz (Planck + WMAP) |
| | + | Linear combination of WMAP K, Ka, and Q band, and Planck 28.4, 44.1, 143 and 353 GHz maps (all at 1 degree resolution), with weights listed in column w_3 of Table 1 in {{PlanckPapers|planck2014-a31}}. These weights exactly null the CMB, almost exactly null free-free emission, and null thermal dust emission to high accuracy except along the inner Galactic plane, where the brightness is uncertain by around 20% due to variation in the dust spectrum. The normalisation leaves a beta = -3 power law at the same amplitude as in the Planck 28.4 GHz map. (As presented in Fig. 3b of {{PlanckPapers|planck2014-a31}}.) |
| | | | |
| | </div> | | </div> |
