Difference between revisions of "Catalogues"

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{{DISPLAYTITLE:2015 Catalogues}}
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{{DISPLAYTITLE:Catalogues}}
 +
The 2015 compact source catalogues will not be regenerated using data from the 2018 release and remain the most up-to-date products.
  
== (2015) Second Catalogue of Compact Sources ==
+
<div class="toccolours" style="background-color: #FFDAB9" >
 +
 
 +
=== (2015) Second Catalogue of Compact Sources (PCCS2 and PCCS2E)===
  
 
The second Planck Catalogue of Compact Sources (PCCS2) is a set of single-frequency source catalogues extracted from the Planck full-mission maps in intensity and polarization (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_SkyMap_???_2048_R2.00_full.fits). The catalogues have been constructed as described in  [[Compact_Source_catalogues#Planck_Catalogue_of_Compact_Sources|PCCS]] and in section 2 of {{PlanckPapers|planck2014-a35}}. The validation of the catalogues is described in section 3 of {{PlanckPapers|planck2014-a35}}.
 
The second Planck Catalogue of Compact Sources (PCCS2) is a set of single-frequency source catalogues extracted from the Planck full-mission maps in intensity and polarization (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_SkyMap_???_2048_R2.00_full.fits). The catalogues have been constructed as described in  [[Compact_Source_catalogues#Planck_Catalogue_of_Compact_Sources|PCCS]] and in section 2 of {{PlanckPapers|planck2014-a35}}. The validation of the catalogues is described in section 3 of {{PlanckPapers|planck2014-a35}}.
  
The catalogue at 100 GHz and above has been divided into two sub-catalogues: the PCCS2, here the sources have been detected in regions of the sky where it is possible to estimate the reliability of the detections, either statistically or by using external catalogues; PCCS2, here the detected sources are located in regions of the sky where it is not possible to make an estimate of their reliability.  
+
The catalogue at 100 GHz and above has been divided into two sub-catalogues: the PCCS2, in which the sources have been detected in regions of the sky where it is possible to estimate the reliability of the detections, either statistically or by using external catalogues; and PCCS2E, in which the detected sources are located in regions of the sky where it is not possible to make an estimate of their reliability.  
  
 
By definition, the reliability of the whole  PCCS2 is &ge; 80%, and a flag is available that allows the user to select a subsample of sources with a higher level of reliability (e.g., 90% or 95%).
 
By definition, the reliability of the whole  PCCS2 is &ge; 80%, and a flag is available that allows the user to select a subsample of sources with a higher level of reliability (e.g., 90% or 95%).
  
The nine Planck full-mission frequency channel maps are used as input to the source detection pipelines. They contain 48 months of data for LFI channels and 29 months of data for HFI channels. Therefore the flux densities of sources obtained from the full-mission maps are the average of at least 8 observations for LFI channels or at least 4 observations for HFI channels. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Tables 1 and 2.
+
The nine Planck full-mission frequency channel maps are used as input to the source detection pipelines. They contain 48 months of data for LFI channels and 29 months of data for HFI channels. Therefore the flux densities of sources obtained from the full-mission maps are the average of at least eight observations for LFI channels or at least four observations for HFI channels. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Tables 1 and 2.
  
Four different photometry methods have been used. For one of the methods, the native photometry from the Mexican hat wavelet detection algorithm, the analysis is performed on patches containing tangent plane projections of the map. For the other methods (aperture photometry, point spread function fitting, and Gaussian fitting), the analysis is performed directly on the full-sky maps.
+
Four different photometry methods have been used. For one of the methods (the native photometry from the Mexican-hat wavelet detection algorithm), the analysis is performed on patches containing tangent-plane projections of the map. For the other methods (aperture photometry, point spread function fitting, and Gaussian fitting), the analysis is performed directly on the full-sky maps.
  
<center>'''PCCS2 in Intensity'''</center>
+
<center><small>'''PCCS2 in intensity.'''</small></center>
  
[[File:COMB_30_143_857_PCCS2a.png|800px|thumb|center|Sky distribution of the PCCS2 intensity sources at three different channels: 30 GHz (red circles), 143 GHz (blue circles) and 857 GHz (green circles). The dimension of the circles is related to the brightness of the sources and the beam size of each channel.]]
+
[[File:COMB_30_143_857_PCCS2a.png|800px|thumb|center|Sky distribution of the PCCS2 intensity sources for three different channels: 30 GHz (red circles); 143 GHz (blue circles); and 857 GHz (green circles). The size of the circles is related to the brightness of the sources and the beam size of each channel.]]
  
<center>'''PCCS2E in Intensity'''</center>
+
<center><small>'''PCCS2E in intensity.'''</small></center>
  
[[File:COMB_30_143_857_PCCS2Ea.png|800px|thumb|center|Sky distribution of the PCCS2E intensity sources at three different channels: 143 GHz (blue circles) and 857 GHz (green circles).]]
+
[[File:COMB_30_143_857_PCCS2Ea.png|800px|thumb|center|Sky distribution of the PCCS2E intensity sources for two different channels: 143 GHz (blue circles); and 857 GHz (green circles).]]
  
 
The analysis in polarization has been performed in a non-blind fashion, looking at the position of the sources previously detected in intensity. As a result, polarization flux densities and polarization angles have been measured for hundreds of sources with a significance >99.99%. This high threshold in significance has been chosen to minimize the possibility of misinterpreting a peak of the polarized background as a source. This implies that, in general, most of the polarized sources are very bright, introducing an additional selection effect.
 
The analysis in polarization has been performed in a non-blind fashion, looking at the position of the sources previously detected in intensity. As a result, polarization flux densities and polarization angles have been measured for hundreds of sources with a significance >99.99%. This high threshold in significance has been chosen to minimize the possibility of misinterpreting a peak of the polarized background as a source. This implies that, in general, most of the polarized sources are very bright, introducing an additional selection effect.
  
<center>'''PCCS2 in Polarization'''</center>
+
<center><small>'''PCCS2 in polarization.'''</small></center>
  
[[File:PCCS_POL_30_44_70_v2a.png|800px|thumb|center|Sky distribution of the PCCS2 polarization sources at three different channels: 30GHz (red circles), 44GHz (green circles) and 70GHz (blue circles).]]
+
[[File:PCCS_POL_30_44_70_v2a.png|800px|thumb|center|Sky distribution of the PCCS2 polarization sources in three different channels: 30GHz (red circles); 44GHz (green circles); and 70GHz (blue circles).]]
  
[[File:PCCS_POL_100_143_217_353.png|800px|thumb|center|Sky distribution of the PCCS2 polarization sources at three different channels: 100GHz (red circles), 143GHz (blue circles) and 217GHz (green circles) and 353 GHz (black).]]
+
[[File:PCCS_POL_100_143_217_353.png|800px|thumb|center|Sky distribution of the PCCS2 polarization sources in four different channels: 100GHz (red circles); 143GHz (blue circles); 217GHz (green circles); and 353 GHz (black).]]
  
<center>'''PCCS2E in Polarization'''</center>
+
<center><small>'''PCCS2E in polarization.'''</small></center>
  
[[File:PCCS_POL_100_143_217_353_E.png|800px|thumb|center|Sky distribution of the PCCS2E polarization sources at three different channels: 100GHz (red circles), 143GHz (blue circles) and 217GHz (green circles) and 353 GHz (black).]]
+
[[File:PCCS_POL_100_143_217_353_E.png|800px|thumb|center|Sky distribution of the PCCS2E polarization sources at three different channels: 100GHz (red circles); 143GHz (blue circles); 217GHz (green circles); and 353 GHz (black).]]
  
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=750px
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=750px
|+ '''Table 1: PCCS2 and PCCS2E characteristics.'''
+
|+ <small>'''Table 1: PCCS2 and PCCS2E characteristics.'''</small>
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! Channel || 30 || 44 || 70 || 100 || 143 || 217 || 353 || 545 || 857
 
! Channel || 30 || 44 || 70 || 100 || 143 || 217 || 353 || 545 || 857
Line 43: Line 46:
 
|'''Wavelength [&mu;m]''' || 10561 || 6807 || 4260 || 3000 || 2098 || 1382 || 850 || 550 || 350
 
|'''Wavelength [&mu;m]''' || 10561 || 6807 || 4260 || 3000 || 2098 || 1382 || 850 || 550 || 350
 
|-
 
|-
!colspan="1" |Number of sources
+
!colspan="10" |Number of sources
 
|-
 
|-
 
| PCCS2  || 1560 || 934 || 1296 || 1742 || 2160 || 2135 || 1344 || 1694 || 4891
 
| PCCS2  || 1560 || 934 || 1296 || 1742 || 2160 || 2135 || 1344 || 1694 || 4891
Line 51: Line 54:
 
| Union PCCS2+PCCS2E  || &mdash; || &mdash; || &mdash; || 4229 || 6299 || 18977 || 24009 || 32762 || 48181
 
| Union PCCS2+PCCS2E  || &mdash; || &mdash; || &mdash; || 4229 || 6299 || 18977 || 24009 || 32762 || 48181
 
|-
 
|-
!colspan="10" |Number of sources in the extragalactic zone<sup>a</sup>.
+
!colspan="10" |Number of sources in the extragalactic zone<sup>a</sup>
 
|-
 
|-
 
| PCCS2  || 745 || 367 || 504 || 1742 || 2160 ||  2135 ||  1344 ||  1694 ||  4891
 
| PCCS2  || 745 || 367 || 504 || 1742 || 2160 ||  2135 ||  1344 ||  1694 ||  4891
Line 59: Line 62:
 
| Union PCCS2+PCSS2E || &mdash; || &mdash; || &mdash; || 1742 || 2160 ||  2161 ||  1633 ||  2533 ||  6988
 
| Union PCCS2+PCSS2E || &mdash; || &mdash; || &mdash; || 1742 || 2160 ||  2161 ||  1633 ||  2533 ||  6988
 
|-
 
|-
!colspan="10" |Flux densities [mJy] in the extragalactic zone<sup>a</sup> .
+
!colspan="10" |Flux densities [mJy] in the extragalactic zone<sup>a</sup>
 
|-
 
|-
 
!colspan="1" |PCCS2
 
!colspan="1" |PCCS2
 
|-
 
|-
| minimum<sup>b</sup> ||  376 ||  603 ||  444 ||  232 ||  147 ||  127 ||  242 ||  535 ||  720
+
| Minimum<sup>b</sup> ||  376 ||  603 ||  444 ||  232 ||  147 ||  127 ||  242 ||  535 ||  720
 
|-
 
|-
 
| 90% completeness ||  426 ||  676 ||  489 ||  269 ||  177 ||  152 ||  304 ||  555 ||  791
 
| 90% completeness ||  426 ||  676 ||  489 ||  269 ||  177 ||  152 ||  304 ||  555 ||  791
 
|-
 
|-
| uncertainty ||  87 ||  134 ||  101 ||  55 ||  35 ||    29 ||    55 ||  105 ||  168
+
| Uncertainty ||  87 ||  134 ||  101 ||  55 ||  35 ||    29 ||    55 ||  105 ||  168
 
|-
 
|-
 
!colspan="1" |PCCS2E
 
!colspan="1" |PCCS2E
 
|-
 
|-
| minimum<sup>b</sup> || &mdash; || &mdash; || &mdash; || &mdash;  || &mdash; ||  189 ||  350 ||  597 ||  939
+
| Minimum<sup>b</sup> || &mdash; || &mdash; || &mdash; || &mdash;  || &mdash; ||  189 ||  350 ||  597 ||  939
 
|-
 
|-
 
| 90% completeness ||  &mdash; ||  &mdash; || &mdash; || &mdash; || &mdash; ||  144 ||  311 ||  557 ||  927
 
| 90% completeness ||  &mdash; ||  &mdash; || &mdash; || &mdash; || &mdash; ||  144 ||  311 ||  557 ||  927
 
|-
 
|-
| uncertainty || &mdash; ||  &mdash; ||  &mdash; || &mdash; || &mdash; ||    35 ||    73 ||  144 ||  278
+
| Uncertainty || &mdash; ||  &mdash; ||  &mdash; || &mdash; || &mdash; ||    35 ||    73 ||  144 ||  278
 
|-
 
|-
 
|}
 
|}
 
'''Table 1 Notes'''
 
'''Table 1 Notes'''
 
+
'''<sup>a</sup>''' 30-70 GHz: the extragalactic zone is defined by |b| > 30&deg;. For 100-857 GHz the numbers outside of the Galactic region where the reliability cannot be accurately assessed. Note that for the PCCS2E the only sources that occur in this region lie in the filament mask.<BR>
'''a''' 30-70 GHz: the extragalactic zone is given by |b| > 30&deg;. 100-857 GHz: outside of galactic region where the reliability cannot be accurately assessed. Note that for the PCCS2E the only sources which occur in this region lie in the filament mask.
+
'''<sup>b</sup>''' Minimum flux density of the catalogue in the extragalactic zone after excluding the faintest 10% of sources.
 
 
'''b''' Minimum flux density of the catalogue in the extragalactic zone after excluding the faintest 10% of sources.
 
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=750px
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=750px
|+ '''Table 2: PCCS2 & PCCS2E polarization characteristics for sources with polarized emission significance > 99.99%'''
+
|+ <small>'''Table 2: PCCS2 & PCCS2E polarization characteristics for sources with polarized emission significance > 99.99%'''</small>
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
!Channel  ||  30  ||  44  ||  70  ||  100  ||  143  ||  217  ||  353
 
!Channel  ||  30  ||  44  ||  70  ||  100  ||  143  ||  217  ||  353
Line 95: Line 96:
 
|Polarized flux density uncertainty [mJy]  ||  46  ||  88  ||  91  ||  30  ||  26  ||  30  ||  81
 
|Polarized flux density uncertainty [mJy]  ||  46  ||  88  ||  91  ||  30  ||  26  ||  30  ||  81
 
|-
 
|-
|Minimum polarized flux density completeness 90% [mJy]  ||  199  ||  412  ||  397  ||  135  ||  100  ||  136  ||  347
+
|Minimum polarized flux density for 90% completeness [mJy]  ||  199  ||  412  ||  397  ||  135  ||  100  ||  136  ||  347
 
|-
 
|-
|Minimum polarized flux density completeness 95% [mJy]  ||  251  ||  468  ||  454  ||  160  ||  111  ||  153  ||  399
+
|Minimum polarized flux density for 95% completeness [mJy]  ||  251  ||  468  ||  454  ||  160  ||  111  ||  153  ||  399
 
|-
 
|-
|Minimum polarized flux density completeness 100% [mJy]  ||  600  ||  700  ||  700  ||  250  ||  147  ||  257  ||  426
+
|Minimum polarized flux density for 100% completeness [mJy]  ||  600  ||  700  ||  700  ||  250  ||  147  ||  257  ||  426
 
|-
 
|-
|
+
-
 
|-
 
|-
 
|Number of significantly polarized sources in PCCS2E  ||  &mdash;  || &mdash;  || &mdash;  ||  43  ||  111  ||  325  ||  666
 
|Number of significantly polarized sources in PCCS2E  ||  &mdash;  || &mdash;  || &mdash;  ||  43  ||  111  ||  325  ||  666
Line 109: Line 110:
 
|Polarized flux density uncertainty [mJy]  || &mdash;  ||  &mdash; || &mdash; ||  52  ||  44  ||  55  ||  178
 
|Polarized flux density uncertainty [mJy]  || &mdash;  ||  &mdash; || &mdash; ||  52  ||  44  ||  55  ||  178
 
|-
 
|-
|Minimum polarized flux density completeness 90% [mJy]  ||  &mdash;  ||  &mdash;  ||  &mdash;  ||  410  ||  613  ||  270  ||  567
+
|Minimum polarized flux density for 90% completeness [mJy]  ||  &mdash;  ||  &mdash;  ||  &mdash;  ||  410  ||  613  ||  270  ||  567
 
|-
 
|-
|Minimum polarized flux density completeness 95% [mJy]  ||  &mdash;  ||  &mdash;  ||  &mdash;  ||  599  ||  893  ||  464  ||  590
+
|Minimum polarized flux density for 95% completeness [mJy]  ||  &mdash;  ||  &mdash;  ||  &mdash;  ||  599  ||  893  ||  464  ||  590
 
|-
 
|-
|Minimum polarized flux density completeness 100% [mJy]  || &mdash;  || &mdash;  ||  &mdash;  ||  835  ||  893  ||  786  ||  958
+
|Minimum polarized flux density for 100% completeness [mJy]  || &mdash;  || &mdash;  ||  &mdash;  ||  835  ||  893  ||  786  ||  958
 
|-
 
|-
 
|}
 
|}
 
'''Table 2 Notes'''
 
'''Table 2 Notes'''
  
'''a''' Minimum polarized flux density of the catalogue of significantly polarised sources after excluding the faintest 10% of sources.
+
'''<sup>a</sup>''' Minimum polarized flux density of the catalogue of significantly polarized sources after excluding the faintest 10% of sources.
  
=== Catalogues ===
+
==== Catalogues ====
  
The PCCS2 catalogues are contained in the FITS files:
+
The PCCS2 catalogues (at each frequency) are contained in the FITS files
  
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_030_R2.04.fits|link=COM_PCCS_030_R2.04.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_030_R2.04.fits|link=COM_PCCS_030_R2.04.fits}}
Line 132: Line 133:
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353_R2.01.fits|link=COM_PCCS_353_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353_R2.01.fits|link=COM_PCCS_353_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545_R2.01.fits|link=COM_PCCS_545_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545_R2.01.fits|link=COM_PCCS_545_R2.01.fits}}
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857_R2.01.fits|link=COM_PCCS_857_R2.01.fits}}
+
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857_R2.01.fits|link=COM_PCCS_857_R2.01.fits}} .
  
and the PCCS2E catalogues are contained in the FITS files:
+
The PCCS2E catalogues are contained in the FITS files
  
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-excluded_R2.01.fits|link=COM_PCCS_100-excluded_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-excluded_R2.01.fits|link=COM_PCCS_100-excluded_R2.01.fits}}
Line 143: Line 144:
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-excluded_R2.01.fits|link=COM_PCCS_857-excluded_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-excluded_R2.01.fits|link=COM_PCCS_857-excluded_R2.01.fits}}
  
The structure of these files is as follows:
+
The structure of these files is as follows.
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
|+ '''PCCS2/PCCS2E FITS file structure'''
+
|+ <small>'''PCCS2/PCCS2E FITS file structure'''</small>
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
!colspan="4" | Extension 0: Primary header, no data
 
!colspan="4" | Extension 0: Primary header, no data
 
|- bgcolor="ffdead"
 
|- bgcolor="ffdead"
! FITS Keyword || Data Type || Units || Description
+
! FITS keyword || Data type || Units || Description
 
|-
 
|-
 
|INSTRUME || String || || Instrument (LFI / HFI)
 
|INSTRUME || String || || Instrument (LFI / HFI)
Line 162: Line 163:
 
| TELESCOP || String || || Telescope (PLANCK)
 
| TELESCOP || String || || Telescope (PLANCK)
 
|-
 
|-
| CREATOR || String || || Pipeline Version
+
| CREATOR || String || || Pipeline version
 
|-
 
|-
 
| DATE-OBS || String || days || Beginning of the survey: yyyy-mm-dd
 
| DATE-OBS || String || days || Beginning of the survey: yyyy-mm-dd
Line 180: Line 181:
 
!colspan="4" | Extension 1:  BINTABLE, EXTNAME = PCCS2_''fff'' (where ''fff'' is the frequency channel)
 
!colspan="4" | Extension 1:  BINTABLE, EXTNAME = PCCS2_''fff'' (where ''fff'' is the frequency channel)
 
|-bgcolor="ffdead"
 
|-bgcolor="ffdead"
! Column Name || Data Type || Units || Description
+
! Column Name || Data type || Units || Description
 
|-bgcolor="ffdead"
 
|-bgcolor="ffdead"
 
!colspan="4"|Identification
 
!colspan="4"|Identification
Line 188: Line 189:
 
!colspan="4"|Source position
 
!colspan="4"|Source position
 
|-
 
|-
|GLON || Real*8 || degrees || Galactic longitude based on extraction algorithm
+
|GLON || Real*8 || deg || Galactic longitude based on extraction algorithm
 
|-
 
|-
|GLAT || Real*8 || degrees || Galactic latitude based on extraction algorithm
+
|GLAT || Real*8 || deg || Galactic latitude based on extraction algorithm
 
|-
 
|-
|RA  || Real*8 || degrees || Right ascension (J2000) transformed from (GLON,GLAT)
+
|RA  || Real*8 || deg || Right ascension (J2000) transformed from (GLON,GLAT)
 
|-
 
|-
|DEC  || Real*8 || degrees || Declination (J2000) transformed from (GLON,GLAT)
+
|DEC  || Real*8 || deg || Declination (J2000) transformed from (GLON,GLAT)
 
|-bgcolor="ffdead"
 
|-bgcolor="ffdead"
 
!colspan="4"|Photometry
 
!colspan="4"|Photometry
Line 200: Line 201:
 
|DETFLUX || Real*4 || mJy || Flux density of source as determined by detection method
 
|DETFLUX || Real*4 || mJy || Flux density of source as determined by detection method
 
|-
 
|-
|DETFLUX_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived flux density from detection method
+
|DETFLUX_ERR || Real*4 || mJy || Uncertainty (1 &sigma;) in derived flux density from detection method
 
|-
 
|-
|APERFLUX || Real*4 || mJy || Flux density of source as determined from the aperture photometry
+
|APERFLUX || Real*4 || mJy || Flux density of source as determined from aperture photometry
 
|-
 
|-
|APERFLUX_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived flux density from the aperture photometry
+
|APERFLUX_ERR || Real*4 || mJy || Uncertainty (1 &sigma;) in derived flux density from aperture photometry
 
|-
 
|-
 
|PSFFLUX || Real*4 || mJy || Flux density of source as determined from PSF fitting
 
|PSFFLUX || Real*4 || mJy || Flux density of source as determined from PSF fitting
 
|-
 
|-
|PSFFLUX_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived flux density from PSF fitting
+
|PSFFLUX_ERR || Real*4 || mJy || Uncertainty (1 &sigma;) in derived flux density from PSF fitting
 
|-
 
|-
 
|GAUFLUX || Real*4 || mJy || Flux density of source as determined from 2-D Gaussian fitting
 
|GAUFLUX || Real*4 || mJy || Flux density of source as determined from 2-D Gaussian fitting
 
|-
 
|-
|GAUFLUX_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived flux density from 2-D Gaussian fitting
+
|GAUFLUX_ERR || Real*4 || mJy || Uncertainty (1 &sigma;) in derived flux density from 2-D Gaussian fitting
 
|-
 
|-
 
|GAU_SEMI1 || Real*4 || arcmin || Gaussian fit along axis 1 (FWHM; see note 2 for axis definition)
 
|GAU_SEMI1 || Real*4 || arcmin || Gaussian fit along axis 1 (FWHM; see note 2 for axis definition)
 
|-
 
|-
|GAU_SEMI1_ERR || Real*4 || arcmin || Uncertainty (1 sigma) in derived Gaussian fit along axis 1
+
|GAU_SEMI1_ERR || Real*4 || arcmin || Uncertainty (1 &sigma;) in derived Gaussian fit along axis 1
 
|-
 
|-
 
|GAU_SEMI2 || Real*4 || arcmin || Gaussian fit along axis 2 (FWHM)
 
|GAU_SEMI2 || Real*4 || arcmin || Gaussian fit along axis 2 (FWHM)
 
|-
 
|-
|GAU_SEMI2_ERR || Real*4 || arcmin || Uncertainty (1 sigma) in derived Gaussian fit along axis 2
+
|GAU_SEMI2_ERR || Real*4 || arcmin || Uncertainty (1 &sigma;) in derived Gaussian fit along axis 2
 
|-
 
|-
 
|GAU_THETA || Real*4 || deg || Gaussian fit orientation angle (see note 2)
 
|GAU_THETA || Real*4 || deg || Gaussian fit orientation angle (see note 2)
 
|-
 
|-
|GAU_THETA_ERR || Real*4 || deg || Uncertainty (1 sigma) in derived gaussian fit orientation angle
+
|GAU_THETA_ERR || Real*4 || deg || Uncertainty (1 &sigma;) in derived Gaussian fit orientation angle
 
|-
 
|-
 
|GAU_FWHM_EFF || Real*4 || arcmin || Gaussian fit effective FWHM
 
|GAU_FWHM_EFF || Real*4 || arcmin || Gaussian fit effective FWHM
Line 232: Line 233:
 
|P || Real*4 || mJy || Polarization flux density of the sources as determined by a matched filter (see note 3)
 
|P || Real*4 || mJy || Polarization flux density of the sources as determined by a matched filter (see note 3)
 
|-
 
|-
|P_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived polarization flux density (see note 3)
+
|P_ERR || Real*4 || mJy || Uncertainty (1 &sigma;) in derived polarization flux density (see note 3)
 
|-
 
|-
 
|ANGLE_P || Real*4 || degrees || Orientation of polarization with respect to NGP (see notes 2 and 3)
 
|ANGLE_P || Real*4 || degrees || Orientation of polarization with respect to NGP (see notes 2 and 3)
 
|-
 
|-
|ANGLE_P_ERR || Real*4 || degrees || Uncertainty (1 sigma) in orientation of polarization (see note 3)
+
|ANGLE_P_ERR || Real*4 || degrees || Uncertainty (1 &sigma;) in orientation of polarization (see note 3)
 
|-
 
|-
 
|APER_P || Real*4 || mJy || Polarization flux density of the sources as determined by aperture photometry (see note 3)
 
|APER_P || Real*4 || mJy || Polarization flux density of the sources as determined by aperture photometry (see note 3)
 
|-
 
|-
|APER_P_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived polarization flux density (see note 3)
+
|APER_P_ERR || Real*4 || mJy || Uncertainty (1 &sigma;) in derived polarization flux density (see note 3)
 
|-
 
|-
 
|APER_ANGLE_P || Real*4 || degrees || Orientation of polarization with respect to NGP (see notes 2 and 3)
 
|APER_ANGLE_P || Real*4 || degrees || Orientation of polarization with respect to NGP (see notes 2 and 3)
 
|-
 
|-
|APER_ANGLE_P_ERR || Real*4 || degrees || Uncertainty (1 sigma) in orientation of polarization (see note 3)
+
|APER_ANGLE_P_ERR || Real*4 || degrees || Uncertainty (1 &sigma;) in orientation of polarization (see note 3)
 
|-
 
|-
|P_UPPER_LIMIT || Real*4 || mJy || Polarization flux density 99.99% upper limit. This is provided only when P column is set to NULL; otherwise this column itself contains a NULL.
+
|P_UPPER_LIMIT || Real*4 || mJy || Polarization flux density 99.99% upper limit. This is provided only when the P column is set to NULL; otherwise this column itself contains NULL.
 
|-
 
|-
|APER_P_UPPER_LIMIT || Real*4 || mJy || Polarization flux density 99.99% upper limit. This is provided only when APER_P column is set to NULL; otherwise this column itself contains a NULL.
+
|APER_P_UPPER_LIMIT || Real*4 || mJy || Polarization flux density 99.99% upper limit. This is provided only when the APER_P column is set to NULL; otherwise this column itself contains NULL.
 
|-bgcolor="ffdead"
 
|-bgcolor="ffdead"
 
!colspan="4"|Marginal polarization measurements (100-353 GHz only) &ndash; see note 4
 
!colspan="4"|Marginal polarization measurements (100-353 GHz only) &ndash; see note 4
Line 254: Line 255:
 
|P_STAT || Integer*2 ||  || Polarization detection status
 
|P_STAT || Integer*2 ||  || Polarization detection status
 
|-
 
|-
|PX || Real*4|| mJy || Polarization flux density of the sources as determined by a matched filter using Bayesian polarization estimator.
+
|PX || Real*4|| mJy || Polarization flux density of the sources as determined by a matched filter using a Bayesian polarization estimator
 
|-
 
|-
 
|PX_ERR_LOWER || Real*4|| mJy || PX uncertainty; lower 95% error bar
 
|PX_ERR_LOWER || Real*4|| mJy || PX uncertainty; lower 95% error bar
Line 260: Line 261:
 
|PX_ERR_UPPER || Real*4|| mJy || PX uncertainty; upper 95% error bar
 
|PX_ERR_UPPER || Real*4|| mJy || PX uncertainty; upper 95% error bar
 
|-
 
|-
|ANGLE_PX || Real*4|| degrees || Orientation of polarization with respect to NGP using Bayesian polarization estimator (see note 2)
+
|ANGLE_PX || Real*4|| deg || Orientation of polarization with respect to NGP using Bayesian polarization estimator (see note 2)
 
|-
 
|-
|ANGLE_PX_ERR_LOWER || Real*4|| degrees || ANGLE_PX uncertainty; lower 95% error bar
+
|ANGLE_PX_ERR_LOWER || Real*4|| deg || ANGLE_PX uncertainty; lower 95% error bar
 
|-
 
|-
|ANGLE_PX_ERR_UPPER || Real*4|| degrees || ANGLE_PX uncertainty; upper 95% error bar
+
|ANGLE_PX_ERR_UPPER || Real*4|| deg || ANGLE_PX uncertainty; upper 95% error bar
 
|-bgcolor="ffdead"
 
|-bgcolor="ffdead"
 
!colspan="4"|Flags and validation
 
!colspan="4"|Flags and validation
Line 280: Line 281:
 
|HIGHEST_RELIABILITY_CAT || Integer*4 || || See note 7
 
|HIGHEST_RELIABILITY_CAT || Integer*4 || || See note 7
 
|-bgcolor="ffdead"
 
|-bgcolor="ffdead"
!colspan="4"|Flags and validation (PCCS2E 100-857 GHz only)
+
!colspan="4"|Flags and validation (PCCS2E, 100-857 GHz only)
 
|-
 
|-
 
|WHICH_ZONE || Integer*2 || || See note 8
 
|WHICH_ZONE || Integer*2 || || See note 8
Line 286: Line 287:
 
!colspan="4"|Flags and validation (217-857 GHz only)
 
!colspan="4"|Flags and validation (217-857 GHz only)
 
|-
 
|-
|CIRRUS_N || Integer*2 || || Number of sources (S/N > 5) detected at 857 GHz within a 1-degree radius.
+
|CIRRUS_N || Integer*2 || || Number of sources (S/N > 5) detected at 857 GHz within a 1&deg; radius.
 
|-
 
|-
|SKY_BRIGHTNESS || Real*4 || MJy/sr || The mean 857 GHz brightness within a 2-degree radius. This may be used as another indicator of cirrus contamination.
+
|SKY_BRIGHTNESS || Real*4 || MJy sr<sup>-1</sup> || The mean 857 GHz brightness within a 2&deg; radius. This may be used as another indicator of cirrus contamination.
 
|-bgcolor="ffdead"
 
|-bgcolor="ffdead"
 
!colspan="4"| Flux densities at other frequencies (857 GHz only)
 
!colspan="4"| Flux densities at other frequencies (857 GHz only)
Line 306: Line 307:
  
 
'''Notes'''
 
'''Notes'''
# Format is <tt>PCCS2 fff Glll.ll&plusmn;bb.bb</tt> for sources in the PCCS2 and <tt>PCCS2E fff Glll.ll&plusmn;bb.bb</tt> for sources in the PCCS2E, where fff is the frequency channel and (l, b) is the position of the source in Galactic coordinates truncated to two decimal places.
+
# Format is <tt>PCCS2 fff Glll.ll&plusmn;bb.bb</tt> for sources in the PCCS2 and <tt>PCCS2E fff Glll.ll&plusmn;bb.bb</tt> for sources in the PCCS2E, where "fff" is the frequency channel and l and b the position of the source in Galactic coordinates truncated to two decimal places.
# We follow the IAU/IEEE convention (Hamaker & Bregman 1996) for defining the angle of polarization of a source, and this convention is also used for the other angles in the catalogue. The angle is measured from the North Galactic Pole in a clockwise direction from -90 to 90 degrees.
+
# We follow the IAU/IEEE convention (Hamaker & Bregman 1996) for defining the angle of polarization of a source in this catalogue, and this convention is also used for the other angles in the catalogue. The angle is measured from the North Galactic Pole in a clockwise direction from -90&deg; to 90&deg;.  Note that this is different than the convention used for the CMB maps.
 
# Provided when the significance of the polarization measurement is > 99.99% and set to NULL otherwise.
 
# Provided when the significance of the polarization measurement is > 99.99% and set to NULL otherwise.
# The P_STAT flag gives the status of the marginal polarization detection, possible values are:
+
# The P_STAT flag gives the status of the marginal polarization detection. Possible values are:
#: 3 &ndash; Bright: P field filled in; all PX fields set to NULL.
+
#: 3 &ndash; bright, the P field filled in and all PX fields set to NULL;
#: 2 &ndash; Significant: P field is set to NULL; 0 is outside the PX 95% HPD; all PX fields are filled.
+
#: 2 &ndash; significant, the P field is set to NULL, 0 is outside the PX 95% HPD, and all PX fields are filled;
#: 1 &ndash; Marginal: P field is set to NULL; 0 is inside the PX 95% HPD, but mode of PX posterior distribution is not 0; all PX fields are filled.
+
#: 1 &ndash; marginal, the P field is set to NULL, 0 is inside the PX 95% HPD (but the mode of the PX posterior distribution is not 0) and all PX fields are filled;
#: 0 &ndash; No detection: P field is set to NULL; mode of PX posterior distribution is 0; PX_ERRL, ANGLE_PX, ANGLE_PX_ERR_LOWER, and ANGLE_PX_ERR_UPPER are set to NULL.
+
#: 0 &ndash; no detection, the P field is set to NULL, the mode of the PX posterior distribution is 0, PX_ERRL, ANGLE_PX, ANGLE_PX_ERR_LOWER, and ANGLE_PX_ERR_UPPER are set to NULL.
# The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criterion for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
+
# The EXTENDED flag has the value of "0" if the source is compact and the value of "1" if it is extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criterion for extension being &radic;(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
# The EXT_VAL flag gives the status of the external validation, possible values are:
+
# The EXT_VAL flag gives the status of the external validation. Possible values are:
#: 3 &ndash; The source has a clear counterpart in one of the catalogues used as ancillary data.
+
#: 3 &ndash; the source has a clear counterpart in one of the catalogues used as ancillary data;
#: 2 &ndash; The source does not have a clear counterpart in one of the catalogues used as ancillary data but it has been detected by the internal multi-frequency method.
+
#: 2 &ndash; the source does not have a clear counterpart in one of the catalogues used as ancillary data, but it has been detected by the internal multi-frequency method;
#: 1 &ndash; The source does not have a clear counterpart in one of the catalogues used as ancillary data and it has not been detected by the internal multi-frequency method, but it has been detected in a previous Planck source catalogue.
+
#: 1 &ndash; the source does not have a clear counterpart in one of the catalogues used as ancillary data and it has not been detected by the internal multi-frequency method, but it has been detected in a previous Planck source catalogue;
#: 0 &ndash; The source does not have a clear counterpart in one of the catalogues used as ancillary data and it has not been detected by the internal multi-frequency method.
+
#: 0 &ndash; the source does not have a clear counterpart in one of the catalogues used as ancillary data and has not been detected by the internal multi-frequency method.
# The HIGHEST_RELIABILTY_CAT column contains the highest reliability catalogue to which the source belongs. As the full catalogue reliability is &ge; 80%, this is the lowest possible value in this column. Where possible this is provided in steps of 1% otherwise it is in steps of 5%.
+
# The HIGHEST_RELIABILTY_CAT column contains the highest reliability catalogue to which the source belongs. As the full catalogue reliability is &ge; 80%, this is the lowest possible value in this column. Where possible this is provided in steps of 1%, otherwise it is in steps of 5%.
 
# The WHICH_ZONE column encodes the zone in which the source lies:
 
# The WHICH_ZONE column encodes the zone in which the source lies:
#: 1 &ndash; source lies inside filament mask.
+
#: 1 &ndash; source lies inside the filament mask;
#: 2 &ndash; source lies inside Galactic zone.
+
#: 2 &ndash; source lies inside the Galactic zone;
#: 3 &ndash; sources lies in both filament mask and Galactic zone.
+
#: 3 &ndash; sources lies in both the filament mask and Galactic zone.
  
=== Zone map ===
+
==== Zone map ====
  
For each HFI frequency channel there is an associated map which defines the quantified-reliability (PCCS2) and unquantified-reliability (PCCS2E) zones are on the sky.
+
For each HFI frequency channel there is an associated map that defines where the quantified-reliability (PCCS2) and unquantified-reliability (PCCS2E) zones are on the sky.
  
The files are called:
+
The files are called
  
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-zoneMask_R2.01.fits|link=COM_PCCS_100-zoneMask_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-zoneMask_R2.01.fits|link=COM_PCCS_100-zoneMask_R2.01.fits}}
Line 337: Line 338:
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-zoneMask_R2.01.fits|link=COM_PCCS_353-zoneMask_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-zoneMask_R2.01.fits|link=COM_PCCS_353-zoneMask_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-zoneMask_R2.01.fits|link=COM_PCCS_545-zoneMask_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-zoneMask_R2.01.fits|link=COM_PCCS_545-zoneMask_R2.01.fits}}
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-zoneMask_R2.01.fits|link=COM_PCCS_857-zoneMask_R2.01.fits}}
+
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-zoneMask_R2.01.fits|link=COM_PCCS_857-zoneMask_R2.01.fits}} .
  
The structure of the files is as follows:
+
The structure of the files is shown in the following table.
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
|+ '''Zone map FITS file structure'''
+
|+ <small>'''Zone map FITS file structure'''</small>
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
!colspan="4" | Extension 0: Primary header, no data
 
!colspan="4" | Extension 0: Primary header, no data
 
|- bgcolor="ffdead"
 
|- bgcolor="ffdead"
! FITS Keyword || Data Type || Units || Description
+
! FITS keyword || Data type || Units || Description
 
|-
 
|-
 
|DATE || String ||  || Date of creation of file
 
|DATE || String ||  || Date of creation of file
Line 352: Line 353:
 
! colspan="4" | Extension 1: BINTABLE, HEALPix map (see note 1)
 
! colspan="4" | Extension 1: BINTABLE, HEALPix map (see note 1)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS keyword || Data Type || Value || Description
+
! FITS keyword || Data type || Value || Description
 
|-
 
|-
 
|PIXTYPE || String || HEALPIX || HEALPix pixelation
 
|PIXTYPE || String || HEALPIX || HEALPix pixelation
Line 368: Line 369:
  
 
'''Notes'''
 
'''Notes'''
# This FITS extension contains an integer HEALPix map which encodes the information on which of 4 possible regions on the sky each pixel belongs to:
+
# This FITS extension contains an integer HEALPix map, which encodes the information on which of four possible regions on the sky each pixel belongs to:
#: 0 &ndash; quantified-reliability zone (PCCS2).
+
#: 0 &ndash; quantified-reliability zone (PCCS2);
#: 1 &ndash; filament mask.
+
#: 1 &ndash; filament mask;
#: 2 &ndash; Galactic zone.
+
#: 2 &ndash; Galactic zone;
 
#: 3 &ndash; filament mask and Galactic zone.
 
#: 3 &ndash; filament mask and Galactic zone.
  
=== S/N threshold map ===
+
==== S/N threshold map ====
  
For each HFI frequency channel there are a number of maps which contains the S/N threshold used to accept sources into the PCCS2 and PCCS2E catalogues.
+
For each HFI frequency channel there are a number of maps that contains the S/N threshold used to accept sources into the PCCS2 and PCCS2E catalogues.
  
For the full catalogue (80% reliability in the quantified reliability zone) they are:
+
For the full catalogue (80% reliability in the quantified reliability zone) they are
  
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-SN-threshold_R2.01.fits|link=COM_PCCS_100-SN-threshold_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-SN-threshold_R2.01.fits|link=COM_PCCS_100-SN-threshold_R2.01.fits}}
Line 385: Line 386:
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-SN-threshold_R2.01.fits|link=COM_PCCS_353-SN-threshold_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-SN-threshold_R2.01.fits|link=COM_PCCS_353-SN-threshold_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-SN-threshold_R2.01.fits|link=COM_PCCS_545-SN-threshold_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-SN-threshold_R2.01.fits|link=COM_PCCS_545-SN-threshold_R2.01.fits}}
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-SN-threshold_R2.01.fits|link=COM_PCCS_857-SN-threshold_R2.01.fits}}
+
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-SN-threshold_R2.01.fits|link=COM_PCCS_857-SN-threshold_R2.01.fits}} .
  
For 85% reliability they are:
+
For 85% reliability they are
  
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_100-SN-threshold-85pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_100-SN-threshold-85pc-reliability_R2.01.fits}}
Line 394: Line 395:
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_353-SN-threshold-85pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_353-SN-threshold-85pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_545-SN-threshold-85pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_545-SN-threshold-85pc-reliability_R2.01.fits}}
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_857-SN-threshold-85pc-reliability_R2.01.fits}}
+
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_857-SN-threshold-85pc-reliability_R2.01.fits}} .
  
For 90% reliability they are:
+
For 90% reliability they are
  
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_100-SN-threshold-90pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_100-SN-threshold-90pc-reliability_R2.01.fits}}
Line 403: Line 404:
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_353-SN-threshold-90pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_353-SN-threshold-90pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_545-SN-threshold-90pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_545-SN-threshold-90pc-reliability_R2.01.fits}}
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_857-SN-threshold-90pc-reliability_R2.01.fits}}
+
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_857-SN-threshold-90pc-reliability_R2.01.fits}} .
  
For 95% reliability they are:
+
For 95% reliability they are
  
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_100-SN-threshold-95pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_100-SN-threshold-95pc-reliability_R2.01.fits}}
Line 412: Line 413:
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_353-SN-threshold-95pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_353-SN-threshold-95pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_545-SN-threshold-95pc-reliability_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_545-SN-threshold-95pc-reliability_R2.01.fits}}
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_857-SN-threshold-95pc-reliability_R2.01.fits}}
+
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_857-SN-threshold-95pc-reliability_R2.01.fits}} .
  
The structure of the files is as follows:
+
The structure of the files is shown in the following table.
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
|+ '''Zone map FITS file structure'''
+
|+ <small>'''Zone map FITS file structure'''</small>
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
!colspan="4" | Extension 0: Primary header, no data
 
!colspan="4" | Extension 0: Primary header, no data
 
|- bgcolor="ffdead"
 
|- bgcolor="ffdead"
! FITS Keyword || Data Type || Units || Description
+
! FITS keyword || Data type || Units || Description
 
|-
 
|-
 
|DATE || String ||  || Date of creation of file
 
|DATE || String ||  || Date of creation of file
Line 427: Line 428:
 
! colspan="4" | Extension 1: BINTABLE, HEALPix map (see note 1)
 
! colspan="4" | Extension 1: BINTABLE, HEALPix map (see note 1)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS keyword || Data Type || Value || Description
+
! FITS keyword || Data type || Value || Description
 
|-
 
|-
 
|PIXTYPE || String || HEALPIX || HEALPix pixelation
 
|PIXTYPE || String || HEALPIX || HEALPix pixelation
Line 445: Line 446:
 
# This FITS extension contains a single precision HEALPix map of the S/N threshold applied in the generation of the catalogue at that position on the sky.
 
# This FITS extension contains a single precision HEALPix map of the S/N threshold applied in the generation of the catalogue at that position on the sky.
  
===Noise map===
+
====Noise map====
  
For each HFI frequency channel there is an associated map which contains the detection noise as a function of position on the sky.
+
For each HFI frequency channel there is an associated map that contains the detection noise as a function of position on the sky.
  
The files are called:
+
The files are called
  
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-noise-level_R2.01.fits|link=COM_PCCS_100-noise-level_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100-noise-level_R2.01.fits|link=COM_PCCS_100-noise-level_R2.01.fits}}
Line 456: Line 457:
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-noise-level_R2.01.fits|link=COM_PCCS_353-noise-level_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-noise-level_R2.01.fits|link=COM_PCCS_353-noise-level_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-noise-level_R2.01.fits|link=COM_PCCS_545-noise-level_R2.01.fits}}
 
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-noise-level_R2.01.fits|link=COM_PCCS_545-noise-level_R2.01.fits}}
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-noise-level_R2.01.fits|link=COM_PCCS_857-noise-level_R2.01.fits}}
+
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857-noise-level_R2.01.fits|link=COM_PCCS_857-noise-level_R2.01.fits}} .
  
The structure of the files is as follows:
+
The structure of the files shown in the following table.
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
 
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
|+ '''Zone map FITS file structure'''
+
|+ <small>'''Zone map FITS file structure'''</small>
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
!colspan="4" | Extension 0: Primary header, no data
 
!colspan="4" | Extension 0: Primary header, no data
 
|- bgcolor="ffdead"
 
|- bgcolor="ffdead"
! FITS Keyword || Data Type || Units || Description
+
! FITS keyword || Data type || Units || Description
 
|-
 
|-
 
|DATE || String ||  || Date of creation of file
 
|DATE || String ||  || Date of creation of file
Line 471: Line 472:
 
! colspan="4" | Extension 1: BINTABLE, HEALPix map (see note 1)
 
! colspan="4" | Extension 1: BINTABLE, HEALPix map (see note 1)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS keyword || Data Type || Value || Description
+
! FITS keyword || Data type || Value || Description
 
|-
 
|-
 
|PIXTYPE || String || HEALPIX || HEALPix pixelation
 
|PIXTYPE || String || HEALPIX || HEALPix pixelation
Line 489: Line 490:
  
  
<div class="toccolours mw-collapsible mw-collapsed" style="width:800px">
+
==== Previous releases: (2013) PCCS and (2011) ERCSC ====
 +
<hr>
 +
<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #EEE8AA;width:95%">
 
'''Second Planck Release (2013): Description of the PCCS'''
 
'''Second Planck Release (2013): Description of the PCCS'''
 
<div class="mw-collapsible-content">
 
<div class="mw-collapsible-content">
Line 513: Line 516:
 
| '''Beam FWHM<span style="color:red"><sup>1</sup></span> [arcmin]''' || 32.38 || 27.10 || 13.30 || 9.88 || 7.18 || 4.87 || 4.65 || 4.72 || 4.39
 
| '''Beam FWHM<span style="color:red"><sup>1</sup></span> [arcmin]''' || 32.38 || 27.10 || 13.30 || 9.88 || 7.18 || 4.87 || 4.65 || 4.72 || 4.39
 
|-
 
|-
|'''SNR threshold''' || 4.0 || 4.0 || 4.0 || 4.6 || 4.7 || 4.8 || 4.9<span style="color:red"><sup>2</sup></span>/6.0<span style="color:red"><sup>3</sup></span> || 4.7/7.0 || 4.9/7.0
+
|'''S/N threshold''' || 4.0 || 4.0 || 4.0 || 4.6 || 4.7 || 4.8 || 4.9<span style="color:red"><sup>2</sup></span>/6.0<span style="color:red"><sup>3</sup></span> || 4.7/7.0 || 4.9/7.0
 
|-
 
|-
 
| '''# of detections''' || 1256 || 731 || 939 || 3850 || 5675 || 16070 || 17689 || 26472 || 35719  
 
| '''# of detections''' || 1256 || 731 || 939 || 3850 || 5675 || 16070 || 17689 || 26472 || 35719  
Line 580: Line 583:
 
!colspan="4" | Extension 0: Primary header, no data
 
!colspan="4" | Extension 0: Primary header, no data
 
|- bgcolor="ffdead"  
 
|- bgcolor="ffdead"  
! FITS Keyword || Data Type || Units || Description
+
! FITS keyword || Data type || Units || Description
 
|-  
 
|-  
 
|INSTRUME || String || || LFI or HFI
 
|INSTRUME || String || || LFI or HFI
Line 600: Line 603:
 
!colspan="4" | Extension 1:  (BINTABLE)
 
!colspan="4" | Extension 1:  (BINTABLE)
 
|-bgcolor="ffdead"  
 
|-bgcolor="ffdead"  
! Column Name || Data Type || Units || Description
+
! Column Name || Data type || Units || Description
 
|-bgcolor="ffdead"  
 
|-bgcolor="ffdead"  
 
!colspan="4"|Identification
 
!colspan="4"|Identification
 
|-
 
|-
|NAME || String || || Source name (Note 1)
+
|NAME || String || || Source name (note 1)
 
|-bgcolor="ffdead"  
 
|-bgcolor="ffdead"  
 
!colspan="4"|Source Position
 
!colspan="4"|Source Position
Line 634: Line 637:
 
|GAUFLUX_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived flux density from 2-D Gaussian fitting
 
|GAUFLUX_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived flux density from 2-D Gaussian fitting
 
|-
 
|-
|GAU_SEMI1 || Real*4 || arcmin || Gaussian fit along axis 1 (FWHM; see Note 4 for axis definition)
+
|GAU_SEMI1 || Real*4 || arcmin || Gaussian fit along axis 1 (FWHM; see note 4 for axis definition)
 
|-
 
|-
 
|GAU_SEMI1_ERR || Real*4 || arcmin || Uncertainty (1 sigma) in derived Gaussian fit along axis 1
 
|GAU_SEMI1_ERR || Real*4 || arcmin || Uncertainty (1 sigma) in derived Gaussian fit along axis 1
Line 642: Line 645:
 
|GAU_SEMI2_ERR || Real*4 || arcmin || Uncertainty (1 sigma) in derived Gaussian fit along axis 2
 
|GAU_SEMI2_ERR || Real*4 || arcmin || Uncertainty (1 sigma) in derived Gaussian fit along axis 2
 
|-
 
|-
|GAU_THETA || Real*4 || deg || Gaussian fit orientation angle (Note 4)
+
|GAU_THETA || Real*4 || deg || Gaussian fit orientation angle (note 4)
 
|-
 
|-
 
|GAU_THETA_ERR || Real*4 || deg || Uncertainty (1 sigma) in derived gaussian fit orientation angle
 
|GAU_THETA_ERR || Real*4 || deg || Uncertainty (1 sigma) in derived gaussian fit orientation angle
Line 650: Line 653:
 
!colspan="4"|Flags and validation
 
!colspan="4"|Flags and validation
 
|-
 
|-
|EXTENDED || Integer*2 || || Extended source flag (Note 2)
+
|EXTENDED || Integer*2 || || Extended source flag (note 2)
 
|-
 
|-
 
|CIRRUS_N || Integer*2 || || Number of sources detected at 857 GHz within 1 degree
 
|CIRRUS_N || Integer*2 || || Number of sources detected at 857 GHz within 1 degree
 
|-
 
|-
|EXT_VAL || Integer*2 || || External validation flag (Note 3)
+
|EXT_VAL || Integer*2 || || External validation flag (note 3)
 
|-
 
|-
 
|ERCSC || String || || Name of the ERCSC counterpart if any  
 
|ERCSC || String || || Name of the ERCSC counterpart if any  
Line 675: Line 678:
  
 
'''Notes'''
 
'''Notes'''
# Source names consist of a prefix and a position. The prefix used is PCCS1 fff for the catalogue at fff GHz. The position is in Galactic coordinates and specified as "Glll.ll±bb.bb" where the (l,b) values are truncated to two decimal places. For example, a source detected at (l,b) = (120.237, 4.231) in the 545 GHz Planck map would be labelled PCCS1 545 G120.23±04.23.
+
# Source names consist of a prefix and a position. The prefix used is PCCS1 fff for the catalogue at fff GHz. The position is in Galactic coordinates and specified as "Glll.ll±bb.bb" where the (<i>l</i>,<i>b</i>) values are truncated to two decimal places. For example, a source detected at (<i>l</i>,<i>b</i>) = (120.237, 4.231) in the 545 GHz Planck map would be labelled PCCS1 545 G120.23±04.23.
 
# The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criteria for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
 
# The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criteria for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
 
# The EXT_VAL flag takes the value of 0, 1, or 2, based on the following conditions:
 
# The EXT_VAL flag takes the value of 0, 1, or 2, based on the following conditions:
Line 682: Line 685:
 
#: = 0: The source has no clear counterpart in one of the ancillary catalogues and it has not been detected by the internal multi-frequency method or neighbouring frequencies.
 
#: = 0: The source has no clear counterpart in one of the ancillary catalogues and it has not been detected by the internal multi-frequency method or neighbouring frequencies.
 
# The x-axis is defined for each source as parallel to the line of constant colatitude, with the same direction as the longitude. Therefore the position angles are measured anticlockwise from the y-axis.
 
# The x-axis is defined for each source as parallel to the line of constant colatitude, with the same direction as the longitude. Therefore the position angles are measured anticlockwise from the y-axis.
 +
 +
  
 
</div>
 
</div>
 
 
</div>
 
</div>
  
<div class="toccolours mw-collapsible mw-collapsed" style="width:800px">
+
<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #d5fdf4;width:95%">
 
'''First Planck Release (2011): Description of the 2011 ERCSC (Early Compact Source, Cold Core and SZ Catalogues )'''
 
'''First Planck Release (2011): Description of the 2011 ERCSC (Early Compact Source, Cold Core and SZ Catalogues )'''
 
<div class="mw-collapsible-content">
 
<div class="mw-collapsible-content">
Line 696: Line 700:
 
The ERCSC consisted of nine source lists, one at each of the nine Planck frequency channels. The number of sources in the lists range from 705 at 30 GHz to 8988 at 857 GHz. No attempt was made to cross-match the sources from the different frequencies due to the wide range of spatial resolutions (33 arcmin at 30 GHz to 4.3 arcmin at 857 GHz) spanned by Planck. Furthermore, a list of ''Cold Cores'' of interstellar molecular clouds within the Galaxy and a list of galaxy clusters detected through the Sunyaev- Zel’dovich effect (SZ), were also provided. These consisted of candidate sources that were detected using multifrequency algorithms that use the distinct spectral signature of such sources. The Cold Cores catalogue contained 915 sources while the SZ cluster catalogue consisted of 189 sources
 
The ERCSC consisted of nine source lists, one at each of the nine Planck frequency channels. The number of sources in the lists range from 705 at 30 GHz to 8988 at 857 GHz. No attempt was made to cross-match the sources from the different frequencies due to the wide range of spatial resolutions (33 arcmin at 30 GHz to 4.3 arcmin at 857 GHz) spanned by Planck. Furthermore, a list of ''Cold Cores'' of interstellar molecular clouds within the Galaxy and a list of galaxy clusters detected through the Sunyaev- Zel’dovich effect (SZ), were also provided. These consisted of candidate sources that were detected using multifrequency algorithms that use the distinct spectral signature of such sources. The Cold Cores catalogue contained 915 sources while the SZ cluster catalogue consisted of 189 sources
  
In order to generate the ERCSC,  four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is >90%. Reliability is defined as the fraction of sources in the catalog which have measured flux densities which are within 30% of their true flux density. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10σ photometric flux density limit of the catalogue at $|b| > 30$ deg is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion.  The sensitivity of the ERCSC is shown in the figure below. The ERCSC sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs.  
+
In order to generate the ERCSC,  four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is >90%. Reliability is defined as the fraction of sources in the catalog which have measured flux densities which are within 30% of their true flux density. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10σ photometric flux density limit of the catalogue at |<i>b</i>| > 30&deg; is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion.  The sensitivity of the ERCSC is shown in the figure below. The ERCSC sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared-luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs.  
  
 
The multifrequency information from Planck allows some basic classification of the sources to be undertaken. In the Galactic plane, at frequencies below 100 GHz, the majority of the sources are dominated by synchrotron or free-free emission. At the higher frequencies, the sources are almost exclusively dominated by thermal dust emission. At high Galactic latitudes however, the synchrotron sources  dominate the source counts to 217 GHz with dusty sources being the primary source population at 353 GHz and higher. Recent attempts to classify a subset of the Planck 857 GHz sources at high latitudes based on cross-correlations with sources in other catalogs such as WISE and SDSS, found that almost half of them are associated with stars and low-redshift galaxies while a significant fraction (44%) might be interstellar medium features{{BibCite|Johnson2013}}.
 
The multifrequency information from Planck allows some basic classification of the sources to be undertaken. In the Galactic plane, at frequencies below 100 GHz, the majority of the sources are dominated by synchrotron or free-free emission. At the higher frequencies, the sources are almost exclusively dominated by thermal dust emission. At high Galactic latitudes however, the synchrotron sources  dominate the source counts to 217 GHz with dusty sources being the primary source population at 353 GHz and higher. Recent attempts to classify a subset of the Planck 857 GHz sources at high latitudes based on cross-correlations with sources in other catalogs such as WISE and SDSS, found that almost half of them are associated with stars and low-redshift galaxies while a significant fraction (44%) might be interstellar medium features{{BibCite|Johnson2013}}.
Line 708: Line 712:
 
The figure shows the ERCSC flux density limits, quanitfied as the faintest ERCSC source at |b|<10 deg (dashed black line) and at |b|>30 deg (solid black line), compared to those of other wide area surveys ({{PlanckPapers|planck2011-1-10}}). Also shown are spectra of known sources of foreground emission as red lines. The ERCSC sensitivity is worse in the Galactic plane due to the strong contribution of ISM emission, especially at submillimeter wavelengths. At face value, the WMAP and Planck flux density limits appear to be comparable at the lowest frequencies, but the Planck ERCSC is much more complete as discussed in {{PlanckPapers|planck2011-1-10}}.
 
The figure shows the ERCSC flux density limits, quanitfied as the faintest ERCSC source at |b|<10 deg (dashed black line) and at |b|>30 deg (solid black line), compared to those of other wide area surveys ({{PlanckPapers|planck2011-1-10}}). Also shown are spectra of known sources of foreground emission as red lines. The ERCSC sensitivity is worse in the Galactic plane due to the strong contribution of ISM emission, especially at submillimeter wavelengths. At face value, the WMAP and Planck flux density limits appear to be comparable at the lowest frequencies, but the Planck ERCSC is much more complete as discussed in {{PlanckPapers|planck2011-1-10}}.
  
 +
</div>
 +
</div>
  
+
</div>
'''Union Catalogue'''
 
  
The union catalogue is contained in  ''{{PLASingleFile|fileType=cat | name=COM_PCCS_SZ-union_R1.12.fits | link=COM_PCCS_SZ-union_R1.12.fits}}''.
+
<div class="toccolours" style="background-color: #FFDAB9" >
 +
<div class="toccolours" style="background-color: #FFDAB9" >
  
 +
=== (2015) Bayesian Extraction and Estimation Package (BeeP) reprocessing of PCCS2+PCCS2E at 857 GHz ===
  
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
<span class="sans-serif">BeeP</span>’s catalogue was developed using the data and the methodology described in the companion paper {{PlanckPapers|planck2020-LV}}.<br />
|- bgcolor="ffdead" 
 
!colspan="4" | Extension 0: Primary header, no data
 
|- bgcolor="ffdead" 
 
! FITS Keyword || Data Type || Units || Description
 
|-
 
|INSTRUME || String || || Instrument.
 
|-
 
| VERSION || String || || Version of catalogue.
 
|-
 
| DATE || String || || Date file created: yyyy-mm-dd.
 
|-
 
| ORIGIN || String || || Name of organization responsible for the data.
 
|-
 
| TELESCOP || String || || PLANCK.
 
|-
 
| CREATOR || String || || Pipeline version.
 
|-
 
| DATE-OBS || String || || Start time of the survey: yyyy-mm-dd.
 
|-
 
| DATE-END || String || || End time of the survey: yyyy-mm-dd.
 
|-
 
| PROCVER || String || || Data version.
 
|-
 
| PP_ALPHA || Real*4 || || GNFW pressure profile $\alpha$ parameter.
 
|-
 
| PP_BETA || Real*4 || || GNFW pressure profile $\beta$ parameter.
 
|-
 
| PP_GAMMA || Real*4 || || GNFW pressure profile $\gamma$ parameter.
 
|-  
 
| PP_C500 || Real*4 || || GNFW pressure profile $c_{500}$ parameter.
 
|-
 
| PP_Y2YFH || Real*4 || || Conversion factor from $Y$ to $Y_{500}$.
 
  
|- bgcolor="ffdead"  
+
Traits:<br />
!colspan="4" | Extension 1: data extension (BINTABLE)
+
* It is a catalogue of compact objects.
|- bgcolor="ffdead"  
+
* It is the result of a ‘''non-blind''’ exercise where Planck’s PCCS2+2E catalogue positions at 857 GHz were used. It contains exactly the same number of rows as the original catalogue and no attempt of detecting new sources was made.
! Column Name || Data Type || Units || Description
+
* It is a parametric Bayesian multi-channel algorithm. The source parameter estimates are derived from the posterior distributions of a data model likelihood.
 +
* It employs Planck all-sky temperature maps at <math display="inline">353, 545, 857</math> GHz channels from the Planck 2015 release and the <math display="inline">3000</math> GHz IRIS map, a reprocessed IRAS map.<br />
 +
 
 +
The catalogue product is made of three components:<br />
 +
* A table with source parameter estimates and uncertainty summary statistics: [http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST.NAME=COM_PCCS_BEEP_R2.00.fits COM_PCCS_BEEP_R2.00.fits].
 +
* A collection of Spectral Energy Density (SED) figures. <span>Not yet available</span>
 +
* A collection of figures with the parameter posterior distributions. <span>Not yet available</span>
 +
 
 +
==== Table of source parameter estimates. ====
 +
The table with the source parameters contains 48181 rows, as many as in Planck 857 GHz channel PCCS2 and PCCSE catalogues combined. Each row has 108 fields (columns). If a field value is ill defined or not available, then its value is set to largest negative value of the double type in the IEEE standard: <math display="inline">\approx -1.797693 \times 10^{305}</math>. The table of source parameter estimates (columns) is divided into 5 sections:
 +
 
 +
'''General'''<br />
 +
Contains fields that are independent of the physical model used to described the source, or background, emission. It holds the reliability assessment fields (see section A.1.2 and 6.2.3 of the companion paper).
 +
* <span class="sans-serif">BeeP</span> position columns were obtained using the MBB SED model.
 +
* If a likelihood maximum was not found, then <span class="sans-serif">MAXFOUND</span> is set to <math display="inline">0</math>, otherwise is <math display="inline">1</math>.
 +
* <span class="sans-serif">NPSNR</span> is <span class="sans-serif">BeeP</span>’s proxy for the Signal-to-Noise Ratio (SNR) in a statistical sense (detection significance) like ‘''how many sigmas this detection is''’. It cannot be read as the flux density divided by the flux density error bar. A Gaussian homogeneous background is assumed.
 +
* <span class="sans-serif">SRCSIG</span> is <span class="sans-serif">BeeP</span>’s detection significance. It is derived from <span class="sans-serif">NPSNR</span> with a non-Gaussianity correction based on <span class="sans-serif">RELTH</span> applied.
 +
* <span class="sans-serif">EST_QUALITY</span> indicates the expected quality of the source parameter estimates. The highest quality is 5. Then, if a source does not meet the conditions in table, the correspondent penalty is subtracted.
 +
* The field &quot;<span class="sans-serif">NAME</span>&quot; has the exact same source name as in Planck’s 857 GHz channel PCCS2+2E and should be used to reference any source in this catalogue.<br />
 +
 
 +
'''Thermal sub-catalogue''' (see section 6.2.1 of the companion paper)
 +
* The sources Spectral Energy Density (SED) was modeled after a Modified Black-Body (MBB) with <math display="inline">3</math> parameters: Temperature (<math display="inline">T</math>), Spectral index (<math display="inline">\beta</math>) and Flux density at a reference channel (<math display="inline">S_{\textsf{ref}}</math>).
 +
* The MBB parameters, together with the source radius and position, make the likelihood parameter set.
 +
* Colour correction coefficients were included in the likelihood.<br />
 +
 
 +
'''‘Free’ amplitude at each channel sub-catalogue'''<br />
 +
Contains a sub-catalogue of independent flux density measurements (not dependent on a SED physical model) at each of the utilized channels (see section A.1.2 of the companion paper).
 +
* Main goal was to allow a direct comparison with catalogues obtained at each channel independently. No source SED model was used
 +
* The likelihood parameter set was the flux density at each channel plus source position and radius. The best fit flux densities at each channel and error bars were computed from the flux density posterior distributions. With the <math display="inline">4</math> pairs {<math display="inline">S_\nu,\sigma_{S_\nu}</math>}, a MBB curve was fitted using a Gaussian likelihood.
 +
* During the estimation of the initial flux densities at each channel, colour-correction was not used. However when later fitting the MBB parameters colour-correction coefficients were included.<br />
 +
 
 +
'''Background thermal properties catalogue''' (see section 6.3 of the companion paper)
 +
* Main goal was to provide a measurement of the contrast between the thermal properties of the background and the source.
 +
* The average brightness around each PCCS2+2E position (<math display="inline">32\times32</math> pixels; <math display="inline">\approx 55'\times55'</math>) and its standard deviation were computed for each individual channel. The map offset levels had previously been corrected.
 +
* With the <math display="inline">4</math> pairs {<math display="inline">B_\nu,\sigma_{B_\nu}</math>}, a MBB curve with colour correction, was fitted using a Gaussian likelihood.
 +
* The Signal-to-Noise Ratio Raw (SNRr) was computed by dividing the source average brightness at each channel by the background brightness standard deviation. The source average brightness was estimated by dividing the MBB flux density estimate at that frequency by the total solid angle resulting from the convolution of the beam, at that channel, and the intrinsic source extension.<br />
 +
 
 +
'''Source ID and association fields'''<br />
 +
Adds a <span class="sans-serif">BeeP</span> source index. Contains the separation between <span class="sans-serif">BeeP</span>’s catalogue positions and those in Planck’s 857 PCCS2+2E and flags potential multiple detections of the same physical object. The field <span class="sans-serif">BEEPSRCASS</span> contains either the same index as that of the source or the index of a close neighbour if it is inside a radius of <math display="inline">8'</math> and its <span class="sans-serif">NPSNR</span> is higher.<br />
 +
 
 +
[[File:fullSkyTempMol_3_01.png|800px|center]]
 +
<div style='text-align: center;'>Sky distribution of the sources Modified Black Body (MBB) model temperatures in the catalogue (colour scale in thermodynamic kelvins). ''Bottom:'' Spectral indices of the MBB model.</div>
 +
<br>
 +
[[File:fullSkyBetaMol_3_01.png|800px|center ]]
 +
<div style='text-align: center;'>Spectral indices of the MBB model.</div>
 +
<br>
 +
[[File:fullSkySrcsigMol_3_01.png|800px|center|none]]
 +
<div style='text-align: center;'>Sky distribution of the sources <math display="inline">\log_{10}</math><span class="sans-serif">SRCSIG</span> statistic (colour scale). Sources inside the IRIS mask were not included. Sources inside the IRIS mask were not included.</div>
 +
 
 +
<div id="table:CorrectionFlux">
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" width=750px
 +
|+ <small>'''Flux density corrections'''</small>
 +
|- bgcolor="ffdead" 
 +
|+  Recommended values for the flux density error bar correction <math display="inline">c</math> (mJy)
 +
! Set
 +
! location
 +
!align="right"| c (mJy)
 
|-
 
|-
|INDEX || Int*4 || || Index. Used to cross-reference with individual catalogues.
+
| PCCS2
 +
| Planck’s PCCS2 region
 +
|align="right"| 57
 
|-
 
|-
|NAME || String || || Source name, (Note 1)
+
| PCCS2E <math display="inline">\wedge \, |glat| > 10^\circ</math>
 +
| Planck’s PCCS2E region and <math display="inline">|glat| > 10^\circ</math>
 +
|align="right"| 168
 
|-
 
|-
|GLON || Real*8 || degrees || Galactic longitude.
+
| <math display="inline">|glat| \leq 10^\circ</math>
 +
| <math display="inline">|glat| \leq 10^\circ</math>
 +
|align="right"| 820
 +
|}
 +
</div>
 +
 
 +
==== Description of the catalogue columns. ====
 +
 
 +
<div id="table:catalogueFields">
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" width=750px
 +
|+ <small>'''BeeP Columns'''</small>
 +
|- bgcolor="ffdead" 
 +
|+ Description of the fields in the table component of the catalogue.
 +
! Field name
 +
! Type
 +
! Size
 +
! Units
 +
! Description
 +
! Comments
 
|-
 
|-
|GLAT || Real*8 || degrees || Galactic latitude.
+
|
|-
+
|
|RA   || Real*8 || degrees || Right ascension (J2000) transformed from (GLON,GLAT).
+
|
 +
|
 +
|
 +
|
 +
|-
 +
| NAME
 +
| char
 +
| 20
 +
|
 +
| PCCS2+2E Source name
 +
|
 +
|-
 +
| PCCS2RA
 +
| double
 +
| 8
 +
| Degrees
 +
| J2000 RA in PCCS2+2E
 +
|
 +
|-
 +
| PCCS2DEC
 +
| double
 +
| 8
 +
| Degrees
 +
| J2000 DEC in PCCS2+2E
 +
|
 
|-
 
|-
|DEC  || Real*8 || degrees || Declination (J2000) transformed from (GLON,GLAT).
+
| BEEPGLON
 +
| double
 +
| 8
 +
| Degrees
 +
| Galactic longitude estimated by <span class="sans-serif">BeeP</span>
 +
| Average of 95% highest likelihood samples
 +
|-
 +
| BEEPGLAT
 +
| double
 +
| 8
 +
| Degrees
 +
| Galactic latitude estimated by <span class="sans-serif">BeeP</span>
 +
| Average of 95% highest likelihood samples
 +
|-
 +
| BEEPRA
 +
| double
 +
| 8
 +
| Degrees
 +
| J2000 RA estimated by <span class="sans-serif">BeeP</span>
 +
| Computed from BEEPGLON and BEEPGLAT
 
|-
 
|-
|POS_ERR || Real*4 || arcmin || Position uncertainty (approximate 68% confidence interval). See [[#Caveats|Caveats]] below.
+
| BEEPDEC
 +
| double
 +
| 8
 +
| Degrees
 +
| J2000 DEC estimated by <span class="sans-serif">BeeP</span>
 +
| Computed from BEEPGLON and BEEPGLAT
 
|-
 
|-
|SNR || Real*4 || || Signal-to-noise ratio of the detection.
+
| PCCS2GLON
 +
| double
 +
| 8
 +
| Degrees
 +
| Galactic longitude in PCCS2+2E
 +
|
 
|-
 
|-
|PIPELINE || Int*4 || || Souce pipeline: 1= MMF1; 2 = MMF3; 3 = PwS.
+
| PCCS2GLAT
 +
| double
 +
| 8
 +
| Degrees
 +
| Galactic latitude in PCCS2+2E
 +
|
 
|-
 
|-
|PIPE_DET || Int*4 || || Pipelines which detect this object (note 2).
+
| NPSNR
 +
| double
 +
| 8
 +
| Unitless
 +
| Source detection significance uncorrected
 +
| Background assumed Gaussian (see section A.1.2 of PIP LV)
 
|-
 
|-
|PCCS || Bool || || Indicates whether detection matches any PCCS source.
+
| RELTH
 +
| double
 +
| 8
 +
| Unitless
 +
| 95% percentile of the likelihood background statistic
 +
| Used to correct for the background non-gaussinaty (see section A.1.2 of PIP LV)
 
|-
 
|-
|VALIDATION || Int*4 || || External validation status (Note 3)
+
| ACCEPT
 +
| double
 +
| 8
 +
| Unitless
 +
| Sample acceptance ratio of the MCMC chain
 +
| If low (<math display="inline">< 10\%</math>) might be indicative of unreliable estimates
 
|-
 
|-
|ID_EXT || String|| || External identifier of cluster.
+
| INPIX
 +
| double
 +
| 8
 +
| Unitless
 +
| Percentage of pixels in-painted in the field
 +
| Very high numbers might indicate unreliable estimates
 
|-
 
|-
|REDSHIFT || Real*4 || || Redshift of cluster.
+
| MAXFOUND
 +
| double
 +
| 8
 +
| 0 / 1
 +
| If a likelihood maximum was found within a radius of 3 pixels from the original location
 +
| If a maximum is not found this is an indication that <span class="sans-serif">BeeP</span>’s position might not be a compact source
 
|-
 
|-
|COSMO || Bool || || Detection is in the cosmology sample.
+
| SRCSIG
 +
| double
 +
| 8
 +
| Unitless
 +
| Source detection significance
 +
| Corrected for background non-gaussianity (see section A.1.2 of PIP LV)
 
|-
 
|-
|COMMENT|| Bool || || Detection has a comment in the associated text file (Note 4).
+
| EST_QUALITY
|}
+
| double
 
+
| 8
'''Notes'''
+
| Unitless
# format is ''PSZ1 Glll.ll+mn;bb.b'' where (l,b) are the Galactic and truncated to 2 decimal places.
+
| Source parameter estimates quality flag [5 - 0].
# The three least significant decimal digits are used to represent detection or non-detection by the pipelines. Order of the digits: hundreds = MMF1; tens = MMF3; units = PwS. If it is detected then the corresponding digit is set to 1, otherwise it is set to 0.
+
| Quality starts at 5 and the penalties in table [[#table:QualityPenalties|[table:QualityPenalties]]] are applied. Higher values mean higher quality.
# values are: 1 = candidate of class 1; 2 = candidate of class 2; 3 = candidate of class 3; 10 = Planck cluster confirmed by follow-up;  20 = known cluster.
+
|-
# The  comments on the detections in the catalogue are contained in a text file called ''{{PLASingleFile|fileType=catdoc | name=COM_PCCS_SZ-union_comments_R1.11.txt | link=COM_PCCS_SZ-union_comments_R1.11.txt}}'', which contains one line for each detection in the union catalogue with COMMENT = T. The line starts with the INDEX and NAME of the detection to facilitate cross-referencing. The remainder of the line is the comment on that detection.
+
| POSERR
 
+
| double
'''Individual Catalogues'''
+
| 8
 
+
| Arcmin
The individual pipeline catalogues are contained in the FITS files
+
| Source position uncertainty. Radius of uncertainty around source best fit position
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-MMF1_R1.11.fits  | link=COM_PCCS_SZ-MMF1_R1.11.fits }} (Matched Multi-Filter method #1)
+
| <math display="inline">\sigma; \sigma</math> is the Rayleigh distribution scale factor (see section 6.2.3 of PIP LV)
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-MMF3_R1.12.fits  | link=COM_PCCS_SZ-MMF3_R1.12.fits }} (Matched Multi-Filter method #3)
+
|-
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-PwS_R1.11.fits  | link=COM_PCCS_SZ-PwS_R1.11.fits }} (Powell Snakes method)
+
|
Their structure is as follows:
+
|
 
+
|
 
+
|
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
|
|+ '''FITS file structure'''
+
|
|- bgcolor="ffdead"  
+
|-
 
+
| BETA
! colspan="4" | Ext. 0: Primary header, no data
+
| double
|- bgcolor="ffdead" 
+
| 8
! FITS Keyword || Data Type || Units || Description
+
| Unitless
|-  
+
| Source spectral index (MBB); Modified Black Body
|INSTRUME || String || || Instrument.
+
| Posterior median value
|-  
+
|-
| VERSION || String || || Version of catalogue.
+
| BETAL2SB
|-  
+
| double
| DATE || String || || Date file created: yyyy-mm-dd.
+
| 8
|-  
+
| Unitless
| ORIGIN || String || || Name of organization responsible for the data.
+
| Source spectral index uncertainty lower boundary
|-  
+
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
| TELESCOP || String || || PLANCK.
+
|-
|-  
+
| BETAH2SB
| CREATOR || String || || Pipeline version.
+
| double
|-  
+
| 8
| DATE-OBS || String || || Start time of the survey: yyyy-mm-dd.
+
| Unitless
|-
+
| Source spectral index uncertainty upper boundary
| DATE-END || String || || End time of the survey: yyyy-mm-dd.
+
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
|-  
+
|-
| PROCVER || String || || Data version.
+
| TEMP
|-  
+
| double
| PP_ALPHA || Real*4 || || GNFW pressure profile $\alpha$ parameter.
+
| 8
|-  
+
| Kelvin
| PP_BETA || Real*4 || || GNFW pressure profile $\beta$ parameter.
+
| Source temperature (MBB); Modified Black Body
|-  
+
| Posterior median value
| PP_GAMMA || Real*4 || || GNFW pressure profile $\gamma$ parameter.
+
|-
|-  
+
| TL2SB
| PP_C500 || Real*4 || || GNFW pressure profile $c_{500}$ parameter.
+
| double
|-  
+
| 8
| PP_Y2YFH || Real*4 || || Conversion factor from $Y$ to $Y_{500}$.
+
| Kelvin
|- bgcolor="ffdead"  
+
| Source temperature uncertainty lower boundary
 
+
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 
+
|-
! colspan="4" | Ext. 1: EXTNANE = ''PSZ_INDIVIDUAL'' (BINTABLE)
+
| TH2SB
|- bgcolor="ffdead" 
+
| double
! Column Name || Data Type || Units || Description
+
| 8
 +
| Kelvin
 +
| Source temperature uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| EXT
 +
| double
 +
| 8
 +
| Arcmin
 +
| Source extension before beam convolution
 +
| This radius is constant across all channels. The extension parameter was obtained with ''likelihood'' beam widths (see section A.2.3 of PIP LV); Posterior median value
 +
|-
 +
| EXTL2SB
 +
| double
 +
| 8
 +
| Arcmin
 +
| Source extension uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 +
|-
 +
| EXTH2SB
 +
| double
 +
| 8
 +
| Arcmin
 +
| Source extension uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| R
 +
| double
 +
| 8
 +
| Arcmin
 +
| Source radius before beam convolution
 +
| This radius is constant across all channels. The parameter was computed from EXT and gives an indication of whether the source is extended (see section 6.2.2 of PIP LV)
 +
|-
 +
| SREF
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at the reference frequency
 +
| Reference frequency is <math display="inline">857</math> GHz; Posterior median value
 +
|-
 +
| SREFL2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at the reference frequency uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 +
|-
 +
| SREFH2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at the reference frequency uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| S3000
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">3000</math> GHz; MBB predicted at <math display="inline">3000</math> GHz
 +
| Posterior median value
 +
|-
 +
| S3000L2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">3000</math> GHz uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 +
|-
 +
| S3000H2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">3000</math> GHz uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| S857
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">857</math> GHz; MBB predicted at <math display="inline">857</math> GHz
 +
| Posterior median value
 +
|-
 +
| S857L2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">857</math> GHz uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 +
|-
 +
| S857H2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">857</math> GHz uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| S545
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">545</math> GHz; MBB predicted at <math display="inline">545</math> GHz
 +
| Posterior median value
 
|-
 
|-
|INDEX || Int*4 || || Index from union catalogue.
+
| S545L2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">545</math> GHz uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 
|-
 
|-
|NAME || String || || Source name - see Note1
+
| S545H2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">545</math> GHz uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 
|-
 
|-
|GLON || Real*8 || degrees || Galactic longitude.
+
| S353
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">353</math> GHz; MBB predicted at <math display="inline">353</math> GHz
 +
| Posterior median value
 
|-
 
|-
|GLAT || Real*8 || degrees || Galactic latitude.
+
| S353L2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">353</math> GHz uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 
|-
 
|-
|RA  || Real*8 || degrees || Right ascension (J2000) transformed from (GLON,GLAT).
+
| S353H2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">353</math> GHz uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 
|-
 
|-
|DEC  || Real*8 || degrees || Declination (J2000) transformed from (GLON,GLAT).
+
| BETAMLIKE
 +
| double
 +
| 8
 +
| Unitless
 +
| Source spectral index (MBB); Modified Black Body
 +
| Maximum likelihood estimate
 
|-
 
|-
|POS_ERR || Real*4 || arcmin || Position uncertainty (approximate 68% confidence interval). See [[#Caveats|Caveats]] below.
+
| TEMPMLIKE
 +
| double
 +
| 8
 +
| Kelvin
 +
| Source temperature (MBB); Modified Black Body
 +
| Maximum likelihood estimate
 
|-
 
|-
|SNR || Real*4 || || Signal-to-noise ratio of the detection.
+
| SREFMLIKE
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at reference frequency; Modified Black Body
 +
| Maximum likelihood estimate
 
|-
 
|-
|SNR_COMPAT || Real*4 || || SNR of the detection in compatibility mode (Note 2)
+
|
 +
|
 +
|
 +
|
 +
|
 +
|
 +
|-
 +
| FREEGLON
 +
| double
 +
| 8
 +
| Degrees
 +
| Galactic longitude (FREE channel amplitudes)
 +
| Average of 95% highest likelihood samples
 +
|-
 +
| FREEGLAT
 +
| double
 +
| 8
 +
| Degrees
 +
| Galactic latitude (FREE channel amplitudes)
 +
| Average of 95% highest likelihood samples
 +
|-
 +
| FREES3000
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">3000</math> GHz; Estimated directly at the IRIS map
 +
| Posterior median value
 +
|-
 +
| FREES3000L2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">3000</math> GHz uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 
|-
 
|-
|TS_MIN || Real*4 || || Minimum value of $\theta_\mathrm{s}$ in grid in second extension HDU (see below).
+
| FREES3000H2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">3000</math> GHz uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 
|-
 
|-
|TS_MAX || Real*4 || || Maximum value of $\theta_\mathrm{s}$ in grid in second extension HDU (see below).
+
| FREES857
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">857</math> GHz; Estimated directly at Planck’s <math display="inline">857</math> GHz map
 +
| Posterior median value
 
|-
 
|-
|Y_MIN || Real*4 || || Minimum value of $Y$ in grid in second extension HDU (see below).
+
| FREES857L2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at <math display="inline">857</math> GHz uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 
|-
 
|-
|Y_MAX || Real*4 || || Maximum value of $Y$ in grid in second extension HDU (see below).
+
| FREES857H2SB
 
+
| double
|- bgcolor="ffdead"  
+
| 8
! Keyword || Data Type || Value || Description
+
| Jy
|-  
+
| Flux density at <math display="inline">857</math> GHz uncertainty upper boundary
| PIPELINE || String || || Name of detection pipeline.
+
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
|- bgcolor="ffdead"  
+
|-
 
+
| FREES545
 
+
| double
! colspan="4" | Ext. 2: EXTNAME = ''PSZ_PROBABILITY'' (IMAGE) - Note 3
+
| 8
|- bgcolor="ffdead" 
+
| Jy
! Keyword || Data Type || Value || Description
+
| Flux density at <math display="inline">545</math> GHz; Estimated directly at Planck’s <math display="inline">545</math> GHz map
|-  
+
| Posterior median value
| NAXIS1 || Integer || 256 || Dim 1
+
|-
|-  
+
| FREES545L2SB
| NAXIS2 || Integer || 256 || Dim 2  
+
| double
|-  
+
| 8
| NAXIS3 || Integer || Nsources || Dim 3 = Number of sources
+
| Jy
|- bgcolor="ffdead" 
+
| Flux density at <math display="inline">545</math> GHz uncertainty lower boundary
! Keyword || Data Type || Value || Description
+
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
|-  
+
|-
| PIPELINE || String || || Name of detection pipeline.
+
| FREES545H2SB
|}
+
| double
 
+
| 8
'''Notes'''
+
| Jy
# Format ''PSZ1 Glll.ll&plusmn;bb.bb'' where (l, b) are the Galactic coordinates truncated to 2 decimal places.
+
| Flux density at <math display="inline">545</math> GHz uncertainty upper boundary
# For PwS, this is the S/N evaluated in a manner compatible with the MMF pipelines. For MMF1 and MMF3, it is identical to SNR.
+
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
# Ext. 2 contains a three-dimensional image with the two-dimensional probability distribution in $\theta_\mathrm{s}$ and $Y$ for each detection. The probability distributions are evaluated on a 256 &times; 256 linear grid between the limits specified in Ext. 1. The limits are determined independently for each detection. The dimension of the 3D image is 256 &times; 256 &times; n, where n is the number of detections. The first dimension is $\theta_\mathrm{s}$ and the second dimension is $Y$.
+
|-
 
+
| FREES353
'''Mask'''
+
| double
 
+
| 8
The mask used to construct the catalogue is contained in a file
+
| Jy
: ''{{PLASingleFile|fileType=catdoc | name=COM_PCCS_SZ-unionMask_2048_R1.11.fits| link=COM_PCCS_SZ-unionMask_2048_R1.11.fits}}''. <span style="color:red">
+
| Flux density at <math display="inline">353</math> GHz; Estimated directly at Planck’s <math display="inline">353</math> GHz map
It is in GALACTIC coordinates, NESTED ordering, NSIDE=2048.
+
| Posterior median value
 
+
|-
'''Additional information'''
+
| FREES353L2SB
 
+
| double
A set of comments on the union catalogue is available in
+
| 8
 
+
| Jy
: ''{{PLASingleFile|fileType=cat | name=COM_DocPCCS_SZ-union-comments_R1.11.txt | link=COM_DocPCCS_SZ-union-comments_R1.11.txt}}''
+
| Flux density at <math display="inline">353</math> GHz uncertainty lower boundary
 
+
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
Additional information on the SZ detections was retrieved from external sources and written into the FITS file
+
|-
 
+
| FREES353H2SB
: ''{{PLASingleFile|fileType=cat | name=COM_PCCS_SZ-validation_R1.12.fits | link=COM_PCCS_SZ-validation_R1.12.fits}}''
+
| double
 
+
| 8
(for more details see {{PlanckPapers|planck2013-p05a}}). This file contains a single ''BINTABLE'' extension.  The table contains 1 line per source, and the columns and their meaning are given below.
+
| Jy
 
+
| Flux density at <math display="inline">353</math> GHz uncertainty upper boundary
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
|+ '''FITS file structure'''
+
|-
|- bgcolor="ffdead" 
+
| FREEEXT
 
+
| double
! colspan="4" | Ext. 0:  (BINTABLE)
+
| 8
|- bgcolor="ffdead" 
+
| Arcmin
! Column Name || Data Type || Units || Description
+
| Source extension before beam convolution
 +
| This radius is constant across all channels. The extension parameter was obtained with ''likelihood'' beam widths (see section A.2.3 of PIP LV); Posterior median value
 +
|-
 +
| FREEEXTL2SB
 +
| double
 +
| 8
 +
| Arcmin
 +
| Source extension uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 +
|-
 +
| FREEEXTH2SB
 +
| double
 +
| 8
 +
| Arcmin
 +
| Source extension uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| FREER
 +
| double
 +
| 8
 +
| Arcmin
 +
| Source radius before beam convolution
 +
| This radius is constant across all channels. The parameter was computed from FREEEXT and gives an indication of whether the source is extended (see section 6.2.2 of PIP LV)
 +
|-
 +
| FREEBETA
 +
| double
 +
| 8
 +
| Unitless
 +
| Source spectral index; Computed from the flux densities estimated at each channel<ref>A Gaussian likelihood was created using the <math display="inline">4</math> flux densities and error bars measured at each channel.</ref>
 +
| Posterior median value
 +
|-
 +
| FREEBETAL2SB
 +
| double
 +
| 8
 +
| Unitless
 +
| Source spectral index uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 +
|-
 +
| FREEBETAH2SB
 +
| double
 +
| 8
 +
| Unitless
 +
| Source spectral index uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| FREETEMP
 +
| double
 +
| 8
 +
| Kelvin
 +
| Source temperature; Computed from the flux densities estimated at each channel
 +
| Posterior median value
 +
|-
 +
| FREETL2SB
 +
| double
 +
| 8
 +
| Kelvin
 +
| Source temperature uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 +
|-
 +
| FREETH2SB
 +
| double
 +
| 8
 +
| Kelvin
 +
| Source temperature uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| FREESREF
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at the reference frequency; Estimated from the likelihood
 +
| Reference frequency is <math display="inline">857</math> GHz; Posterior median value
 +
|-
 +
| FREESREFL2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at the reference frequency uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 +
|-
 +
| FREESREFH2SB
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at the reference frequency uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 +
|-
 +
| FREEBETAMLIKE
 +
| double
 +
| 8
 +
| Unitless
 +
| Source spectral index; Computed from the flux densities estimated at each channel
 +
| Maximum likelihood estimate
 +
|-
 +
| FREETEMPMLIKE
 +
| double
 +
| 8
 +
| Kelvin
 +
| Source temperature; Computed from the flux densities estimated at each channel
 +
| Maximum likelihood estimate
 
|-
 
|-
|INDEX || Int*4 || || Index from union catalogue.
+
| FREESREFMLIKE
 +
| double
 +
| 8
 +
| Jy
 +
| Flux density at the reference frequency; Computed from the flux densities estimated at each channel
 +
| Maximum likelihood estimate
 
|-
 
|-
|NAME || String || || Source name in union catalogue
+
| FREESCHI2
 +
| double
 +
| 8
 +
| Unitless
 +
| <math display="inline">\chi^2</math> of the maximum likelihood estimates
 +
| Reduced <math display="inline">\chi^2</math>
 
|-
 
|-
|REDSHIFT || Real*4 || || Redshift
+
|
|-
+
|
|REDSHIFT_SOURCE || Int*4 || || Source for redshift - see Note 4.
+
|
|-
+
|
|ALT_NAME  || String || || Alternative names.
+
|
 +
|
 +
|-
 +
| BKGB3000
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span><ref>Pixel <math display="inline">\approx 2.95</math> arcmin<math display="inline">^2</math></ref>
 +
| Background brightness at <math display="inline">3000</math> GHz
 +
| Average over the patch (<math display="inline">32\times32</math> pixels)
 +
|-
 +
| BKGB30001S
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness standard deviation at <math display="inline">3000</math> GHz
 +
| Standard deviation over the patch (<math display="inline">32\times32</math> pixels)
 +
|-
 +
| BKGB857
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness at <math display="inline">857</math> GHz
 +
| Average over the patch (<math display="inline">32\times32</math> pixels)
 +
|-
 +
| BKGB8571S
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness standard deviation at <math display="inline">857</math> GHz
 +
| Standard deviation over the patch (<math display="inline">32\times32</math> pixels)
 +
|-
 +
| BKGB545
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness at <math display="inline">545</math> GHz
 +
| Average over the patch (<math display="inline">32\times32</math> pixels)
 +
|-
 +
| BKGB5451S
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness standard deviation at <math display="inline">545</math> GHz
 +
| Standard deviation over the patch (<math display="inline">32\times32</math> pixels)
 +
|-
 +
| BKGB353
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness at <math display="inline">353</math> GHz
 +
| Average over the patch (<math display="inline">32\times32</math> pixels)
 
|-
 
|-
|RA_MCXC  || Real*4 || degrees || Right Ascension of the MCXC identifier.
+
| BKGB3531S
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness standard deviation at <math display="inline">353</math> GHz
 +
| Standard deviation over the patch (<math display="inline">32\times32</math> pixels)
 
|-
 
|-
|DEC_MCXC || Real*4 || degrees || Declination of the MCXC identifier.
+
| BKGBETA
 +
| double
 +
| 8
 +
| Unitless
 +
| Background spectral index (MBB); Computed from the background brightness estimated at each channel<ref>A Gaussian likelihood was created using the <math display="inline">4</math> background brightness and error bars measured at each channel.</ref>
 +
| Posterior median value
 
|-
 
|-
|YZ_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup> || Compton parameter in R500 from SZ-proxy.
+
| BKGBETAL2SB
 +
| double
 +
| 8
 +
| Unitless
 +
| Background spectral index uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 
|-
 
|-
|ERRP_YZ_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup> || Error sup. in YZ_500
+
| BKGBETAH2SB
 +
| double
 +
| 8
 +
| Unitless
 +
| Background spectral index uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 
|-
 
|-
|ERRM_YZ_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup>  || Error inf. in YZ_500
+
| BKGTEMP
 +
| double
 +
| 8
 +
| Kelvin
 +
| Background temperature (MBB)
 +
| Posterior median value
 
|-
 
|-
|M_YZ_500 || Real*4 || 10<sup>14</sup> Msol|| Derived mass estimate (M_YZ_500) from SZ proxy.
+
| BKGTL2SB
 +
| double
 +
| 8
 +
| Kelvin
 +
| Background temperature uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 
|-
 
|-
|ERRP_M_YZ_500 || Real*4 || 10<sup>14</sup> Msol || Error sup. on M_YZ_500.
+
| BKGTH2SB
 +
| double
 +
| 8
 +
| Kelvin
 +
| Background temperature uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 
|-
 
|-
|ERRM_M_YZ_500 || Real*4 || 10<sup>14</sup> Msol || Error sup. on M_YZ_500.
+
| BKGBREF
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness at the reference frequency; Estimated from the likelihood
 +
| Reference frequency is <math display="inline">857</math> GHz; Posterior median value
 
|-
 
|-
|S_X || Real*4 || erg/s/cm<sup>2</sup> || Unabsorbed X-ray flux - see Note 1.
+
| BKGBREFL2SB
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness at the reference frequency uncertainty lower boundary
 +
| Lower boundary is the marginal posterior <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
 
|-
 
|-
|ERR_S_X || Real*4 || erg/s/cm<sup>2</sup> || Error on unabsorbed X-ray flux.
+
| BKGBREFH2SB
 +
| double
 +
| 8
 +
| <span>Jy/pixel</span>
 +
| Background brightness at the reference frequency uncertainty upper boundary
 +
| Upper boundary is the marginal posterior <math display="inline">97.725\%</math> percentile (<math display="inline">+2 \sigma</math>)
 
|-
 
|-
|Y_PSX_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup> || SZ signal for PSZ clusters identified with MCXC clusters- see Note 2.
+
| BKGBETAMLIKE
 +
| double
 +
| 8
 +
| Unitless
 +
| Background spectral index (MBB)
 +
| Maximum likelihood estimate
 
|-
 
|-
|SN_PSX || Real*4 || || Signal to noise for PSZ clusters identified with MCXC clusters - see Note 3.
+
| BKGTEMPMLIKE
|}
+
| double
 
+
| 8
'''Notes'''
+
| Kelvin
# Unabsorbed X-ray flux measured in an aperture of 5 arcmin in the band [0.1-2.4] keV. The aperture is centered on the Planck position, except for candidates associated with a BSC source for which we adopt the X-ray position. For sources with <math>(S/N)_{RASS} < 1\sigma</math>, we only quote an upper limit.
+
| Background temperature (MBB)
# SZ signal re-extracted fixing the size to the X-ray size provided in the MCXC catalogue at the X-ray position, for PSZ clusters identified with MCXC clusters.
+
| Maximum likelihood estimate
# Computed in the Planck data at the X-ray position fixing the size to the X-ray size provided in the MCXC catalogue, for PSZ clusters identified with MCXC clusters.
+
|-
# Source for redshifts:
+
| BKGBREFMLIKE
    -1 : No redshift available
+
| double
      1 : MCXC updated compilation{{BibCite|Piffaretti2011}}
+
| 8
      2 : Databases NED and SIMBAD-CDS
+
| Jy
      3 : SDSS cluster catalogue{{BibCite|Wen2012}}
+
| Background brightness at the reference frequency
      4 : SDSS cluster catalogue{{BibCite|Szabo2011}}
+
| Maximum likelihood estimate
      5 : SPT{{BibCite|Vanderlinde2010}}{{BibCite|Williamson2011}}{{BibCite|Andersson2011}}{{BibCite|Plagge2010}}{{BibCite|Reichardt2013}}{{BibCite|Story2011}}{{BibCite|Song2012}}
+
|-
      6 : ACT{{BibCite|Hasselfield2013}}{{BibCite|Marriage2011}}{{BibCite|Menanteau2010}}{{BibCite|Sifon2013}}
+
| BKGCHI2
      7 : Search in SDSS galaxy catalogue from Planck Collab.
+
| double
    20 : XMM-Newton confirmation from Planck Collab.
+
| 8
    50 : ENO-imaging confirmation from Planck Collab.
+
| Unitless
    60 : WFI-imaging confirmation from Planck Collab.
+
| <math display="inline">\chi^2</math> of the maximum likelihood estimates
    65 : NTT-spectroscopic confirmation from Planck Collab.
+
| Reduced <math display="inline">\chi^2</math>
    500 : RTT-spectroscopic confirmation from Planck Collab.
+
|-
    600 : NOT-spectroscopic confirmation from Planck Collab.
+
| SNRR3000
    650 : GEMINI-spectroscopic confirmation from Planck Collab.
+
| double
    700 : ENO-spectroscopic confirmation from Planck Collab.
+
| 8
 
+
| Unitless
'''Caveats'''
+
| Signal to Noise Ratio Raw (SNRr) at <math display="inline">3000</math> GHz
 
+
| Source average brightness divided the background standard deviation brightness
The following issue was found in Feb. 2014 in R1.11 of the MMF3 catalogue: the POS_ERR field values are overestimated by a factor 3.125 on average.  This issue has been resolved in R1.12.  A corrected version of the union catalogue has also been produced (also R1.12)
+
|-
 
+
| SNRR30001S
The approximate 68% (1-sigma) confidence interval in the POS_ERR field is computed as half of the 95% (2-sigma) confidence interval. Previously this was erroneously described as a 95% confidence interval.
+
| double
 
+
| 8
</div>
+
| Unitless
 
+
| 1 <math display="inline">\sigma</math> error bar of the SNRr at <math display="inline">3000</math> GHz
</div>
+
| Source brightness error bar divided the background standard deviation brightness
 
+
|-
<hr>
+
| SNRR857
 
+
| double
== (2015) Second SZ Catalogue ==
+
| 8
 +
| Unitless
 +
| Signal to Noise Ratio Raw at <math display="inline">857</math> GHz
 +
| Source average brightness divided the background standard deviation brightness
 +
|-
 +
| SNRR8571S
 +
| double
 +
| 8
 +
| Unitless
 +
| 1 <math display="inline">\sigma</math> error bar of the SNRr at <math display="inline">857</math> GHz
 +
| Source brightness error bar divided the background standard deviation brightness
 +
|-
 +
| SNRR545
 +
| double
 +
| 8
 +
| Unitless
 +
| Signal to Noise Ratio Raw at <math display="inline">545</math> GHz
 +
| Source average brightness divided the background standard deviation brightness
 +
|-
 +
| SNRR5451S
 +
| double
 +
| 8
 +
| Unitless
 +
| 1 <math display="inline">\sigma</math> error bar of the SNRr at <math display="inline">545</math> GHz
 +
| Source brightness error bar divided the background standard deviation brightness
 +
|-
 +
| SNRR353
 +
| double
 +
| 8
 +
| Unitless
 +
| Signal to Noise Ratio Raw at <math display="inline">353</math> GHz
 +
| Source average brightness divided the background standard deviation brightness
 +
|-
 +
| SNRR3531S
 +
| double
 +
| 8
 +
| Unitless
 +
| 1 <math display="inline">\sigma</math> error bar of the SNRr at <math display="inline">353</math> GHz
 +
| Source brightness error bar divided the background standard deviation brightness
 +
|-
 +
|
 +
|
 +
|
 +
|
 +
|
 +
|
 +
|-
 +
| SRCINDEX
 +
| double
 +
| 8
 +
| Unitless
 +
| Source index
 +
|
 +
|-
 +
| SRCSEP
 +
| double
 +
| 8
 +
| Arcmin
 +
| Separation between <span class="sans-serif">BeeP</span>’s catalogue positions and PCCS2+2E’s
 +
| BEEPGLON and BEEPGLAT used
 +
|-
 +
| BEEPSRCASS
 +
| double
 +
| 8
 +
| Unitless
 +
| Index of associated source
 +
| A source can be associated with another one if there is a source within a <math display="inline">8'</math> radius with higher <span class="sans-serif">NPSNR</span>
 +
|-
 +
|
 +
|
 +
|
 +
|
 +
|
 +
|
 +
|}
 +
 
 +
</div>
 +
 
 +
==== Position and flux density correction ====
 +
 
 +
In sections B.2, B.3 and B.4 of the companion paper, it is suggested that the catalogue error bars of the source position (<span class="sans-serif">POSERR</span>) and flux density (<span class="sans-serif">SREFH2SB</span>, <span class="sans-serif">SREFL2SB</span>) estimates may be over-optimistic for objects with high <span class="sans-serif">NPSNR</span>. If a more accurate estimate of the uncertainty is desirable, then a correction must be added to the catalogue values.
 +
 
 +
===== Position correction =====
 +
 
 +
On the grounds of the suggestion in the companion paper formulas B.3 and B.7, we recommend the following correction to be added: <math display="block">\label{eq:PositionCorrection}
 +
\sigma^2_{pos} = \textsf{POSERR}^{2} + 0.00545,</math> where <span class="sans-serif">POSERR</span> must be expressed in arcmin. In the paper’s figure B.6 we show, in red and green, the effect of applying the suggested correction.
  
The Planck SZ catalogue is constructed as described in [[Compact_Source_catalogues#Planck_Sunyaev-Zeldovich_catalogue|SZ catalogue]] and in sections 2 and 3 of {{PlanckPapers|planck2014-a36}}. Three pipelines are used to detect SZ clusters: two independent implementations of the Matched Multi-Filter (MMF1 and MMF3), and PowellSnakes (PwS). The main catalogue is constructed as the union of the catalogues from the three detection methods. The completeness and reliability of the catalogues have been assessed through internal and external validation as described in section 4 of {{PlanckPapers|planck2014-a36}}.
+
===== Flux density correction =====
  
The size of a detection is given in terms of the scale size, &theta;<sub>s</sub>, and the flux is given in terms of the total integrated Comptonization parameter, Y = Y<sub>5R500</sub>. The parameters of the GNFW profile assumed by the detection pipelines are written in the headers of the catalogues. For the sake of convenience, the conversion factor from Y to Y<sub>500</sub> is also provided in the header.
+
<math display="block">\label{eq:CorrectionVar}
 +
\sigma_s \equiv \sqrt{\sigma_{cat}^2 + (c * \ln({\small \textsf{NPSNR}}))^2},</math> where <math display="inline">c</math> is one of the constants in table [[#table:CorrectionFlux|1]] and <math display="inline">\sigma_{cat}</math> can be given either by
  
The union catalogue contains the coordinates of a detection, its signal-to-noise ratio, an estimate of Y and its uncertainty, together with a summary of the validation information, including external identification of a cluster and its redshift if they are available. The pipeline from which the information is taken is called the reference pipeline. If more than one pipeline makes the same detection, the information is taken from the the pipeline that makes the most significant detection. Where the redshift is known, we provide the SZ mass for the reference pipeline.
+
<math display="inline">\frac{\textsf{SREFH2SB}-\textsf{SREFL2SB}}{4}</math>
 +
<br /> for a symmetric error bar, or<br />
 +
<math display="inline">\frac{\textsf{SREFH2SB}-\textsf{SREF}}{2}</math> and <math display="inline">\frac{\textsf{SREF}-\textsf{SREFL2SB}}{2}</math>
 +
<br /> if the non-symmetrical character of the uncertainty needs to be preserved.<br />
  
The individual catalogues contain the coordinates and the signal-to-noise ratio of the detections, and information on the size and flux of the detections. The entries are cross-referenced to the detections in the union catalogue. The full information on the degeneracy between &theta;<sub>s</sub> and Y is included in the individual catalogues in the form of the two-dimensional probability distribution for each detection. It is computed on a well-sampled grid to produce a two-dimensional image for each detection. It is provided in this form so it can be combined with a model or external data to produce tighter constraints on the parameters. The individual catalogues also contain Planck measurements of the SZ mass observable, M<sub>SZ</sub>, as calculated using a Y-M scaling relation and an assumed redshift to break the Y-&theta;<sub>s</sub> degeneracy. These are provided for each detection as functions of assumed redshift, in the range 0.01 < z < 1, along with the upper and lower 68% confidence limits.
+
Example of a symmetrical correction: Source ''PCCS2 857 G002.95+57.96'' (<span class="sans-serif">NPSNR</span><math display="inline">= 32.43</math>). <math display="block">\label{eq:SrefCorrectionNUmerical}
 +
\sigma^2_{s} =  \left(\frac{\textsf{SREFH2SB}-\textsf{SREFL2SB}}{4}\right)^2 + (0.057 * \ln(\textsf{NPSNR}))^2,</math> where we have used the correction constant for the ‘''PCCS2 region''’, <math display="inline">c= 57</math> mJy.<br />
 +
<math display="block">\sigma_{s} =  \sqrt{\left(\frac{1.22-0.71}{4}\right)^2 + (0.057 * \ln(32.43)^2} = 236 \, \textrm{mJy},</math> In figures 11 and B.7, we show, in red and blue, the effect of applying the symmetrical correction.
  
The selection function of the union catalogue, the intersection catalogue and the individual catalogues are provided in additional files. The selection function files contains the probability of detection for clusters of given intrinsic parameters &theta;<sub>500</sub> and Y<sub>500</sub>.  The file includes the definition of the survey area in the form of a HEALPix mask, and is evaluated for a range of signal-to-noise thresholds between 4.5 and 10.
+
==== Spectral Energy Density (SED) plots ====
  
=== Union catalogue ===
+
[[File:xSupPicts-COM_PCCS_857_R2_01__PCCS2_857_G171_77_59_53_s.png|500px|center|none]]
  
The union catalogue is contained in ''{{PLASingleFile|fileType=cat | name=HFI_PCCS_SZ-union_R2.08.fits | link=HFI_PCCS_SZ-union_R2.08.fits}}''.
+
<div style='text-align: center;'>Source ‘''SED plot''’, showing the SED curves for the MBB (upper panel) and Free (middle panel) models for one source (NGC 895). The background is given in the bottom panel. The yellow and red dashed curves are the median and maximum-likelihood fits, respectively. The purple and black bands are the <math display="inline">\pm1\,\sigma</math> and <math display="inline">\pm2\,\sigma</math> regions, respectively, of the full posterior density. Blue diamonds are the PCCS2+2E flux-density estimates (<span class="sans-serif">APERFLUX</span>). The green diamonds are: in the upper panel <span><code>BeeP</code></span>’s estimate of the flux density at 857 GHz, and in the middle panel <span><code>BeeP</code></span>’s Free estimates of the flux density at each frequency. In the lower panel, dark green diamonds are the background brightness estimates at each frequency, and the green curves are the maximum likelihood (dashed) and the median (solid) models. Red diamonds are the average source brightness divided by the background rms brightness in that patch, i.e., raw S/N. The data points are slightly displaced from their nominal frequencies to avoid overlaps. | Source ‘''SED plot''’, showing the SED curves for the MBB (upper panel) and Free (middle panel) models for one source (NGC 895). The background is given in the bottom panel. The yellow and red dashed curves are the median and maximum-likelihood fits, respectively. The purple and black bands are the <math display="inline">\pm1\,\sigma</math> and <math display="inline">\pm2\,\sigma</math> regions, respectively, of the full posterior density. Blue diamonds are the PCCS2+2E flux-density estimates (<span class="sans-serif">APERFLUX</span>). The green diamonds are: in the upper panel <span><code>BeeP</code></span>’s estimate of the flux density at 857 GHz, and in the middle panel <span><code>BeeP</code></span>’s Free estimates of the flux density at each frequency. In the lower panel, dark green diamonds are the background brightness estimates at each frequency, and the green curves are the maximum likelihood (dashed) and the median (solid) models. Red diamonds are the average source brightness divided by the background rms brightness in that patch, i.e., raw S/N. The data points are slightly displaced from their nominal frequencies to avoid overlaps.</div>
  
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
Another component of the catalogue is a collection of figures, one for each row, that displays the SED curves for each of the models. There are three different panels in each figure,
|- bgcolor="ffdead"  
+
 
!colspan="4" | Extension 0: Primary header, no data
+
* <span class="sans-serif">SOURCE</span>: Is the PCCS2+2E name of the source.
|- bgcolor="ffdead"  
+
* <span class="sans-serif">BEEPGLON</span> and <span class="sans-serif">BEEPGLAT</span>: Are the Galactic longitude and latitude computed by <span class="sans-serif">BeeP</span> using the MBB SED model.
! FITS Keyword || Data Type || Units || Description
+
* <span class="sans-serif">SRCSIG</span>, <span class="sans-serif">NPSNR</span> and <span class="sans-serif">EST_QUALITY</span> are the fields defining the reliability of the source and the estimation quality (see companion paper section 5.4).
|-
+
* Upper panel - MBB SED curves.<br />
|INSTRUME || String || || Instrument (HFI)
+
This figure shows the SED curves drawn from the MBB parameter samples when marginalising over all others. There is a curve for each sample drawn from <span class="sans-serif">BeeP</span>’s posterior. In purple, if the sample was inside the <math display="inline">68\%</math> HPD<ref>Highest Probability Density region (HPD). For a complete definition see .</ref> of the full posterior, otherwise in black. The golden line is drawn from the Median of the marginalised distributions and the dashed red line from the maximum likelihood solution. The green diamond is <span><code>BeeP</code></span>’s estimate of the reference flux density (at 857 GHz).<br />
|-
 
| VERSION || String || || Version of catalogue
 
|-
 
| DATE || String || || Date file created: yyyy-mm-dd
 
|-
 
| ORIGIN || String || || Name of organization responsible for the data (HFI-DPC)
 
|-
 
| TELESCOP || String || || Telescope (PLANCK)
 
|-
 
| CREATOR || String || || Pipeline version
 
|-
 
| DATE-OBS || String || || Start date of the survey: yyyy-mm-dd
 
|-
 
| DATE-END || String || || End date of the survey: yyyy-mm-dd
 
|-
 
| PROCVER || String || || Data version
 
|-
 
| PP_ALPHA || Real*4 || || GNFW pressure profile &alpha; parameter
 
|-
 
| PP_BETA || Real*4 || || GNFW pressure profile &beta; parameter
 
|-
 
| PP_GAMMA || Real*4 || || GNFW pressure profile &gamma; parameter
 
|-
 
| PP_C500 || Real*4 || || GNFW pressure profile c<sub>500</sub> parameter
 
|-
 
| PP_Y2YFH || Real*4 || || Conversion factor from Y to Y<sub>500</sub>
 
  
|- bgcolor="ffdead"  
+
* Middle panel - ‘Free’ channel amplitudes.<br />
!colspan="4" | Extension 1: BINTABLE, EXTNAME = PSZ2_UNION
+
The green diamonds are <span class="sans-serif">BeeP</span>’s posterior medians of the flux densities at each channel<ref>Sources inside the IRIS mask do not include a flux density at 3000 GHz.</ref>. The purple and black lines have the same meaning as in the upper panel but the posterior samples were drawn from fitting a MBB SED model, using a Gaussian likelihood, to the green diamonds and respective error bars. Blue diamonds are the PCCS2+2E flux-density estimates (<span class="sans-serif">APERFLUX</span>).<br />
|- bgcolor="ffdead"  
+
 
! Column Name || Data Type || Units || Description
+
* Lower panel - Background/Foreground contrast parameters.<br />
|-
+
The dark green diamonds are the background brightness estimates at each frequency. The green curves were fitted to the individual brightness estimates using a MBB model and a Gaussian likelihood just like in the case of the middle panel. The green dashed line is the maximum likelihood solution and the solid the Median. The red diamonds are <span class="sans-serif">BeeP</span>’s SNRr: Source average brightness divided by the background brightness standard deviation in that patch.
|INDEX || Int*4 || || Index used to cross-reference with individual catalogues
+
* The <span class="sans-serif">TEMP</span> and <span class="sans-serif">BETA</span> numerical parameter values, shown in all panels, are the marginalised posterior medians.
|-
+
* The <math display="inline">\chi^2</math> values are the reduced <math display="inline">\chi^2</math> of the maximum likelihood solution.
|NAME || String || || Source name (see note 1)
+
 
|-
+
==== Parameter posterior distributions (‘''corner plots''’) ====
|GLON || Real*8 || degrees || Galactic longitude
+
 
|-
+
This component of the catalogue is another collection of figures showing the MBB parameter posterior distributions of <span class="sans-serif">BeeP</span>’s likelihood in the form of a ‘''corner''’ plot (see figure [[#fig:CornerPlot|5]]).
|GLAT || Real*8 || degrees || Galactic latitude
+
 
|-
+
* <span class="sans-serif">SOURCE</span>: Is the PCCS2+2E name of the source.
|RA  || Real*8 || degrees || Right ascension (J2000) transformed from (GLON,GLAT)
+
* <span class="sans-serif">GLON</span> and <span class="sans-serif">GLAT</span>: Are the Galactic longitude and latitude in the PCCS2+2E catalogue. These are the <math display="inline">(0,0)</math> coordinates of the parameters <math display="inline">dX</math> and <math display="inline">dY</math>.
|-
+
* <span class="sans-serif">SRCSIG</span>, <span class="sans-serif">NPSNR</span> and <span class="sans-serif">EST_QUALITY</span> are the fields defining the reliability of the source and the estimation quality (see companion paper section 5.4).
|DEC || Real*8 || degrees || Declination (J2000) transformed from (GLON,GLAT)
+
* The figures in the diagonal are the marginal distributions (histogram) of each MBB parameter and the non-diagonal show the joint distribution (bi-dimensional histogram) of the row-column parameters.
 +
* Darker patterns mean higher probability density.
 +
* The vertical lines in the marginals ate the {<math display="inline">2.5, 50.0, 97.5</math>} percentiles.
 +
* The violet line is the PCCS2+2E catalogue flux density at the <math display="inline">857</math> GHz channel (<span class="sans-serif">APERFLUX</span>).
 +
 
 +
[[File:xSupPicts-COM_PCCS_857_R2_01__PCCS2_857_G171_77_59_53_c.png|500px|center|none]]
 +
 
 +
<div style='text-align: center;'>A source ‘''corner plot''’ , showing the parameter posterior distributions. This figure shows, in each non-diagonal position, the marginalised bi-dimensional posterior distribution of the parameter samples defining the row and the column. The diagonal locations contain posterior marginalized distributions. The violet line is the PCCS2+2E catalogue flux density at the <math display="inline">857</math> GHz channel. There is one of these plots for each source in <span class="sans-serif">BeeP</span>’s catalogue (<span class="sans-serif">APERFLUX</span>).</div>
 +
 
 +
</div>
 +
</div>
 +
 
 +
 
 +
<div class="toccolours" style="background-color: #FFDAB9" >
 +
<div class="toccolours" style="background-color: #FFDAB9" >
 +
 
 +
==(2015) Planck Catalogue of Galactic Cold Clumps==
 +
 
 +
The Planck Catalogue of  Galactic Cold Clumps (PGCC) is a list of 13188 Galactic sources and 54 sources located in the Small and Large Magellanic Clouds. The sources have been identified in Planck data as sources colder than their environment. The PGCC has been built using 48 months of Planck data at 857, 545, and 353 GHz, combined with the 3-THz IRAS data, as described in {{PlanckPapers | planck2014-a37}}.
 +
 
 +
The all-sky distribution of the PGCC sources is plotted below on the 857-GHz emission shown in logarithmic scale between 10<sup>-2</sup> to 10<sup>2</sup> MJy sr<sup>-1</sup>.
 +
[[File:PGCC_allsky.png|800px|thumb|center|All-sky distribution of the PGCC sources.]]
 +
 
 +
Sources are divided into three categories based on the reliability of the flux density estimates in the IRAS 3-THz and Planck 857, 545, and 353 GHz bands:
 +
* FLUX_QUALITY=1, sources with flux density estimates S/N > 1 in all bands;
 +
* FLUX_QUALITY=2, sources with flux density estimates S/N > 1 only in the 857-, 545-, and 353-GHz Planck bands, considered as very cold source candidates;
 +
* FLUX_QUALITY=3, sources without any reliable flux density estimates, listed as poor candidates.
 +
The all-sky distributions of the PGCC sources per FLUX_QUALITY category are plotted below of the 857-GHz map in grey scale, varying in logarithmically between 10<sup>-2</sup> and 10<sup>2</sup> MJy sr<sup>-1</sup>.
 +
[[File:PGCC_allsky_FQ1.png|800px|thumb|center|All-sky distribution of the PGCC sources with FLUX_QUALITY=1.]]
 +
[[File:PGCC_allsky_FQ2.png|800px|thumb|center|All-sky distribution of the PGCC sources with FLUX_QUALITY=2.]]
 +
[[File:PGCC_allsky_FQ3.png|800px|thumb|center|All-sky distribution of the PGCC sources with FLUX_QUALITY=3.]]
 +
 
 +
Distance estimates have been obtained for 5574 PGCC sources using seven different methods, as described in {{PlanckPapers | planck2014-a37}}. A flag is set to quantify the quality of the distance estimates, defined as follows:
 +
* DIST_QUALITY=0, no distance estimate;
 +
* DIST_QUALITY=1, single distance estimate;
 +
* DIST_QUALITY=2, multiple distance estimates which are consistent within 1&sigma;;
 +
* DIST_QUALITY=3, multiple distance estimates which are not consistent within 1&sigma;;
 +
* DIST_QUALITY=4, single upper limits.
 +
The all-sky distribution of sources with robust distance estimates is shown below.
 +
[[File:PGCC_allsky_DIST.png|800px|thumb|center|All-sky distribution of the  4655 PGCC sources for which a distance estimate with a DIST_QUALITY flag equal to 1 or 2 is available. The various types of distance estimates are defined as follows : kinematic (purple), optical extinction (blue), near-infrared extinction (green), molecular complex association (orange), and Herschel HKP-GCC (red). We also show the distribution of  the 664 sources with an upper-limit estimate  (DIST_QUALITY=4) provided by the near-infrared extinction method (light green). Molecular complexes are outlined with black contours.]]
 +
 
 +
The catalogue is contained in the FITS file {{PLASingleFile | fileType=cat | name=HFI_PCCS_GCC_R2.02.fits  | link=HFI_PCCS_GCC_R2.02.fits }}.
 +
Its structure is shown in the following table.
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=1000px
 +
|+ <small>'''FITS file structure'''</small>
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Identification
 +
|- bgcolor="ffdead"  
 +
! FITS Keyword || Data type || Units || Description
 
|-
 
|-
|POS_ERR || Real*4 || arcmin || Position uncertainty (95% confidence interval)
+
|NAME || String || || Source Name
 
|-
 
|-
|SNR || Real*4 || || Signal-to-noise ratio of the detection
+
|SNR || real*8 || || Maximum S/N over the 857, 545, and 353 GHz Planck cold residual maps
 
|-
 
|-
|PIPELINE || Int*4 || || Pipeline from which information is taken (reference pipeline): 1= MMF1; 2 = MMF3; 3 = PwS
+
|SNR_857 || real*8 || || S/N of the cold residual detection at 857 GHz
 
|-
 
|-
|PIPE_DET || Int*4 || || Pipelines which detect this object (see note 2)
+
|SNR_545 || real*8 || || S/N of the cold residual detection at 545 GHz
 
|-
 
|-
|PCCS2 || Bool || || Indicates whether detection matches with any in PCCS2 catalogues
+
|SNR_353 || real*8 || || S/N of the cold residual detection at 353 GHz
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Source position
 +
|- bgcolor="ffdead" 
 +
! FITS Keyword || Data type || Units || Description
 
|-
 
|-
|PSZ || Int*4 || || Index of matching detection in PSZ1, or -1 if new detection
+
|GLON || real*8 || deg || Galactic longitude based on morphology fitting
 
|-
 
|-
|IR_FLAG || Int*1 || || Flag denoting heavy infrared contamination
+
|GLAT || real*8 || deg || Galactic latitude based on morphology fitting
 
|-
 
|-
|Q_NEURAL || Real*4 || || Neural network quality flag (see note 3)
+
|RA || real*8 || deg || Right ascension (J2000) in degrees transformed from (GLON, GLAT)
 
|-
 
|-
|Y5R500 || Real*4 || 10<sup>-3</sup>&nbsp;arcmin<sup>2</sup> || Mean marginal Y<sub>5R500</sub> as determined by reference pipeline
+
|DEC || real*8 || deg || Declination (J2000) in degrees transformed from (GLON, GLAT)
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Morphology
 +
|- bgcolor="ffdead" 
 +
! FITS Keyword || Data type || Units || Description
 +
|-
 +
|GAU_MAJOR_AXIS || real*8 || arcmin || FWHM along the major axis of the elliptical Gaussian
 
|-
 
|-
|Y5R500_ERR || Real*4 || 10<sup>-3</sup>&nbsp;arcmin<sup>2</sup> || Uncertainty on Y<sub>5R500</sub> as determined by reference pipeline
+
|GAU_MAJOR_AXIS_SIG || real*8 || arcmin || 1&sigma; uncertainty on the FWHM along the major axis
 
|-
 
|-
|VALIDATION || Int*4 || || External validation status (see note 4)
+
|GAU_MINOR_AXIS || real*8 || arcmin || FWHM along the minor axis of the elliptical Gaussian
 +
|-
 +
|GAU_MINOR_AXIS_SIG || real*8 || arcmin ||  1&sigma; uncertainty on the FWHM along the minor axis
 
|-
 
|-
|REDSHIFT_ID || String || || External identifier of cluster associated with redshift measurement (see note 5)
+
|GAU_POSITION_ANGLE || real*8 || rad || Position angle of the elliptical Gaussian (see note 1)
 
|-
 
|-
|REDSHIFT || Real*4 || || Redshift of cluster (see note 5)
+
|GAU_POSITION_ANGLE_SIG || real*8 || rad || 1&sigma; uncertainty on the position angle
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Photometry
 +
|- bgcolor="ffdead" 
 +
! FITS Keyword || Data type || Units || Description
 
|-
 
|-
|MSZ || Real*4 || 10<sup>14</sup>&nbsp;M<sub>sol</sub> || SZ mass proxy (see note 6)
+
|FLUX_3000_CLUMP || real*8 || Jy || Flux density of the clump at 3 THz
 
|-
 
|-
|MSZ_ERR_UP || Real*4 || 10<sup>14</sup>&nbsp;M<sub>sol</sub> || Upper bound of 68% SZ mass proxy confidence interval (see note 6)
+
|FLUX_3000_CLUMP_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the clump at 3 THz
 
|-
 
|-
|MSZ_ERR_LOW || Real*4 || 10<sup>14</sup>&nbsp;M<sub>sol</sub> || Lower bound of 68% SZ mass proxy confidence interval (see note 6)
+
|FLUX_857_CLUMP || real*8 || Jy || Flux density of the clump at 857 GHz
 
|-
 
|-
|MCXC || String || || Identifier of X-ray counterpart in the MCXC, if one is present
+
|FLUX_857_CLUMP_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the clump at 857 GHz
 
|-
 
|-
|REDMAPPER || String || || Identifier of optical counterpart in the RedMAPPer catalogue, if one is present
+
|FLUX_545_CLUMP || real*8 || Jy || Flux density of the clump at 545 GHz
 
|-
 
|-
|ACT || String || || Identifier of SZ counterpart in the ACT catalogues, if one is present
+
|FLUX_545_CLUMP_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the clump at 545 GHz
 
|-
 
|-
|SPT || String || || Identifier of SZ counterpart in the SPT catalogues, if one is present
+
|FLUX_353_CLUMP || real*8 || Jy || Flux density of the clump at 353 GHz
 
|-
 
|-
|WISE_FLAG || Int*4 || || Confirmation flag of WISE overdensity (see note 7)
+
|FLUX_353_CLUMP_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the clump at 353 GHz
 
|-
 
|-
|AMI_EVIDENCE || Real*4 || || Bayesian evidence for AMI counterpart detection (see note 8)
+
|FLUX_3000_WBKG || real*8 || Jy || Flux density of the warm background at 3 THz (see note 2)
 
|-
 
|-
|COSMO || Bool || || Indicates whether detection is in the cosmology sample
+
|FLUX_3000_WBKG_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of warm background at 3 THz
 
|-
 
|-
|COMMENT|| String || || Comments on this detection
+
|FLUX_857_WBKG || real*8 || Jy || Flux density of the warm background at 857 GHz
|}
+
|-
 
+
|FLUX_857_WBKG_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the warm background at 857 GHz
'''Notes'''
+
|-
# Format is <tt>PSZ2 Glll.ll&plusmn;bb.b</tt> where (l,b) are the Galactic coordinates truncated to 2 decimal places.
+
|FLUX_545_WBKG || real*8 || Jy || Flux density of the warm background at 545 GHz
# The three least significant decimal digits are used to represent detection or non-detection by the pipelines. Order of the digits: hundreds = MMF1; tens = MMF3; units = PwS. If it is detected then the corresponding digit is set to 1, otherwise it is set to 0.
+
|-
# Neural network quality flag is 1-Q<sub>bad</sub>, following the definitions in Aghanim et al. 2014.
+
|FLUX_545_WBKG_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the warm background at 545 GHz
# Summary of the external validation, encoding the most robust external identification: 10 = ENO follow-up; 11 = RTT follow-up; 12 = PanSTARRs; 13 = RedMAPPer non-blind; 14 = SDSS high-z; 15 = AMI; 16 = WISE; 20 = legacy identification from the PSZ1; 21 = MCXC; 22 = SPT; 23 = ACT; 24 = RedMAPPer; 25 = legacy identification from PSZ1 with externally updated redshift; 30 = NED; -1 = no known external counterpart.
+
|-
# Redshift source is the most robust external identification listed in the VALIDATION field.
+
|FLUX_353_WBKG || real*8 || Jy || Flux density of the warm background at 353 GHz
# M<sub>SZ</sub> is the hydrostatic mass assuming the best-fit Y-M scaling relation of Arnaud 2010 as a prior. The uncertainties are statistical and based on the Planck measurement uncertainties only.  Not included in the uncertainties are the statistical errors on the scaling relation, the intrinsic scatter in the relation, or systematic errors in data selection for the scaling relation fit.
+
|-
# Assigned by visual inspection: 0 = no significant galaxy overdensity; 1 = possible galaxy overdensity; 2 = probable galaxy overdensity; 3 = significant galaxy overdensity detected; -1 = possible galaxy overdensity (affected by bright star artefacts); -2 = no significant galaxy overdensity (affected by bright star artefacts); -3 = no assessment possible (affected by bright star artefacts); -10 = not analysed.
+
|FLUX_353_WBKG_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the warm background at 353 GHz
# Defined in the paper.
+
|-
 
+
|FLUX_QUALITY || int*4 || 1-3 || Category of flux density reliability (see note 3)
=== Individual catalogues ===
+
|-
 
+
|FLUX_BLENDING || int*4 || 0/1 || 1 if blending issue with flux density estimate (see note 4)
The individual pipeline catalogues are contained in the FITS files
+
|-
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-MMF1_R2.08.fits  | link=HFI_PCCS_SZ-MMF1_R2.08.fits }} (MMF1 pipeline)
+
|FLUX_BLENDING_IDX || int*8 || || Catalogue index of the closest source responsible for blending
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-MMF3_R2.08.fits  | link=HFI_PCCS_SZ-MMF3_R2.08.fits }} (MMF3 pipeline)
+
|-
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-PwS_R2.08.fits  | link=HFI_PCCS_SZ-PwS_R2.08.fits }} (PowellSnakes pipeline)
+
|FLUX_BLENDING_ANG_DIST || real*8 || arcmin || Angular distance to the closest source responsible for blending
 
+
|-
Their structure is as follows:
+
|FLUX_BLENDING_BIAS_3000 || real*8 || % || Relative bias of the flux density at 3 THz due to blending
 
+
|-
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
|FLUX_BLENDING_BIAS_857 || real*8 ||  % || Relative bias of the flux density at 857 GHz due to blending
|+ '''FITS file structure'''
+
|-
|- bgcolor="ffdead" 
+
|FLUX_BLENDING_BIAS_545 || real*8 || % || Relative bias of the flux density at 545 GHz due to blending
! colspan="4" | Extension 0: Primary header, no data
 
|- bgcolor="ffdead" 
 
! FITS Keyword || Data Type || Units || Description
 
 
|-  
 
|-  
|INSTRUME || String || || Instrument (HFI)
+
|FLUX_BLENDING_BIAS_353 || real*8 || % || Relative bias of the flux density at 353 GHz due to blending
|-
+
|- bgcolor="ffdead" 
| VERSION || String || || Version of catalogue
+
! colspan="4" | Distance
|-
+
|- bgcolor="ffdead" 
| DATE || String || || Date file created: yyyy-mm-dd
+
! FITS Keyword || Data type || Units || Description
|-
+
|-
| ORIGIN || String || || Name of organization responsible for the data (HFI-DPC)
+
|DIST_KINEMATIC || real*8 || kpc || Distance estimate [1] using kinematics
|-  
+
|-
| TELESCOP || String || || Telescope (PLANCK)
+
|DIST_KINEMATIC_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [1] using kinematics
|-  
+
|-
| CREATOR || String || || Pipeline version
+
|DIST_OPT_EXT_DR7 || real*8 || kpc || Distance estimate [2] using optical extinction on SDSS DR7
|-  
+
|-
| DATE-OBS || String || || Start time of the survey: yyyy-mm-dd
+
|DIST_OPT_EXT_DR7_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [2] using optical extinction on SDSS DR7
|-
+
|-
| DATE-END || String || || End time of the survey: yyyy-mm-dd
+
|DIST_OPT_EXT_DR9 || real*8 || kpc || Distance estimate [3] using optical extinction on SDSS DR9
|-  
 
| PROCVER || String || || Data version
 
|-
 
| PP_ALPHA || Real*4 || || GNFW pressure profile &alpha; parameter
 
|-  
 
| PP_BETA || Real*4 || || GNFW pressure profile &beta; parameter
 
|-  
 
| PP_GAMMA || Real*4 || || GNFW pressure profile &gamma; parameter
 
|-
 
| PP_C500 || Real*4 || || GNFW pressure profile c<sub>500</sub> parameter
 
|-  
 
| PP_Y2YFH || Real*4 || || Conversion factor from Y to Y<sub>500</sub>
 
 
 
|- bgcolor="ffdead" 
 
! colspan="4" | Extension 1: BINTABLE, EXTNAME = PSZ2_INDIVIDUAL
 
|- bgcolor="ffdead" 
 
! Column Name || Data Type || Units || Description
 
 
|-
 
|-
|INDEX || Int*4 || || Index from union catalogue
+
|DIST_OPT_EXT_DR9_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [3] using optical extinction on SDSS DR9
 
|-
 
|-
|NAME || String || || Source name (see note 1)
+
|DIST_NIR_EXT_IRDC || real*8 || kpc || Distance estimate  [4] using near-IR extinction towards IRDCs
 
|-
 
|-
|GLON || Real*8 || degrees || Galactic longitude
+
|DIST_NIR_EXT_IRDC_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate  [4] using near-IR extinction towards IRDCs
 
|-
 
|-
|GLAT || Real*8 || degrees || Galactic latitude
+
|DIST_NIR_EXT || real*8 || kpc || Distance estimate [5] using near-IR extinction
 
|-
 
|-
|RA  || Real*8 || degrees || Right ascension (J2000) transformed from (GLON, GLAT)
+
|DIST_NIR_EXT_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [5] using near-IR extinction
 
|-
 
|-
|DEC  || Real*8 || degrees || Declination (J2000) transformed from (GLON, GLAT)
+
|DIST_MOLECULAR_COMPLEX || real*8 || kpc || Distance estimate [6] using molecular complex association
 
|-
 
|-
|POS_ERR || Real*4 || arcmin || Position uncertainty (95% confidence interval)
+
|DIST_MOLECULAR_COMPLEX_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [6] using molecular complex association
 
|-
 
|-
|SNR || Real*4 || || Signal-to-noise ratio of detection
+
|DIST_HKP_GCC || real*8 || kpc || Distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
 
|-
 
|-
|TS_MIN || Real*4 || || Minimum value of &theta;<sub>s</sub> in grid in second extension HDU (see note 2)
+
|DIST_HKP_GCC_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
 
|-
 
|-
|TS_MAX || Real*4 || || Maximum value of &theta;<sub>s</sub> in grid in second extension HDU (see note 2)
+
|DIST_OPTION || int*4 || 0-7 || Option of the best distance estimate used in other physical properties
 +
|-
 +
|DIST_QUALITY || int*4 || 0-4 || Quality flag of the consistency between distance estimates (see note 5)
 +
|-
 +
|DIST || real*8 || kpc || Best distance estimate used for further physical properties
 +
|-
 +
|DIST_SIG || real*8 || kpc || 1&sigma; uncertainty on the best distance estimate
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Temperature
 +
|- bgcolor="ffdead" 
 +
! FITS Keyword || Data type || Units || Description
 +
|-
 +
|TEMP_CLUMP || real*8 || K || Temperature of the clump with &beta; as a free parameter
 +
|-
 +
|TEMP_CLUMP_SIG || real*8 || K || 1&sigma; uncertainty on the clump temperature with &beta; free
 +
|-
 +
|TEMP_CLUMP_LOW1 || real*8 || K || Lower 68% confidence limit of the clump temperature with &beta; free
 +
|-
 +
|TEMP_CLUMP_UP1 || real*8 || K || Upper 68% confidence limit of the clump temperature with &beta; free
 +
|-
 +
|BETA_CLUMP || real*8 || || Spectral index &beta; of the clump
 +
|-
 +
|BETA_CLUMP_SIG || real*8 || || 1&sigma; uncertainty (from MCMC) on the emissivity spectral index &beta; of the clump
 +
|-
 +
|BETA_CLUMP_LOW1 || real*8 || || Lower 68% confidence limit of the emissivity spectral index &beta; of the clump
 +
|-
 +
|BETA_CLUMP_UP1 || real*8 || || Upper 68% confidence limit of the emissivity spectral index &beta; of the clump
 
|-
 
|-
|Y_MIN || Real*4 || || Minimum value of Y in grid in second extension HDU (see note 2)
+
|TEMP_BETA2_CLUMP || real*8 || K || Temperature of the clump with &beta; = 2
 
|-
 
|-
|Y_MAX || Real*4 || || Maximum value of Y in grid in second extension HDU (see note 2)
+
|TEMP_BETA2_CLUMP_SIG || real*8 || K || 1&sigma; uncertainty on the temperature of the clump with &beta; = 2
|- bgcolor="ffdead" 
+
|-
! Keyword || Data Type || Value || Description
+
|TEMP_BETA2_CLUMP_LOW1 || real*8 || K || Lower 68% confidence limit of the clump temperature with &beta; = 2
|-  
+
|-
| PIPELINE || String || || Name of detection pipeline
+
|TEMP_BETA2_CLUMP_UP1 || real*8 || K || Upper 68% confidence limit of the clump temperature with &beta; = 2
 
+
|-
|- bgcolor="ffdead" 
+
|TEMP_WBKG || real*8 || K || Temperature of the warm background with &beta; as a free parameter (see note 6)
! colspan="4" | Extension 2: IMAGE, EXTNAME = PSZ2_PROBABILITY (see note 2)
+
|-
|- bgcolor="ffdead" 
+
|TEMP_WBKG_SIG || real*8 || K || 1&sigma; dispersion of the warm background temperature with &beta; free
! Keyword || Data Type || Value || Description
+
|-
|-  
+
|TEMP_WBKG_LOW1 || real*8 || K || Lower 68% confidence limit of the warm background temperature with &beta; free
| NAXIS1 || Integer || 256 || Dimension 1
+
|-
|-  
+
|TEMP_WBKG_UP1 || real*8 || K || Upper 68% confidence limit of the warm background temperature with &beta; free
| NAXIS2 || Integer || 256 || Dimension 2
+
|-
|-  
+
|BETA_WBKG || real*8 || || Spectral index &beta; of the warm background (see note 6)
| NAXIS3 || Integer || N<sub>det</sub> || Dimension 3 = Number of detections
+
|-
|- bgcolor="ffdead" 
+
|BETA_WBKG_SIG || real*8 || || 1&sigma; uncertainty (from MCMC) of the emissivity spectral index &beta; of the warm background
! Keyword || Data Type || Value || Description
+
|-
|-  
+
|BETA_WBKG_LOW1 || real*8 || || Lower 68% confidence limit of the emissivity spectral index &beta; of the warm background
| PIPELINE || String || || Name of detection pipeline
+
|-
 
+
|BETA_WBKG_UP1 || real*8 || || Upper 68% confidence limit of the emissivity spectral index &beta; of the warm background
|- bgcolor="ffdead"
+
|-
! colspan="4" | Extension 3: IMAGE, EXTNAME = PSZ2_MSZ_ARRAY (see note 3)
+
|TEMP_BETA2_WBKG || real*8 || K || Temperature of the warm background with &beta; = 2
|- bgcolor="ffdead" 
+
|-
! Keyword || Data Type || Value || Description
+
|TEMP_BETA2_WBKG_SIG || real*8 || K || 1&sigma; uncertainty on the temperature of the warm background with &beta; = 2
|-  
+
|-
| NAXIS1 || Integer || 100 || Dimension 1
+
|TEMP_BETA2_WBKG_LOW1 || real*8 || K || Lower 68% confidence limit of the warm background temperature with &beta; = 2
|-  
+
|-
| NAXIS2 || Integer || 4 || Dimension 2  
+
|TEMP_BETA2_WBKG_UP1 || real*8 || K || Upper 68% confidence limit of the warm background temperature with &beta; = 2
|-  
+
|- bgcolor="ffdead" 
| NAXIS3 || Integer || N<sub>det</sub> || Dimension 3 = Number of detections
+
! colspan="4" | Physical properties
 
+
|- bgcolor="ffdead"
|- bgcolor="ffdead"  
+
! FITS Keyword || Data type || Units || Description
! Keyword || Data Type || Value || Description
+
|-
|-  
+
|NH2 || real*8 || cm<sup>-2</sup> || Column density <i>N</i><sub>H<sub>2</sub></sub> of the clump
| PIPELINE || String || || Name of detection pipeline
+
|-
|}
+
|NH2_SIG || real*8 || cm<sup>-2</sup> || 1&sigma; uncertainty on the column density
 
+
|-
 
+
|NH2_LOW[1,2,3] || real*8 || cm<sup>-2</sup> || Lower 68%, 95%, and 99% confidence limit of the column density
'''Notes'''
+
|-
# Format <tt>PSZ2 Glll.ll&plusmn;bb.bb</tt> where (l, b) are the Galactic coordinates truncated to 2 decimal places.
+
|NH2_UP[1,2,3]  || real*8 || cm<sup>-2</sup> || Upper 68%, 95%, and 99% confidence limit of the column density
# Extension 2 contains a three-dimensional image with the two-dimensional probability distribution in &theta;<sub>s</sub> and Y for each detection. The probability distributions are evaluated on a 256 &times; 256 linear grid between the limits specified in extension 1. The limits are determined independently for each detection. The dimension of the 3D image is 256 &times; 256 &times; N<sub>det</sub>, where N<sub>det</sub> is the number of detections.  The first dimension is &theta;<sub>s</sub> and the second dimension is Y.
+
|-
# Extension 3 contains a three-dimensional image with the information on the M<sub>SZ</sub> observable per cluster as a function of assumed redshift. The image dimensions are 100 &times; 4 &times; N<sub>det</sub>, where N<sub>det</sub> is the number of detections. The first dimension is the assumed redshift. The second dimension has size 4: the first element is the assumed redshift value corresponding to the M<sub>SZ</sub> values. The second element is the M<sub>SZ</sub> lower 68% confidence bound, the third element is the M<sub>SZ</sub> estimate and the fourth element is the M<sub>SZ</sub> upper 68% confidence bound, all in units of 10<sup>14</sup>&nbsp;M<sub>sol</sub>. These uncertainties are based on the Planck measurement uncertainties only. Not included in the error estimates are the statistical errors on the scaling relation, the intrinsic scatter in the relation, or systematic errors in data selection for the scaling relation fit.
+
|MASS || real*8 || <i>M</i><sub>&#9737;</sub> || Mass estimate of the clump
 
+
|-
=== Selection function ===
+
|MASS_SIG  || real*8 || <i>M</i><sub>&#9737;</sub> || 1&sigma; uncertainty on the mass estimate of the clump
 
+
|-
The selection function for the union, intersection and individual pipeline catalogues are contained in the FITS files:
+
|MASS_LOW[1,2,3]  || real*8 || <i>M</i><sub>&#9737;</sub> || Lower 68%, 95%, and 99% confidence limit of the mass estimate
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-union-survey_R2.08.fits  | link=HFI_PCCS_SZ-selfunc-union-survey_R2.08.fits }} (union catalogue, survey mask)
+
|-
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-union-cosmolog_R2.08.fits  | link=HFI_PCCS_SZ-selfunc-union-cosmology_R2.08.fits }} (union catalogue, cosmology mask)
+
|MASS_UP[1,2,3]  || real*8 || <i>M</i><sub>&#9737;</sub> || Upper 68%, 95%, and 99% confidence limit of the mass estimate
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-intersec-survey_R2.08.fits  | link=HFI_PCCS_SZ-selfunc-intersec-survey_R2.08.fits }} (intersection catalogue, survey mask)
+
|-
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-intersec-cosmolog_R2.08.fits  | link=HFI_PCCS_SZ-selfunc-intersec-cosmolog_R2.08.fits }} (intersection catalogue, cosmology mask)
+
|DENSITY || real*8 || cm<sup>-3</sup> || Mean density of the clump
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-MMF1-survey_R2.08.fits  | link=HFI_PCCS_SZ-selfunc-MMF1-survey_R2.08.fits }} (MMF1 catalogue, survey mask)
+
|-
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-MMF1-cosmolog_R2.08.fits | link=HFI_PCCS_SZ-selfunc-MMF1-cosmolog_R2.08.fits }} (MMF1 catalogue, cosmology mask)
+
|DENSITY_SIG  || real*8 || cm<sup>-3</sup> || 1&sigma; uncertainty on the mean density estimate of the clump
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-MMF3-survey_R2.08.fits  | link=HFI_PCCS_SZ-selfunc-MMF3-survey_R2.08.fits }} (MMF3 catalogue, survey mask)
+
|-
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-MMF3-cosmolog_R2.08.fits  | link=HFI_PCCS_SZ-selfunc-MMF3-cosmolog_R2.08.fits }} (MMF3 catalogue, cosmology mask)
+
|DENSITY_LOW[1,2,3]  || real*8 || cm<sup>-3</sup> || Lower 68%, 95%, and 99% confidence limit of the mean density estimate
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-PwS-survey_R2.08.fits | link=HFI_PCCS_SZ-selfunc-PwS-survey_R2.08.fits }} (PowellSnakes catalogue, survey mask)
+
|-
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-selfunc-PwS-cosmolog_R2.08.fits  | link=HFI_PCCS_SZ-selfunc-PwS-cosmolog_R2.08.fits }} (PowellSnakes catalogue, cosmology mask)
+
|DENSITY_UP[1,2,3|| real*8 || cm<sup>-3</sup> || Upper 68%, 95%, and 99% confidence limit of the mean density estimate
 
+
|-
Their structure is as follows:
+
|SIZE || real*8 || pc || Physical size of the clump
 
+
|-
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
|SIZE_SIG  || real*8 || pc  || 1&sigma; uncertainty on the physical size estimate of the clump
|+ '''FITS file structure'''
+
|-
|- bgcolor="ffdead" 
+
|SIZE_LOW[1,2,3]  || real*8 || pc  || Lower 68%, 95%, and 99% confidence limit of the physical size estimate
! colspan="4" | Extension 0: Primary header, no data
+
|-
|- bgcolor="ffdead" 
+
|SIZE_UP[1,2,3]  || real*8 || pc || Upper 68%, 95%, and 99% confidence limit of the physical size estimate
! FITS Keyword || Data Type || Units || Description
+
|-
|-  
+
|LUMINOSITY || real*8 || <i>L</i><sub>&#9737;</sub> || Luminosity of the clump
|INSTRUME || String || || Instrument (HFI)
+
|-
|-  
+
|LUMINOSITY_SIG  || real*8 || <i>L</i><sub>&#9737;</sub> || 1&sigma; uncertainty on the luminosity estimate of the clump
| VERSION || String || || Version of catalogue
+
|-
|-  
+
|LUMINOSITY_LOW[1,2,3]  || real*8 || <i>L</i><sub>&#9737;</sub>  || Lower 68%, 95%, and 99% confidence limit of the luminosity estimate
| DATE || String || || Date file created: yyyy-mm-dd
+
|-
|-  
+
|LUMINOSITY_UP[1,2,3]  || real*8 || <i>L</i><sub>&#9737;</sub> || Upper 68%, 95%, and 99% confidence limit of the luminosity estimate
| ORIGIN || String || || Name of organization responsible for the data (HFI-DPC)
+
|- bgcolor="ffdead" 
|-  
+
! colspan="4" | Flags
| TELESCOP || String || || Telescope (PLANCK)
+
|- bgcolor="ffdead" 
|-  
+
! FITS Keyword || Data type || Units || Description
| CREATOR || String || || Pipeline version
+
|-
|-  
+
|XFLAG_LMC || int*4 || 0/1 || 1 if part of the LMC
| DATE-OBS || String || || Start time of the survey: yyyy-mm-dd
+
|-
|-  
+
|XFLAG_SMC || int*4 || 0/1 || 1 if part of the SMC
| DATE-END || String || || End time of the survey: yyyy-mm-dd
+
|-
|-  
+
|XFLAG_ECC || int*4 || 0/1 || 1 if present in the ECC
| PROCVER || String || || Data version
 
|-  
 
| JOIN || String || || Join type (UNION, INTERSEC, MMF1, MMF3, PwS)
 
|-  
 
| MASK || String || || Mask name (SURVEY, COSMOLOG)
 
 
 
|- bgcolor="ffdead" 
 
! colspan="4" | Extension 1: BINTABLE, HEALPix map (see note 1)
 
|- bgcolor="ffdead" 
 
! FITS keyword || Data Type || Value || Description
 
 
|-
 
|-
|PIXTYPE || String || HEALPIX || HEALPix pixelation
+
|XFLAG_PCCS_857 || int*4 || 0/1 || 1 if present in the PCCS 857 GHz band
 
|-
 
|-
|ORDERING || String || RING || Pixel ordering
+
|XFLAG_PCCS_545 || int*4 || 0/1 || 1 if present in the PCCS 545 GHz band
 
|-
 
|-
|NSIDE || Int*4 || 2048 || HEALPix resolution parameter
+
|XFLAG_PCCS_353 || int*4 || 0/1 || 1 if present in the PCCS 353 GHz band
 
|-
 
|-
|NPIX ||Int*4 || 50331648 || Number of pixels
+
|XFLAG_PCCS_217 || int*4 || 0/1 || 1 if present in the PCCS 217 GHz band
 
|-
 
|-
|COORDSYS || String || G || Coordinate system
+
|XFLAG_PCCS_143 || int*4 || 0/1 || 1 if present in the PCCS 143 GHz band
 +
|-
 +
|XFLAG_PCCS_100 || int*4 || 0/1 || 1 if present in the PCCS 100 GHz band
 +
|-
 +
|XFLAG_PCCS_70 || int*4 || 0/1 || 1 if present in the PCCS 70 GHz band
 +
|-
 +
|XFLAG_PCCS_44 || int*4 || 0/1 || 1 if present in the PCCS 44 GHz band
 +
|-
 +
|XFLAG_PCCS_30 || int*4 || 0/1 || 1 if present in the PCCS 30 GHz band
 +
|-
 +
|XFLAG_PSZ || int*4 || 0/1 || 1 if present in the PCCS PSZ
 +
|-
 +
|XFLAG_PHZ || int*4 || 0/1 || 1 if present in the PCCS HZ
 +
|-
 +
|XFLAG_HKP_GCC || int*4 || 0/1 || 1 if present in the Herschel HKP-GCC
 +
 
 +
|}
 +
 
 +
 
 +
'''Notes'''
 +
# 1: The position angle of the 2D ellipse is defined as the angle between the axis parallele to the Galactic plane and the major axis, measured clockwise.
 +
# 2: The warm background flux densities are computed using the same solid angle as for the clump flux densities, but on the warm conponent map.
 +
# 3: See text above for a full description of the FLUX_QUALITY flag, for which "1" is best.
 +
# 4: This relative bias due to blending provides a rough estimate of the factor that should be applied to the clump flux densities to obtain a corrected estimate. It has been completed using on a very simple modelling of clump morphologies and the local environment. It therefore should be used with caution.
 +
# 5: See text above for a full description of the DIST_QUALITY flag.
 +
# 6: Temperature and spectral index of the warm background are based on the warm background flux density estimates obtained on the same solid angle used for the clumps
 +
 
 +
 
 +
==(2015) Planck list of high-redshift source candidates==
 +
 
 +
The Planck list of high-redshift source candidates (PHZ) is a list of 2151 sources located in the cleanest 26% of the sky and identified as point sources
 +
exhibiting an excess in the submillimetre compared to their environment. It has been built using the 48 months ofPlanck data at 857, 545, 353, and 217 GHz, combined with the 3-THz IRAS data, as described in {{PlanckPapers | planck2015-XXXIX}}. These sources are considered as high-z source candidates (z>1.5-2), given the very low contamination by Galactic cirrus, and their typical colour-colour ratios. A subsample of the PHZ list has already been followed-up with Herschel, and chararcterized as overdensities of red galaxies for more than 93% of the population, and as strongly lensed galaxies in 3% of the cases, as detailed in {{PlanckPapers | planck2014-XXVIII}}.
 +
 
 +
The all-sky distribution of the PHZ sources is shown below on an orthographic projection.
 +
[[File:PHZ_allsky.png|800px|thumb|center|All-sky distribution of the 2151 PHZ sources in orthographic projection.]]
  
|- bgcolor="ffdead" 
 
! colspan="4" | Extension 2: IMAGE, EXTNAME = SELFUNC (see note 2)
 
|- bgcolor="ffdead" 
 
! Keyword || Data Type || Value || Description
 
|-
 
| NAXIS1 || Integer || 30 || Dimension 1
 
|-
 
| NAXIS2 || Integer || 32 || Dimension 2
 
|-
 
| NAXIS3 || Integer || 12 || Dimension 3
 
|- bgcolor="ffdead" 
 
! Keyword || Data Type || Value || Description
 
|-
 
| AXIS1 || String || CY500 || Name of axis 1
 
|-
 
| AXIS2 || String || T500 || Name of axis 2
 
|-
 
| AXIS3 || String || SNRCUT || Name of axis 3
 
|-
 
| UNITS || String || PERCENT || Units of selection function
 
|-
 
| COMPTYPE || String || DIFF || Type of selection function (differential)
 
  
|- bgcolor="ffdead"
+
The PHz source list is contained in the FITS file {{PLASingleFile | fileType=cat | name=HFI_PCCS_HZ_R2.00.fits  | link=HFI_PCCS_HZ_R2.00.fits }}.
! colspan="4" | Extension 3: IMAGE, EXTNAME = YGRID (see note 3)
+
Its structure is as follows.
|- bgcolor="ffdead" 
 
! Keyword || Data Type || Value || Description
 
|-
 
| NAXIS1 || Integer || 30 || Dimension 1
 
|- bgcolor="ffdead" 
 
! Keyword || Data Type || Value || Description
 
|-
 
| COL1 || String || CY500 || Grid values of Y<sub>500</sub>
 
  
|- bgcolor="ffdead"
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=1000px
! colspan="4" | Extension 4: IMAGE, EXTNAME = TGRID (see note 4)
+
|+ '''FITS file structure'''
|- bgcolor="ffdead"  
+
|- bgcolor="ffdead"
! Keyword || Data Type || Value || Description
+
! colspan="4" | Identification
|-  
+
|- bgcolor="ffdead"
| NAXIS1 || Integer || 32 || Dimension 1
+
! FITS Keyword || Data type || Units || Description
|- bgcolor="ffdead"  
+
|-
! Keyword || Data Type || Value || Description
+
|NAME || String || || Source name
|-  
+
|-
| COL1 || String || T500 || Grid values of &theta;<sub>500</sub>
+
|SNR_X545 || real*8 || || S/N in the 545 GHz excess map
 
+
|-
|- bgcolor="ffdead"
+
|SNR_D857 || real*8 || || S/N in the 857 GHz cleaned map
! colspan="4" | Extension 5: IMAGE, EXTNAME = SNR_THRESH (see note 5)
+
|-
|- bgcolor="ffdead"  
+
|SNR_D545 || real*8 || || S/N in the 545 GHz cleaned map
! Keyword || Data Type || Value || Description
+
|-
|-  
+
|SNR_D353 || real*8 || || S/N in the 353 GHz cleaned map
| NAXIS1 || Integer || 12 || Dimension 1
+
|- bgcolor="ffdead" 
|- bgcolor="ffdead"  
+
! colspan="4" | Source position
! Keyword || Data Type || Value || Description
+
|- bgcolor="ffdead"
|-  
+
! FITS Keyword || Data type || Units || Description
| COL1 || String || S/N || Grid values of S/N threshold
+
|-
 
+
|GLON || real*8 || deg || Galactic longitude based on morphology fitting
|}
+
|-
 
+
|GLAT || real*8 || deg || Galactic latitude based on morphology fitting
'''Notes'''
+
|-
# Extension 1 contains a mask defining the survey region, given by an N<sub>side</sub> = 2048 ring-ordered HEALPix map in GALACTIC coordinates. Pixels in the survey region have the value 1.0 while pixels outside of the survey region have value 0.0.
+
|RA || real*8 || deg || Right ascension (J2000) in degrees transformed from (GLON, GLAT)
# Extension 2 contains a three-dimensional image containing the survey completeness probability distribution for various S/N thresholds. The information is stored in an image of size 30 &times; 32 &times; 12. The first dimension is Y<sub>500</sub>, the second dimension is &theta;<sub>500</sub> and the third dimension is the signal-to-noise threshold. The units are percent and lie in the range 0-100 and denote the detection probability of a cluster in the given (Y<sub>500</sub>, &theta;<sub>500</sub>) bin.
+
|-
# Extension 3 contains the Y<sub>500</sub> grid values for the completeness data cube in the second extension. It has length 30 and spans the range from 1.12480 &times; 10<sup>-4</sup> arcmin<sup>2</sup> to 7.20325 &times; 10<sup>-2</sup> arcmin<sup>2</sup> in logarithmic steps.
+
|DEC || real*8 || deg || Declination (J2000) in degrees transformed from (GLON, GLAT)
# Extension 4 contains the θ<sub>500</sub> grid values for the completeness data cube in the second extension. It has length 32 and spans the range from 0.9416 arcmin to 35.31 arcmin in logarithmic steps.
+
|- bgcolor="ffdead"
# Extension 5 contains the signal-to-noise threshold grid values for the completeness data cube in the second extension. It has length 12 and contains thresholds from 4.5 to 10.0 in steps of 0.5.
+
! colspan="4" | Morphology
 
+
|- bgcolor="ffdead"
<div class="toccolours mw-collapsible mw-collapsed" style="width:800px">
+
! FITS Keyword || Data type || Units || Description
'''Second Planck Release (2013): Description of the Planck SZ Catalogue'''
+
|-
<div class="mw-collapsible-content">
+
|GAU_MAJOR_AXIS || real*8 || arcmin || FWHM along the major axis of the elliptical Gaussian
 
+
|-
The Planck SZ catalogue is constructed as described in [[Compact_Source_catalogues#Planck_Sunyaev-Zeldovich_catalogue|SZ catalogue]] and in section 2 of {{PlanckPapers|planck2013-p05a}}.
+
|GAU_MAJOR_AXIS_SIG || real*8 || arcmin || 1&sigma; uncertainty on the FWHM along the major axis
 
+
|-
Three pipelines are used to detect SZ clusters: two independent implementations of the Matched Multi-Filter (MMF1 and MMF3), and PowellSnakes (PwS). The main catalogue is constructed as the union of the catalogues from the three detection methods. The individual catalogues are provided for the expert user in order to assess the consistency of the pipelines. The completeness and reliability of the catalogues have been assessed through internal and external validation as described in sections 3-6 of {{PlanckPapers|planck2013-p05a}}.
+
|GAU_MINOR_AXIS || real*8 || arcmin ||  FWHM along the minor axis of the elliptical Gaussian
 
+
|-
The union catalogue contains the coordinates and the signal-to-noise ratio of the detections and a summary of the external validation information, including external identification of a cluster and its redshift if it is available.
+
|GAU_MINOR_AXIS_SIG || real*8 || arcmin ||  1&sigma; uncertainty on the FWHM along the minor axis
 
+
|-
The individual catalogues contain the coordinates and the signal-to-noise ratio of the detections, and information on the size and flux of the detections. The entries are cross-referenced to the detections in the union catalogue.
+
|GAU_POSITION_ANGLE || real*8 || rad || Position angle of the elliptical Gaussian (see note 1)
 
+
|-
The size of a detection is given in terms of the scale size, $\theta_\mathrm{s}$, and the flux is given in terms of the total integrated Comptonization parameter, $Y = Y_{5r_{500}}$. The parameters of the GNFW profile assumed by the detection pipelines is written in the headers in the catalogues. For the sake of convenience, the conversion factor from $Y$ to $Y_{500}$ is also written in the header.
+
|GAU_POSITION_ANGLE_SIG || real*8 || rad || 1&sigma; uncertainty on the position angle
 
+
|- bgcolor="ffdead"
The full information on the degeneracy between $\theta_\mathrm{s}$ and $Y$ is included in the individual catalogues in the form of the two-dimensional probability distribution for each detection. It is computed on a well-sampled grid to produce a two-dimensional image for each detection. The degeneracy information is provided in this form so it can be combined with a model or external data to produce tighter constraints on the parameters.
+
! colspan="4" | Photometry
 
+
|- bgcolor="ffdead" 
 
+
! FITS Keyword || Data type || Units || Description
 
+
|-
==(2015) Planck Catalogue of Galactic Cold Clumps==
+
|FLUX_CLEAN_857 || real*8 || Jy || Flux density of the clump at 857 GHz
 
+
|-
The Planck Catalogue of Galactic Cold Clumps (PGCC) is a list of 13188 Galactic sources and 54 sources located in the Small and Large Magellanic Clouds. The sources have been identified in Planck data as sources colder than their environment. It has been buit using the 48 months Planck data at 857, 545, and 353 GHz combined with the 3 THz IRAS data, as it is described in {{PlanckPapers | planck2014-a37}}.
+
|FLUX_CLEAN_857_SIG_SKY || real*8 || Jy || 1&sigma; uncertainty at 857 GHz due to sky confusion
 +
|-
 +
|FLUX_CLEAN_857_SIG_DATA || real*8 || Jy || 1&sigma; uncertainty at 857 GHz due to measurement error
 +
|-
 +
|FLUX_CLEAN_857_SIG_GEOM || real*8 || Jy || 1&sigma; uncertainty at 857 GHz due to elliptical Gaussian fit accuracy
 +
|-
 +
|FLUX_CLEAN_545 || real*8 || Jy || Flux density of the clump at 545 GHz
 +
|-
 +
|FLUX_CLEAN_545_SIG_SKY || real*8 || Jy || 1&sigma; uncertainty at 545 GHz due to sky confusion
 +
|-
 +
|FLUX_CLEAN_545_SIG_DATA || real*8 || Jy || 1&sigma; uncertainty at 545 GHz due to measurement error
 +
|-
 +
|FLUX_CLEAN_545_SIG_GEOM || real*8 || Jy || 1&sigma; uncertainty at 545 GHz due to elliptical Gaussian fit accuracy
 +
|-
 +
|FLUX_CLEAN_353 || real*8 || Jy || Flux density of the clump at 353 GHz
 +
|-
 +
|FLUX_CLEAN_353_SIG_SKY || real*8 || Jy || 1&sigma; uncertainty at 353 GHz due to sky confusion
 +
|-
 +
|FLUX_CLEAN_353_SIG_DATA || real*8 || Jy || 1&sigma; uncertainty at 353 GHz due to measurement error
 +
|-
 +
|FLUX_CLEAN_353_SIG_GEOM || real*8 || Jy || 1&sigma; uncertainty at 353 GHz due to elliptical Gaussian fit accuracy
 +
|-
 +
|FLUX_CLEAN_217 || real*8 || Jy || Flux density of the clump at 217 GHz
 +
|-
 +
|FLUX_CLEAN_217_SIG_SKY || real*8 || Jy || 1&sigma; uncertainty at 217 GHz due to sky confusion
 +
|-
 +
|FLUX_CLEAN_217_SIG_DATA || real*8 || Jy || 1&sigma; uncertainty at 217 GHz due to measurement error
 +
|-
 +
|FLUX_CLEAN_217_SIG_GEOM || real*8 || Jy || 1&sigma; uncertainty at 217 GHz due to elliptical Gaussian fit accuracy
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Physical Properties
 +
|- bgcolor="ffdead" 
 +
! FITS Keyword || Data type || Units || Description
 +
|-
 +
|PROB_COLCOL || real*8 ||  || Colour-colour selection probability
 +
|-
 +
|EBV_MEAN || real*8 ||  || Mean extinction <i>E</i>(<i>B</i> − <i>V</i>)<sub>xgal</sub> within the source PSF
 +
|-
 +
|EBV_APER || real*8 ||  || Aperture estimate of the extinction <i>E</i>(<i>B</i> <i>V</i>)<sub>xgal</sub> within the source PSF
 +
|-
 +
|EBV_APER_SIG || real*8 ||  || 1&sigma; uncertainty of the aperture extinction <i>E</i>(<i>B</i> <i>V</i>)<sub>xgal</sub> within the source PSF
 +
|-
 +
|ZPHOT_[25,30,35,40,45,50]K || real*8 || || Submm photometric redshift estimate with <i>T</i><sub>xgal</sub> = 25, 30, 35, 40, 45, and 50 K
 +
|-
 +
|ZPHOT_[25,30,35,40,45,50]K_LOW || real*8 || || Lower limit of the 68 % confidence level
 +
|-
 +
|ZPHOT_[25,30,35,40,45,50]K_UP || real*8 ||  || Upper limit of the 68 % confidence level
 +
|-
 +
|ZPHOT_[25,30,35,40,45,50]K_CHI2 || real*8 ||  || Reduced &chi;<sup>2</sup> of the best fit
 +
|-
 +
|LFIR_[25,30,35,40,45,50]K || real*8 || <i>L</i><sub>&#9737;</sub> || FIR luminosity estimate with <math>T_{xgal}</math> = 25, 30, 35, 40, 45, and 50 K
 +
|-
 +
|LFIR_[25,30,35,40,45,50]K_LOW || real*8 ||  <i>L</i><sub>&#9737;</sub> || Lower limit of the 68 % confidence level
 +
|-
 +
|LFIR_[25,30,35,40,45,50]K_UP || real*8 ||  <i>L</i><sub>&#9737;</sub> || Upper limit of the 68 % confidence level
 +
|-
 +
|SFR_[25,30,35,40,45,50]K || real*8 || <i>M</i><sub>&#9737;</sub>yr<sup>-1</sup> || Star Formation Rate estimate with <i>T</i><sub>xgal</i> = 25, 30, 35, 40, 45, and 50 K
 +
|-
 +
|SFR_[25,30,35,40,45,50]K_LOW || real*8 || <i>M</i><sub>&#9737;</sub>yr<sup>-1</sup> || Lower limit of the 68 % confidence level
 +
|-
 +
|SFR_[25,30,35,40,45,50]K_UP || real*8 || <i>M</i><sub>&#9737;</sub>yr<sup>-1</sup> || Upper limit of the 68 % confidence level
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Flags
 +
|- bgcolor="ffdead" 
 +
! FITS Keyword || Data type || Units || Description
 +
|-
 +
|XFLAG_PLANCK || string || || Contains the list of Planck catalogues matching the source: PCCS 857-, 545-, 353-, 217-, 143-, 100-, 70-, 44-, 33-GHz, PSZ, and PGCC
 +
|-
 +
|XFLAG_HERSCHEL || int*4 || 0/1 || 1 if present in the Herschel follow-up programme
  
The all-sky distribution of the PGCC sources is shown below on top of the 857 GHz emission shown in logarithmic scale between 10<sup>-2</sup> to 10<sup>2</sup> MJy/sr.
+
|}
[[File:PGCC_allsky.png|800px|thumb|center|All-sky distribution of the PGCC sources.]]
+
 
 +
 
 +
== (2015) Second SZ Catalogue ==
 +
 
 +
The Planck SZ catalogue is constructed as described in [[Compact_Source_catalogues#Planck_Sunyaev-Zeldovich_catalogue|SZ catalogue]] and in sections 2 and 3 of {{PlanckPapers|planck2014-a36}}. Three pipelines are used to detect SZ clusters: two independent implementations of the Matched Multi-Filter (MMF1 and MMF3), and PowellSnakes (PwS). The main catalogue is constructed as the union of the catalogues from the three detection methods. The completeness and reliability of the catalogues have been assessed through internal and external validation, as described in section 4 of {{PlanckPapers|planck2014-a36}}.
 +
 
 +
The size of a detected object is given in terms of the scale size, &theta;<sub>s</sub>, and the flux is given in terms of the total integrated Comptonization parameter, <i>Y</i> = <i>Y</i><sub>5R500</sub>. The parameters of the generalized NFW profile assumed by the detection pipelines are written in the headers of the catalogues. For the sake of convenience, the conversion factor from <i>Y</i> to <i>Y</i><sub>500</sub> is also provided in the header.
 +
 
 +
The union catalogue contains the coordinates of a detection, its signal-to-noise ratio, an estimate of <i>Y</i> and its uncertainty, together with a summary of the validation information, including external identification of a cluster and its redshift, if they are available. The pipeline from which the information is taken is called the reference pipeline. If more than one pipeline makes the same detection, the information is taken from the the pipeline that makes the most significant detection. Where the redshift is known, we provide the SZ mass for the reference pipeline.
 +
 
 +
The individual catalogues contain the coordinates and the signal-to-noise ratios of the detections, and information on the sizes and flux densities of the detections. The entries are cross-referenced to the detections in the union catalogue. The full information on the degeneracy between &theta;<sub>s</sub> and <i>Y</i> is included in the individual catalogues in the form of the two-dimensional probability distribution for each detection. It is computed on a well-sampled grid to produce a two-dimensional image for each detection. This is provided in this form so it can be combined with a model or external data to produce tighter constraints on the source parameters. The individual catalogues also contain Planck measurements of the SZ mass observable, <i>M</i><sub>SZ</sub>, as calculated using a <i>Y-M</i> scaling relation and an assumed redshift, in order to break the <i>Y</i>-&theta;<sub>s</sub> degeneracy.  These are provided for each detection as functions of assumed redshift, in the range 0.01 < <i>z</i> < 1, along with the upper and lower 68% confidence limits.
  
Sources are divided into three categories based on the reliability of the flux density estimates in IRAS 3 THz and Planck 857, 545, and 353 GHz bands.
+
The selection function of the union catalogue, the intersection catalogue, and the individual catalogues are provided in additional files. The selection function files contain the probability of detection for clusters of given intrinsic parameters &theta;<sub>500</sub> and <i>Y</i><sub>500</sub>. The file includes the definition of the survey area in the form of a HEALPix mask, and is evaluated for a range of signal-to-noise thresholds between 4.5 and 10.
* FLUX_QUALITY=1 : sources with flux density estimates S/N > 1 in all bands ;
 
* FLUX_QUALITY=2 : sources with flux density estimates S/N > 1 only in 857, 545, and 353 GHz Planck bands, considered as very cold source candidates ;
 
* FLUX_QUALITY=3 : sources without any reliable flux density estimates, listed as poor candidates.
 
The all-sky distributions of the PGCC sources per FLUX_QUALITY category are shown below on top of the 857 GHz map in grey scale shown in logarithmic scale between 10<sup>-2</sup> to 10<sup>2</sup> MJy/sr.
 
[[File:PGCC_allsky_FQ1.png|800px|thumb|center|All-sky distribution of the PGCC sources with FLUX_QUALITY=1.]]
 
[[File:PGCC_allsky_FQ2.png|800px|thumb|center|All-sky distribution of the PGCC sources with FLUX_QUALITY=2.]]
 
[[File:PGCC_allsky_FQ3.png|800px|thumb|center|All-sky distribution of the PGCC sources with FLUX_QUALITY=3.]]
 
  
Distance estimates have been obtained on 5574 PGCC sources using seven different methods/technics, as described in {{PlanckPapers | planck2014-a37}}. A flag is raised to quantify the quality of the distance estimates, defined as follows:
+
==== Union catalogue ====
* DIST_QUALITY=0 : No distance estimate ;
 
* DIST_QUALITY=1 : Single distance estimate ;
 
* DIST_QUALITY=2 : Multiple distance estimates which are consistent within 1<math>\sigma</math> ;
 
* DIST_QUALITY=3 : Multiple distance estimates which are not consistent within 1<math>\sigma</math> ;
 
* DIST_QUALITY=4 : Single upper limits.
 
The all-sky distribution of the sources with robust distance estimates is shown below.
 
[[File:PGCC_allsky_DIST.png|800px|thumb|center|All-sky distribution of the  4655 PGCC sources for which a distance estimate with a DIST_QUALITY flag equal to 1 or 2 is available. The various types of distance estimates are defined as follows : kinematic (purple), optical extinction (blue), near-infrared extinction (green), molecular complex association (orange), and Herschel HKP-GCC (red). We also show the distribution of  the 664 sources with an upper-limit estimate  (DIST_QUALITY=4) provided by the near-infrared extinction method (light green). Molecular complexes are outlined with black contours.]]
 
  
The catalogue is contained in the FITS file {{PLASingleFile | fileType=cat | name=HFI_PCCS_GCC_R2.02.fits | link=HFI_PCCS_GCC_R2.02.fits }}.  
+
The union catalogue is contained in ''{{PLASingleFile|fileType=cat | name=HFI_PCCS_SZ-union_R2.08.fits | link=HFI_PCCS_SZ-union_R2.08.fits}}''.
It structure is as follows:
 
  
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=1000px
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
|+ '''FITS file structure'''
 
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! colspan="4" | Identification
+
!colspan="4" | Extension 0: primary header, no data
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS Keyword || Data Type || Units || Description
+
! FITS keyword || Data type || Units || Description
 
|-  
 
|-  
|NAME || String || || Source Name
+
|INSTRUME || String || || Instrument (HFI)
 
|-  
 
|-  
|SNR || real*8 || || Maximum S/N over the 857, 545, and 353 GHz Planck cold residual maps
+
| VERSION || String || || Version of catalogue
 
|-  
 
|-  
|SNR_857 || real*8 || || S/N of the cold residual detection at 857 GHz
+
| DATE || String || || Date file created: yyyy-mm-dd
 
|-  
 
|-  
|SNR_545 || real*8 || || S/N of the cold residual detection at 545 GHz
+
| ORIGIN || String || || Name of organization responsible for the data (HFI-DPC)
 
|-  
 
|-  
|SNR_353 || real*8 || || S/N of the cold residual detection at 353 GHz
+
| TELESCOP || String || || Telescope (PLANCK)
|- bgcolor="ffdead" 
 
! colspan="4" | Source position
 
|- bgcolor="ffdead" 
 
! FITS Keyword || Data Type || Units || Description
 
 
|-  
 
|-  
|GLON || real*8 || deg || Galactic longitude based on morphology fitting
+
| CREATOR || String || || Pipeline version
 
|-  
 
|-  
|GLAT || real*8 || deg || Galactic latitude based on morphology fitting
+
| DATE-OBS || String || || Start date of the survey: yyyy-mm-dd
 
|-  
 
|-  
|RA || real*8 || deg || Right ascension (J2000) in degrees transformed from (GLON, GLAT)
+
| DATE-END || String || || End date of the survey: yyyy-mm-dd
 
|-  
 
|-  
|DEC || real*8 || deg || Declination (J2000) in degrees transformed from (GLON, GLAT)
+
| PROCVER || String || || Data version
|- bgcolor="ffdead" 
 
! colspan="4" | Morphology
 
|- bgcolor="ffdead" 
 
! FITS Keyword || Data Type || Units || Description
 
 
|-  
 
|-  
|GAU_MAJOR_AXIS || real*8 || arcmin || FWHM along the major axis of the elliptical Gaussian
+
| PP_ALPHA || Real*4 || || GNFW pressure profile &alpha; parameter
 
|-  
 
|-  
|GAU_MAJOR_AXIS_SIG || real*8 || arcmin || 1<math>\sigma</math> uncertainty on the FWHM along the major axis
+
| PP_BETA || Real*4 || || GNFW pressure profile &beta; parameter
 
|-  
 
|-  
|GAU_MINOR_AXIS || real*8 || arcmin || FWHM along the minor axis of the elliptical Gaussian
+
| PP_GAMMA || Real*4 || || GNFW pressure profile &gamma; parameter
 
|-  
 
|-  
|GAU_MINOR_AXIS_SIG || real*8 || arcmin || 1<math>\sigma</math> uncertainty on the FWHM along the minor axis
+
| PP_C500 || Real*4 || || GNFW pressure profile <i>c</i><sub>500</sub> parameter
 
|-  
 
|-  
|GAU_POSITION_ANGLE || real*8 || rad || Position angle of the elliptical gaussian (see note 1)
+
| PP_Y2YFH || Real*4 || || Conversion factor from <i>Y</i> to <i>Y</i><sub>500</sub>
|-
+
 
|GAU_POSITION_ANGLE_SIG || real*8 || rad || 1<math>\sigma</math> uncertainty on the position angle
 
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! colspan="4" | Photometry
+
!colspan="4" | Extension 1: BINTABLE, EXTNAME = PSZ2_UNION
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS Keyword || Data Type || Units || Description
+
! Column Name || Data type || Units || Description
|-  
+
|-
|FLUX_3000_CLUMP || real*8 || Jy || Flux density of the clump at 3 THz
+
|INDEX || Int*4 || || Index used to cross-reference with individual catalogues
|-  
+
|-
|FLUX_3000_CLUMP_SIG || real*8 || Jy || 1<math>\sigma</math> uncertainty on the flux density of the clump at 3 THz
+
|NAME || String || || Source name (see note 1)
|-  
+
|-
|FLUX_857_CLUMP || real*8 || Jy || Flux density of the clump at 857 GHz
+
|GLON || Real*8 || deg || Galactic longitude
|-  
+
|-
|FLUX_857_CLUMP_SIG || real*8 || Jy || 1<math>\sigma</math> uncertainty on the flux density of the clump at 857 GHz
+
|GLAT || Real*8 || deg || Galactic latitude
|-  
+
|-
|FLUX_545_CLUMP || real*8 || Jy || Flux density of the clump at 545 GHz
+
|RA  || Real*8 || deg || Right ascension (J2000) transformed from (GLON,GLAT)
|-  
+
|-
|FLUX_545_CLUMP_SIG || real*8 || Jy || 1<math>\sigma</math> uncertainty on the flux density of the clump at 545 GHz
+
|DEC  || Real*8 || deg || Declination (J2000) transformed from (GLON,GLAT)
|-  
+
|-
|FLUX_353_CLUMP || real*8 || Jy || Flux density of the clump at 353 GHz
+
|POS_ERR || Real*4 || arcmin || Position uncertainty (95% confidence interval)
|-  
+
|-
|FLUX_353_CLUMP_SIG || real*8 || Jy || 1<math>\sigma</math> uncertainty on the flux density of the clump at 353 GHz
+
|SNR || Real*4 || || Signal-to-noise ratio of the detection
|-  
+
|-
|FLUX_3000_WBKG || real*8 || Jy || Flux density of the warm background at 3 THz (see note 2)
+
|PIPELINE || Int*4 || || Pipeline from which information is taken (reference pipeline): 1= MMF1; 2 = MMF3; 3 = PwS
|-  
+
|-
|FLUX_3000_WBKG_SIG || real*8 || Jy || 1<math>\sigma</math> uncertainty on the flux density of warm background at 3 THz
+
|PIPE_DET || Int*4 || || Pipelines that detect this object (see note 2)
|-  
+
|-
|FLUX_857_WBKG || real*8 || Jy || Flux density of the warm background at 857 GHz
+
|PCCS2 || Bool || || Indicates whether detection matches with any in PCCS2 catalogues
|-  
+
|-
|FLUX_857_WBKG_SIG || real*8 || Jy || 1<math>\sigma</math> uncertainty on the flux density of the warm background at 857 GHz
+
|PSZ || Int*4 || || Index of matching detection in PSZ1, or -1 if new detection
|-  
+
|-
|FLUX_545_WBKG || real*8 || Jy || Flux density of the warm background at 545 GHz
+
|IR_FLAG || Int*1 || || Flag denoting heavy IR contamination
|-  
+
|-
|FLUX_545_WBKG_SIG || real*8 || Jy || 1<math>\sigma</math> uncertainty on the flux density of the warm background at 545 GHz
+
|Q_NEURAL || Real*4 || || Neural network quality flag (see note 3)
|-  
+
|-
|FLUX_353_WBKG || real*8 || Jy || Flux density of the warm background at 353 GHz
+
|Y5R500 || Real*4 || 10<sup>-3</sup>&nbsp;arcmin<sup>2</sup> || Mean marginal <i>Y</i><sub>5R500</sub> as determined by reference pipeline
|-  
+
|-
|FLUX_353_WBKG_SIG || real*8 || Jy || 1<math>\sigma</math> uncertainty on the flux density of the warm background at 353 GHz
+
|Y5R500_ERR || Real*4 || 10<sup>-3</sup>&nbsp;arcmin<sup>2</sup> || Uncertainty on <i>Y</i><sub>5R500</sub> as determined by reference pipeline
|-  
+
|-
|FLUX_QUALITY || int*4 || 1-3 || Category of flux density reliability (see note 3)
+
|VALIDATION || Int*4 || || External validation status (see note 4)
|-  
+
|-
|FLUX_BLENDING || int*4 || 0/1 || 1 if blending issue with flux density estimate (see note 4)
+
|REDSHIFT_ID || String || || External identifier of cluster associated with redshift measurement (see note 5)
|-  
+
|-
|FLUX_BLENDING_IDX || int*8 || || Catalogue index of the closest source responsible for blending
+
|REDSHIFT || Real*4 || || Redshift of cluster (see note 5)
|-  
+
|-
|FLUX_BLENDING_ANG_DIST || real*8 || arcmin || Angular distance to the closest source responsible for blending
+
|MSZ || Real*4 || 10<sup>14</sup>&nbsp;<i>M</i><sub>&#9737;</sub> || SZ mass proxy (see note 6)
|-  
+
|-
|FLUX_BLENDING_BIAS_3000 || real*8 || % || Relative bias of the flux density at 3000 GHz due to blending
+
|MSZ_ERR_UP || Real*4 || 10<sup>14</sup>&nbsp;<i>M</i><sub>&#9737;</sub> || Upper bound of 68% SZ mass proxy confidence interval (see note 6)
|-  
+
|-
|FLUX_BLENDING_BIAS_857 || real*8 || % || Relative bias of the flux density at 857 GHz due to blending
+
|MSZ_ERR_LOW || Real*4 || 10<sup>14</sup>&nbsp;<i>M</i><sub>&#9737;</sub> || Lower bound of 68% SZ mass proxy confidence interval (see note 6)
|-  
+
|-
|FLUX_BLENDING_BIAS_545 || real*8 || % || Relative bias of the flux density at 545 GHz due to blending
+
|MCXC || String || || Identifier of X-ray counterpart in the MCXC, if one is present
|-   
+
|-
|FLUX_BLENDING_BIAS_353 || real*8 ||  % || Relative bias of the flux density at 353 GHz due to blending
+
|REDMAPPER || String || || Identifier of optical counterpart in the RedMAPPer catalogue, if one is present
|- bgcolor="ffdead"   
+
|-
! colspan="4" | Distance
+
|ACT || String || || Identifier of SZ counterpart in the ACT catalogues, if one is present
|- bgcolor="ffdead"   
+
|-
! FITS Keyword || Data Type || Units || Description
+
|SPT || String || || Identifier of SZ counterpart in the SPT catalogues, if one is present
 +
|-
 +
|WISE_FLAG || Int*4 || || Confirmation flag of WISE overdensity (see note 7)
 +
|-
 +
|AMI_EVIDENCE || Real*4 || || Bayesian evidence for AMI counterpart detection (see note 8)
 +
|-
 +
|COSMO || Bool || || Indicates whether detection is in the cosmology sample
 +
|-
 +
|COMMENT|| String || || Comments on this detection
 +
|}
 +
 
 +
'''Notes'''
 +
# Format is <tt>PSZ2 Glll.ll&plusmn;bb.b</tt> where <i>l</i> and <i>b</i> are the Galactic coordinates, truncated to two decimal places.
 +
# The three least significant decimal digits are used to represent detection or non-detection by the pipelines. The order of the digits is: hundreds = MMF1; tens = MMF3; units = PwS. If it is detected then the corresponding digit is set to 1, otherwise it is set to 0.
 +
# Neural network quality flag is 1-<i>Q</i><sub>bad</sub>, following the definitions in Aghanim et al. 2014.
 +
# Summary of the external validation, encoding the most robust external identification: 10 = ENO follow-up; 11 = RTT follow-up; 12 = PanSTARRs; 13 = RedMAPPer non-blind; 14 = SDSS high-z; 15 = AMI; 16 = WISE; 20 = legacy identification from the PSZ1; 21 = MCXC; 22 = SPT; 23 = ACT; 24 = RedMAPPer; 25 = legacy identification from PSZ1 with externally updated redshift; 30 = NED; and -1 = no known external counterpart.
 +
# The redshift source is the most robust external identification listed in the VALIDATION field.
 +
# <i>M</i><sub>SZ</sub> is the hydrostatic mass assuming the best-fit <i>Y-M</i> scaling relation of Arnaud (2010) as a prior. The uncertainties are statistical and based on the Planck measurement uncertainties only.  Not included in the uncertainties are the statistical errors on the scaling relation, the intrinsic scatter in the relation, or systematic errors in data selection for the scaling relation fit.
 +
# Assigned by visual inspection: 0 = no significant galaxy overdensity; 1 = possible galaxy overdensity; 2 = probable galaxy overdensity; 3 = significant galaxy overdensity detected; -1 = possible galaxy overdensity (affected by bright star artefacts); -2 = no significant galaxy overdensity (affected by bright star artefacts); -3 = no assessment possible (affected by bright star artefacts); and -10 = not analysed.
 +
# Defined in the paper.
 +
 
 +
==== Individual catalogues ====
 +
 
 +
The individual pipeline catalogues are contained in the FITS files
 +
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-MMF1_R2.08.fits | link=HFI_PCCS_SZ-MMF1_R2.08.fits }} (MMF1 pipeline)
 +
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-MMF3_R2.08.fits  | link=HFI_PCCS_SZ-MMF3_R2.08.fits }} (MMF3 pipeline)
 +
* {{PLASingleFile | fileType=cat | name=HFI_PCCS_SZ-PwS_R2.08.fits | link=HFI_PCCS_SZ-PwS_R2.08.fits }} (PowellSnakes pipeline).
 +
 
 +
Their structure is shown in the following table.
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|+ <small>'''FITS file structure'''</small>
 +
|- bgcolor="ffdead"   
 +
! colspan="4" | Extension 0: Primary header, no data
 +
|- bgcolor="ffdead"   
 +
! FITS keyword || Data type || Units || Description
 
|-  
 
|-  
|DIST_KINEMATIC || real*8 || kpc || Distance estimate [1] using kinematics
+
|INSTRUME || String || || Instrument (HFI)
 
|-  
 
|-  
|DIST_KINEMATIC_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [1] using kinematics
+
| VERSION || String || || Version of catalogue
 
|-  
 
|-  
|DIST_OPT_EXT_DR7 || real*8 || kpc || Distance estimate [2] using optical extinction on SDSS DR7
+
| DATE || String || || Date file created: yyyy-mm-dd
 
|-  
 
|-  
|DIST_OPT_EXT_DR7_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [2] using optical extinction on SDSS DR7
+
| ORIGIN || String || || Name of organization responsible for the data (HFI-DPC)
 
|-  
 
|-  
|DIST_OPT_EXT_DR9 || real*8 || kpc || Distance estimate [3] using optical extinction on SDSS DR9
+
| TELESCOP || String || || Telescope (PLANCK)
 
|-  
 
|-  
|DIST_OPT_EXT_DR9_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [3] using optical extinction on SDSS DR9
+
| CREATOR || String || || Pipeline version
 
|-  
 
|-  
|DIST_NIR_EXT_IRDC || real*8 || kpc || Distance estimate  [4] using near-infrared extinction towards IRDCs
+
| DATE-OBS || String || || Start time of the survey: yyyy-mm-dd
 
|-  
 
|-  
|DIST_NIR_EXT_IRDC_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate  [4] using near-infrared extinction towards IRDCs
+
| DATE-END || String || || End time of the survey: yyyy-mm-dd
 
|-  
 
|-  
|DIST_NIR_EXT || real*8 || kpc || Distance estimate [5] using near-infrared extinction
+
| PROCVER || String || || Data version
 
|-  
 
|-  
|DIST_NIR_EXT_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [5] using near-infrared extinction
+
| PP_ALPHA || Real*4 || || GNFW pressure profile &alpha; parameter
 
|-  
 
|-  
|DIST_MOLECULAR_COMPLEX || real*8 || kpc || Distance estimate [6] using molecular complex association
+
| PP_BETA || Real*4 || || GNFW pressure profile &beta; parameter
 
|-  
 
|-  
|DIST_MOLECULAR_COMPLEX_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [6] using molecular complex association
+
| PP_GAMMA || Real*4 || || GNFW pressure profile &gamma; parameter
 
|-  
 
|-  
|DIST_HKP_GCC || real*8 || kpc || Distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
+
| PP_C500 || Real*4 || || GNFW pressure profile <i>c</i><sub>500</sub> parameter
 
|-  
 
|-  
|DIST_HKP_GCC_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
+
| PP_Y2YFH || Real*4 || || Conversion factor from <i>Y</i> to <i>Y</i><sub>500</sub>
|-
+
 
|DIST_OPTION || int*4 || 0-7 || Option of the best distance estimate used in other physical properties
 
|-
 
|DIST_QUALITY || int*4 || 0-4 || Quality Flag of the consistency between distance estimates (see note 5)
 
|-
 
|DIST || real*8 || kpc || Best distance estimate used for further physical properties
 
|-
 
|DIST_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the best distance estimate
 
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! colspan="4" | Temperature
+
! colspan="4" | Extension 1: BINTABLE, EXTNAME = PSZ2_INDIVIDUAL
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS Keyword || Data Type || Units || Description
+
! Column name || Data type || Units || Description
|-  
+
|-
|TEMP_CLUMP || real*8 || K || Temperature of the clump with <math>\beta</math> as a free parameter
+
|INDEX || Int*4 || || Index from union catalogue
|-  
+
|-
|TEMP_CLUMP_SIG || real*8 || K || 1<math>\sigma</math> uncertainty on the clump temperature with <math>\beta</math> free
+
|NAME || String || || Source name (see note 1)
|-  
+
|-
|TEMP_CLUMP_LOW1 || real*8 || K || Lower 68% confidence limit of the clump temperature with <math>\beta</math> free
+
|GLON || Real*8 || deg || Galactic longitude
|-  
+
|-
|TEMP_CLUMP_UP1 || real*8 || K || Upper 68% confidence limit of the clump temperature with <math>\beta</math> free
+
|GLAT || Real*8 || deg || Galactic latitude
 +
|-
 +
|RA  || Real*8 || deg || Right ascension (J2000) transformed from (GLON, GLAT)
 +
|-
 +
|DEC  || Real*8 || deg || Declination (J2000) transformed from (GLON, GLAT)
 +
|-
 +
|POS_ERR || Real*4 || arcmin || Position uncertainty (95% confidence interval)
 +
|-
 +
|SNR || Real*4 || || Signal-to-noise ratio of detection
 +
|-
 +
|TS_MIN || Real*4 || || Minimum value of &theta;<sub>s</sub> in grid in second extension HDU (see note 2)
 +
|-
 +
|TS_MAX || Real*4 || || Maximum value of &theta;<sub>s</sub> in grid in second extension HDU (see note 2)
 +
|-
 +
|Y_MIN || Real*4 || || Minimum value of <i>Y</i> in grid in second extension HDU (see note 2)
 +
|-
 +
|Y_MAX || Real*4 || || Maximum value of <i>Y</i> in grid in second extension HDU (see note 2)
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|BETA_CLUMP || real*8 || || Spectral index <math>\beta</math> of the clump
+
| PIPELINE || String || || Name of detection pipeline
 +
 
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Extension 2: IMAGE, EXTNAME = PSZ2_PROBABILITY (see note 2)
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|BETA_CLUMP_SIG || real*8 || || 1<math>\sigma</math> uncertainty (from MCMC) on the emissivity spectral index <math>\beta</math> of the clump
+
| NAXIS1 || Integer || 256 || Dimension 1
 
|-  
 
|-  
|BETA_CLUMP_LOW1 || real*8 || || Lower 68% confidence limit of the emissivity spectral index <math>\beta</math> of the clump
+
| NAXIS2 || Integer || 256 || Dimension 2
 
|-  
 
|-  
|BETA_CLUMP_UP1 || real*8 || || Upper 68% confidence limit of the emissivity spectral index <math>\beta</math> of the clump
+
| NAXIS3 || Integer || <i>N</i><sub>det</sub> || Dimension 3 = Number of detections
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|TEMP_BETA2_CLUMP || real*8 || K || Temperature of the clump with <math>\beta</math> = 2
+
| PIPELINE || String || || Name of detection pipeline
|-  
+
 
|TEMP_BETA2_CLUMP_SIG || real*8 || K || 1<math>\sigma</math> uncertainty on the temperature of the clump with <math>\beta</math> = 2
+
|- bgcolor="ffdead"
|-  
+
! colspan="4" | Extension 3: IMAGE, EXTNAME = PSZ2_MSZ_ARRAY (see note 3)
|TEMP_BETA2_CLUMP_LOW1 || real*8 || K || Lower 68% confidence limit of the clump temperature with <math>\beta</math> = 2
+
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|TEMP_BETA2_CLUMP_UP1 || real*8 || K || Upper 68% confidence limit of the clump temperature with <math>\beta</math> = 2
+
| NAXIS1 || Integer || 100 || Dimension 1
 
|-  
 
|-  
|TEMP_WBKG || real*8 || K || Temperature of the warm background with <math>\beta</math> as a free parameter (see note 6)
+
| NAXIS2 || Integer || 4 || Dimension 2
 
|-  
 
|-  
|TEMP_WBKG_SIG || real*8 || K || 1<math>\sigma</math> dispersion of the warm background temperature with <math>\beta</math> free
+
| NAXIS3 || Integer || <i>N</i><sub>det</sub> || Dimension 3 = Number of detections
 +
 
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|TEMP_WBKG_LOW1 || real*8 || K || Lower 68% confidence limit of the warm background temperature with <math>\beta</math> free
+
| PIPELINE || String || || Name of detection pipeline
 +
|}
 +
 
 +
 
 +
'''Notes'''
 +
# Format <tt>PSZ2 Glll.ll&plusmn;bb.bb</tt> where <i>l</i> and <i>b</i> are the Galactic coordinates truncated to two decimal places.
 +
# Extension 2 contains a three-dimensional image with the two-dimensional probability distribution in &theta;<sub>s</sub> and <i>Y</i> for each detection. The probability distributions are evaluated on a 256 &times; 256 linear grid between the limits specified in extension 1. The limits are determined independently for each detection. The dimension of the 3D image is 256 &times; 256 &times; <i>N</i><sub>det</sub>, where <i>N</i><sub>det</sub> is the number of detections.  The first dimension is &theta;<sub>s</sub> and the second dimension is <i>Y</i>.
 +
# Extension 3 contains a three-dimensional image with the information on the <i>M</i><sub>SZ</sub> observable per cluster as a function of assumed redshift. The image dimensions are 100 &times; 4 &times; <i>N</i><sub>det</sub>, where <i>N</i><sub>det</sub> is the number of detections. The first dimension is the assumed redshift. The second dimension has size 4: the first element is the assumed redshift value corresponding to the <i>M</i><sub>SZ</sub> values; the second element is the <i>M</i><sub>SZ</sub> lower 68% confidence bound; the third element is the M<sub>SZ</sub> estimate; and the fourth element is the <i>M</i><sub>SZ</sub> upper 68% confidence bound, all in units of 10<sup>14</sup>&nbsp;<i>M</i><sub>&#9737;</sub>. These uncertainties are based on the Planck measurement uncertainties only. Not included in the error estimates are the statistical errors on the scaling relation, the intrinsic scatter in the relation, or systematic errors in data selection for the scaling relation fit.
 +
 
 +
==== Selection function ====
 +
 
 +
The selection function for the union, intersection, and individual pipeline catalogues are contained in the FITS files
 +
 
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-union-survey_R2.08.fits (union catalogue, survey mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-union-cosmolog_R2.08.fits (union catalogue, cosmology mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-intersec-survey_R2.08.fits (intersection catalogue, survey mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-intersec-cosmolog_R2.08.fits  (intersection catalogue, cosmology mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-MMF1-survey_R2.08.fits (MMF1 catalogue, survey mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-MMF1-cosmolog_R2.08.fits (MMF1 catalogue, cosmology mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-MMF3-survey_R2.08.fits (MMF3 catalogue, survey mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-MMF3-cosmolog_R2.08.fits (MMF3 catalogue, cosmology mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-PwS-survey_R2.08.fits  (PowellSnakes catalogue, survey mask)
 +
* http://pla.esac.esa.int/pla/aio/product-action?SOURCE_LIST_ASSOCIATED_PRODUCT.FILE_ID=HFI_PCCS_SZ-selfunc-PwS-cosmolog_R2.08.fits (PowellSnakes catalogue, cosmology mask).
 +
 
 +
 
 +
Their structure is shown in the following table.
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|+ <small>'''FITS file structure'''</small>
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Extension 0: Primary header, no data
 +
|- bgcolor="ffdead" 
 +
! FITS keyword || Data type || Units || Description
 
|-  
 
|-  
|TEMP_WBKG_UP1 || real*8 || K || Upper 68% confidence limit of the warm background temperature with <math>\beta</math> free
+
|INSTRUME || String || || Instrument (HFI)
 
|-  
 
|-  
|BETA_WBKG || real*8 || || Spectral index <math>\beta</math> of the warm background (see note 6)
+
| VERSION || String || || Version of catalogue
 
|-  
 
|-  
|BETA_WBKG_SIG || real*8 || || 1<math>\sigma</math> uncertainty (from MCMC) of the emissivity spectral index <math>\beta</math> of the warm background
+
| DATE || String || || Date file created: yyyy-mm-dd
 
|-  
 
|-  
|BETA_WBKG_LOW1 || real*8 || || Lower 68% confidence limit of the emissivity spectral index <math>\beta</math> of the warm background
+
| ORIGIN || String || || Name of organization responsible for the data (HFI-DPC)
 
|-  
 
|-  
|BETA_WBKG_UP1 || real*8 || || Upper 68% confidence limit of the emissivity spectral index <math>\beta</math> of the warm background
+
| TELESCOP || String || || Telescope (PLANCK)
 
|-  
 
|-  
|TEMP_BETA2_WBKG || real*8 || K || Temperature of the warm background with <math>\beta</math> = 2
+
| CREATOR || String || || Pipeline version
 +
|-
 +
| DATE-OBS || String || || Start time of the survey: yyyy-mm-dd
 
|-  
 
|-  
|TEMP_BETA2_WBKG_SIG || real*8 || K || 1<math>\sigma</math> uncertainty on the temperature of the warm background with <math>\beta</math> = 2
+
| DATE-END || String || || End time of the survey: yyyy-mm-dd
 
|-  
 
|-  
|TEMP_BETA2_WBKG_LOW1 || real*8 || K || Lower 68% confidence limit of the warm background temperature with <math>\beta</math> = 2
+
| PROCVER || String || || Data version
 +
|-
 +
| JOIN || String || || Join type (UNION, INTERSEC, MMF1, MMF3, PwS)
 
|-  
 
|-  
|TEMP_BETA2_WBKG_UP1 || real*8 || K || Upper 68% confidence limit of the warm background temperature with <math>\beta</math> = 2
+
| MASK || String || || Mask name (SURVEY, COSMOLOG)
 +
 
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Extension 1: BINTABLE, HEALPix map (see note 1)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! colspan="4" | Physical properties
+
! FITS keyword || Data type || Value || Description
 +
|-
 +
|PIXTYPE || String || HEALPIX || HEALPix pixelation
 +
|-
 +
|ORDERING || String || RING || Pixel ordering
 +
|-
 +
|NSIDE || Int*4 || 2048 || HEALPix resolution parameter
 +
|-
 +
|NPIX ||Int*4 || 50331648 || Number of pixels
 +
|-
 +
|COORDSYS || String || G || Coordinate system
 +
 
 +
|- bgcolor="ffdead" 
 +
! colspan="4" | Extension 2: IMAGE, EXTNAME = SELFUNC (see note 2)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS Keyword || Data Type || Units || Description
+
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|NH2 || real*8 || cm<sup>-2</sup> || Column density <math>N_{H_2}</math> of the clump
+
| NAXIS1 || Integer || 30 || Dimension 1
 
|-  
 
|-  
|NH2_SIG || real*8 || cm<sup>-2</sup> || 1<math>\sigma</math> uncertainty on the column density
+
| NAXIS2 || Integer || 32 || Dimension 2
 
|-  
 
|-  
|NH2_LOW[1,2,3] || real*8 || cm<sup>-2</sup> || Lower 68%, 95% and 99% confidence limit of the column density
+
| NAXIS3 || Integer || 12 || Dimension 3
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|NH2_UP[1,2,3]  || real*8 || cm<sup>-2</sup> || Upper 68%, 95% and 99% confidence limit of the column density
+
| AXIS1 || String || CY500 || Name of axis 1
 
|-  
 
|-  
|MASS || real*8 || <math>M_{o}</math> || Mass estimate of the clump
+
| AXIS2 || String || T500 || Name of axis 2
 
|-  
 
|-  
|MASS_SIG  || real*8 || <math>M_{o}</math> || 1<math>\sigma</math> uncertainty on the mass estimate of the clump
+
| AXIS3 || String || SNRCUT || Name of axis 3
 
|-  
 
|-  
|MASS_LOW[1,2,3]  || real*8 || <math>M_{o}</math> || Lower 68%, 95% and 99% confidence limit of the mass estimate
+
| UNITS || String || PERCENT || Units of selection function
 
|-  
 
|-  
|MASS_UP[1,2,3|| real*8 || <math>M_{0}</math> || Upper 68%, 95% and 99% confidence limit of the mass estimate
+
| COMPTYPE || String || DIFF || Type of selection function (differential)
 +
 
 +
|- bgcolor="ffdead"
 +
! colspan="4" | Extension 3: IMAGE, EXTNAME = YGRID (see note 3)
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|DENSITY || real*8 || cm<sup>-3</sup> || Mean density of the clump
+
| NAXIS1 || Integer || 30 || Dimension 1
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|DENSITY_SIG  || real*8 || cm<sup>-3</sup> || 1<math>\sigma</math> uncertainty on the mean density estimate of the clump
+
| COL1 || String || CY500 || Grid values of <i>Y</i><sub>500</sub>
 +
 
 +
|- bgcolor="ffdead"
 +
! colspan="4" | Extension 4: IMAGE, EXTNAME = TGRID (see note 4)
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|DENSITY_LOW[1,2,3]  || real*8 || cm<sup>-3</sup>  || Lower 68%, 95% and 99% confidence limit of the mean density estimate
+
| NAXIS1 || Integer || 32 || Dimension 1
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|DENSITY_UP[1,2,3]  || real*8 || cm<sup>-3</sup> || Upper 68%, 95% and 99% confidence limit of the mean density estimate
+
| COL1 || String || T500 || Grid values of &theta;<sub>500</sub>
 +
 
 +
|- bgcolor="ffdead"
 +
! colspan="4" | Extension 5: IMAGE, EXTNAME = SNR_THRESH (see note 5)
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|SIZE || real*8 || pc || Physical size of the clump
+
| NAXIS1 || Integer || 12 || Dimension 1
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|SIZE_SIG  || real*8 || pc  || 1<math>\sigma</math> uncertainty on the physical size estimate of the clump
+
| COL1 || String || S/N || Grid values of S/N threshold
|-  
+
 
|SIZE_LOW[1,2,3]  || real*8 || pc  || Lower 68%, 95% and 99% confidence limit of the physical size estimate
+
|}
|-  
+
 
|SIZE_UP[1,2,3|| real*8 || pc || Upper 68%, 95% and 99% confidence limit of the physical size estimate
+
'''Notes'''
|-
+
# Extension 1 contains a mask defining the survey region, given by an <i>N</i><sub>side</sub> = 2048 ring-ordered HEALPix map in GALACTIC coordinates. Pixels in the survey region have the value 1.0, while pixels outside  the survey region have value 0.0.
|LUMINOSITY || real*8 || L<sub>o</sub> || Luminosity of the clump
+
# Extension 2 contains a three-dimensional image, giving the survey completeness probability distribution for various S/N thresholds. The information is stored in an image of size 30 &times; 32 &times; 12. The first dimension is <i>Y</i><sub>500</sub>, the second dimension is &theta;<sub>500</sub> and the third dimension is the signal-to-noise threshold. The units are percentages and lie in the range 0-100, denoting the detection probability of a cluster in the given (<i>Y</i><sub>500</sub>, &theta;<sub>500</sub>) bin.
|-
+
# Extension 3 contains the <i>Y</i><sub>500</sub> grid values for the completeness data cube in the second extension. It has length 30 and spans the range from 1.12480 &times; 10<sup>-4</sup> arcmin<sup>2</sup> to 7.20325 &times; 10<sup>-2</sup> arcmin<sup>2</sup> in logarithmic steps.
|LUMINOSITY_SIG  || real*8 || L<sub>o</sub> || 1<math>\sigma</math> uncertainty on the luminosity estimate of the clump
+
# Extension 4 contains the θ<sub>500</sub> grid values for the completeness data cube in the second extension. It has length 32 and spans the range from 0.9416 arcmin to 35.31 arcmin in logarithmic steps.
|-
+
# Extension 5 contains the signal-to-noise threshold grid values for the completeness data cube in the second extension. It has length 12 and contains thresholds from 4.5 to 10.0 in steps of 0.5.
|LUMINOSITY_LOW[1,2,3]  || real*8 || L<sub>o</sub> || Lower 68%, 95% and 99% confidence limit of the luminosity estimate
+
 
|-
+
=== Previous releases: (2013) PSZ1 ===
|LUMINOSITY_UP[1,2,3]  || real*8 || L<sub>o</sub> || Upper 68%, 95% and 99% confidence limit of the luminosity estimate
+
 
|- bgcolor="ffdead"   
+
<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #EEE8AA;width:95%">
! colspan="4" | Flags
+
'''Second Planck Release (2013): Description of the Planck SZ Catalogue'''
|- bgcolor="ffdead"   
+
<div class="mw-collapsible-content">
! FITS Keyword || Data Type || Units || Description
+
 
|-
+
The Planck SZ catalogue is constructed as described in [[Compact_Source_catalogues#Planck_Sunyaev-Zeldovich_catalogue|SZ catalogue]] and in section 2 of {{PlanckPapers|planck2013-p05a}}.
|XFLAG_LMC || int*4 || 0/1 || 1 if part of the LMC
+
 
|-
+
Three pipelines are used to detect SZ clusters: two independent implementations of the Matched Multi-Filter (MMF1 and MMF3), and PowellSnakes (PwS). The main catalogue is constructed as the union of the catalogues from the three detection methods. The individual catalogues are provided for the expert user in order to assess the consistency of the pipelines. The completeness and reliability of the catalogues have been assessed through internal and external validation as described in sections 3-6 of {{PlanckPapers|planck2013-p05a}}.
|XFLAG_SMC || int*4 || 0/1 || 1 if part of the SMC
+
 
 +
The union catalogue contains the coordinates and the signal-to-noise ratio of the detections and a summary of the external validation information, including external identification of a cluster and its redshift if it is available.
 +
 
 +
The individual catalogues contain the coordinates and the signal-to-noise ratio of the detections, and information on the size and flux of the detections. The entries are cross-referenced to the detections in the union catalogue.
 +
 
 +
The size of a detection is given in terms of the scale size, &theta;<sub>s</sub>, and the flux is given in terms of the total integrated Comptonization parameter, <i>Y</i> = <i>Y</i><sub>5r<sub>500</sub></sub>. The parameters of the GNFW profile assumed by the detection pipelines is written in the headers in the catalogues. For the sake of convenience, the conversion factor from <i>Y</i> to <i>Y</i><sub>500</sub> is also written in the header.
 +
 
 +
The full information on the degeneracy between &theta;<sub>s</sub> and <i>Y</i> is included in the individual catalogues in the form of the two-dimensional probability distribution for each detection. It is computed on a well-sampled grid to produce a two-dimensional image for each detection. The degeneracy information is provided in this form so it can be combined with a model or external data to produce tighter constraints on the parameters.
 +
 
 +
 +
'''Union Catalogue'''
 +
 
 +
The union catalogue is contained in  ''{{PLASingleFile|fileType=cat | name=COM_PCCS_SZ-union_R1.12.fits | link=COM_PCCS_SZ-union_R1.12.fits}}''.
 +
 
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|- bgcolor="ffdead"   
 +
!colspan="4" | Extension 0: Primary header, no data
 +
|- bgcolor="ffdead"   
 +
! FITS Keyword || Data type || Units || Description
 
|-  
 
|-  
|XFLAG_ECC || int*4 || 0/1 || 1 if present in the ECC
+
|INSTRUME || String || || Instrument.
 
|-  
 
|-  
|XFLAG_PCCS_857 || int*4 || 0/1 || 1 if present in the PCCS 857 GHz band
+
| VERSION || String || || Version of catalogue.
 
|-  
 
|-  
|XFLAG_PCCS_545 || int*4 || 0/1 || 1 if present in the PCCS 545 GHz band
+
| DATE || String || || Date file created: yyyy-mm-dd.
 
|-  
 
|-  
|XFLAG_PCCS_353 || int*4 || 0/1 || 1 if present in the PCCS 353 GHz band
+
| ORIGIN || String || || Name of organization responsible for the data.
 
|-  
 
|-  
|XFLAG_PCCS_217 || int*4 || 0/1 || 1 if present in the PCCS 217 GHz band
+
| TELESCOP || String || || PLANCK.
 +
|-
 +
| CREATOR || String || || Pipeline version.
 +
|-
 +
| DATE-OBS || String || || Start time of the survey: yyyy-mm-dd.
 +
|-
 +
| DATE-END || String || || End time of the survey: yyyy-mm-dd.
 +
|-
 +
| PROCVER || String || || Data version.
 +
|-
 +
| PP_ALPHA || Real*4 || || GNFW pressure profile &alpha; parameter.
 +
|-
 +
| PP_BETA || Real*4 || || GNFW pressure profile &beta; parameter.
 +
|-
 +
| PP_GAMMA || Real*4 || || GNFW pressure profile &gamma; parameter.
 +
|-
 +
| PP_C500 || Real*4 || || GNFW pressure profile <i>c</i><sub>500</sub> parameter.
 
|-  
 
|-  
|XFLAG_PCCS_143 || int*4 || 0/1 || 1 if present in the PCCS 143 GHz band
+
| PP_Y2YFH || Real*4 || || Conversion factor from <i>Y</i> to <i>Y</i><sub>500</sub>.
 +
 
 +
|- bgcolor="ffdead" 
 +
!colspan="4" | Extension 1: data extension (BINTABLE)
 +
|- bgcolor="ffdead" 
 +
! Column Name || Data type || Units || Description
 
|-
 
|-
|XFLAG_PCCS_100 || int*4 || 0/1 || 1 if present in the PCCS 100 GHz band
+
|INDEX || Int*4 || || Index. Used to cross-reference with individual catalogues.
 
|-
 
|-
|XFLAG_PCCS_70 || int*4 || 0/1 || 1 if present in the PCCS 70 GHz band
+
|NAME || String || || Source name (note 1).
 
|-
 
|-
|XFLAG_PCCS_44 || int*4 || 0/1 || 1 if present in the PCCS 44 GHz band
+
|GLON || Real*8 || degrees || Galactic longitude.
 
|-
 
|-
|XFLAG_PCCS_30 || int*4 || 0/1 || 1 if present in the PCCS 30 GHz band
+
|GLAT || Real*8 || degrees || Galactic latitude.
 
|-
 
|-
|XFLAG_PSZ || int*4 || 0/1 || 1 if present in the PCCS PSZ
+
|RA  || Real*8 || degrees || Right ascension (J2000) transformed from (GLON,GLAT).
 
|-
 
|-
|XFLAG_PHZ || int*4 || 0/1 || 1 if present in the PCCS HZ
+
|DEC  || Real*8 || degrees || Declination (J2000) transformed from (GLON,GLAT).
 +
|-
 +
|POS_ERR || Real*4 || arcmin || Position uncertainty (approximate 68% confidence interval). See [[#Caveats|Caveats]] below.
 +
|-
 +
|SNR || Real*4 || || Signal-to-noise ratio of the detection.
 +
|-
 +
|PIPELINE || Int*4 || || Souce pipeline: 1= MMF1; 2 = MMF3; 3 = PwS.
 +
|-
 +
|PIPE_DET || Int*4 || || Pipelines which detect this object (note 2).
 +
|-
 +
|PCCS || Bool || || Indicates whether detection matches any PCCS source.
 +
|-
 +
|VALIDATION || Int*4 || || External validation status (note 3)
 +
|-
 +
|ID_EXT || String|| || External identifier of cluster.
 +
|-
 +
|REDSHIFT || Real*4 || || Redshift of cluster.
 +
|-
 +
|COSMO || Bool || || Detection is in the cosmology sample.
 
|-
 
|-
|XFLAG_HKP_GCC || int*4 || 0/1 || 1 if present in the Herschel HKP-GCC
+
|COMMENT|| Bool || || Detection has a comment in the associated text file (note 4).
 
 
 
|}
 
|}
  
  
Notes:
+
'''Notes'''
* 1: The position angle of the 2D ellipse is defined as the angle between the axis parallele to the Galactic plane and the major axis, counted clockwise.
+
# format is ''PSZ1 Glll.ll+mn;bb.b'' where <i>l</i> nd <i>b</i> are the Galactic and truncated to 2 decimal places.
* 2: The warm bakcground flux densities are computed using the same solid angle as for the clumps flux densities, but on the warm conponent map.
+
# The three least significant decimal digits are used to represent detection or non-detection by the pipelines. Order of the digits: hundreds = MMF1; tens = MMF3; units = PwS. If it is detected then the corresponding digit is set to 1, otherwise it is set to 0.
* 3: See text above for a full description of the FLUX_QUALITY flag, for which 1 is best.
+
# values are: 1 = candidate of class 1; 2 = candidate of class 2; 3 = candidate of class 3; 10 = Planck cluster confirmed by follow-up;  20 = known cluster.
* 4: This relative bias due to blending provides a rough estimate of the factor that should be applied on the clumpds flux densities to get a corrected estimate. It has been obtained on a very simple modelling of clumps morphology and the local environment. It has therefore to be taken very carefully.
+
# The  comments on the detections in the catalogue are contained in a text file called ''{{PLASingleFile|fileType=catdoc | name=COM_PCCS_SZ-union_comments_R1.11.txt | link=COM_PCCS_SZ-union_comments_R1.11.txt}}'', which contains one line for each detection in the union catalogue with COMMENT = T. The line starts with the INDEX and NAME of the detection to facilitate cross-referencing. The remainder of the line is the comment on that detection.
* 5: See text above for a full description of the DIST_QUALITY flag.
 
* 6: Temperature and spectral index of the warm background are based on the warm background flux density estimates obtained on the same solid angle used for clumps
 
  
 +
'''Individual Catalogues'''
  
 +
The individual pipeline catalogues are contained in the FITS files
 +
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-MMF1_R1.11.fits  | link=COM_PCCS_SZ-MMF1_R1.11.fits }} (Matched Multi-Filter method #1)
 +
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-MMF3_R1.12.fits  | link=COM_PCCS_SZ-MMF3_R1.12.fits }} (Matched Multi-Filter method #3)
 +
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-PwS_R1.11.fits  | link=COM_PCCS_SZ-PwS_R1.11.fits }} (Powell Snakes method)
 +
Their structure is as follows:
  
==(2015) Planck List of high-redshift source candidates==
 
  
The Planck list of high-redshift source candidates (PHZ) is a list of 2151 sources located in the cleanest 26% of the sky and identified as point sources
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
exhibiting an excess in the submillimeter compared to their environment. It has been built using the 48 months Planck data at 857, 545, 353 and 217 GHz combined with the 3 THz IRAS data, as it is described in {{PlanckPapers | }}. These sources are considered as high-z source candidates (z>1.5-2), given the very low contamination by Galactic cirrus. 
 
 
 
 
 
 
 
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=1000px
 
 
|+ '''FITS file structure'''
 
|+ '''FITS file structure'''
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! colspan="4" | Identification
+
 
 +
! colspan="4" | Ext. 0: Primary header, no data
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS Keyword || Data Type || Units || Description
+
! FITS Keyword || Data type || Units || Description
 
|-  
 
|-  
|NAME || String || || Source Name
+
|INSTRUME || String || || Instrument.
 
|-  
 
|-  
|SNR_X545 || real*8 || || S/N in the 545 GHz excess map
+
| VERSION || String || || Version of catalogue.
 
|-  
 
|-  
|SNR_D857 || real*8 || || S/N in the 857 GHz cleaned map
+
| DATE || String || || Date file created: yyyy-mm-dd.
 
|-  
 
|-  
|SNR_D545 || real*8 || || S/N in the 545 GHz cleaned map
+
| ORIGIN || String || || Name of organization responsible for the data.
 
|-  
 
|-  
|SNR_D353 || real*8 || || S/N in the 353 GHz cleaned map
+
| TELESCOP || String || || PLANCK.
|- bgcolor="ffdead" 
 
! colspan="4" | Source position
 
|- bgcolor="ffdead" 
 
! FITS Keyword || Data Type || Units || Description
 
 
|-  
 
|-  
|GLON || real*8 || deg || Galactic longitude based on morphology fitting
+
| CREATOR || String || || Pipeline version.
 
|-  
 
|-  
|GLAT || real*8 || deg || Galactic latitude based on morphology fitting
+
| DATE-OBS || String || || Start time of the survey: yyyy-mm-dd.
 
|-  
 
|-  
|RA || real*8 || deg || Right ascension (J2000) in degrees transformed from (GLON, GLAT)
+
| DATE-END || String || || End time of the survey: yyyy-mm-dd.
 
|-  
 
|-  
|DEC || real*8 || deg || Declination (J2000) in degrees transformed from (GLON, GLAT)
+
| PROCVER || String || || Data version.
|- bgcolor="ffdead" 
 
! colspan="4" | Morphology
 
|- bgcolor="ffdead" 
 
! FITS Keyword || Data Type || Units || Description
 
 
|-  
 
|-  
|GAU_MAJOR_AXIS || real*8 || arcmin || FWHM along the major axis of the elliptical Gaussian
+
| PP_ALPHA || Real*4 || || GNFW pressure profile &alpha; parameter.
 
|-  
 
|-  
|GAU_MAJOR_AXIS_SIG || real*8 || arcmin || 1<math>\sigma</math> uncertainty on the FWHM along the major axis
+
| PP_BETA || Real*4 || || GNFW pressure profile &beta; parameter.
 
|-  
 
|-  
|GAU_MINOR_AXIS || real*8 || arcmin || FWHM along the minor axis of the elliptical Gaussian
+
| PP_GAMMA || Real*4 || || GNFW pressure profile &gamma; parameter.
 
|-  
 
|-  
|GAU_MINOR_AXIS_SIG || real*8 || arcmin || 1<math>\sigma</math> uncertainty on the FWHM along the minor axis
+
| PP_C500 || Real*4 || || GNFW pressure profile <i>c</i><sub>500</sub> parameter.
 
|-  
 
|-  
|GAU_POSITION_ANGLE || real*8 || rad || Position angle of the elliptical gaussian (see note 1)
+
| PP_Y2YFH || Real*4 || || Conversion factor from <i>Y</i> to <i>Y</i><sub>500</sub>.
|-
 
|GAU_POSITION_ANGLE_SIG || real*8 || rad || 1<math>\sigma</math> uncertainty on the position angle
 
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! colspan="4" | Photometry
+
 
 +
 
 +
! colspan="4" | Ext. 1: EXTNANE = ''PSZ_INDIVIDUAL'' (BINTABLE)
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
! FITS Keyword || Data Type || Units || Description
+
! Column Name || Data type || Units || Description
|-  
+
|-
|FLUX_CLEAN_857 || real*8 || Jy || Flux density of the clump at 857 GHz
+
|INDEX || Int*4 || || Index from union catalogue.
|-  
+
|-
|FLUX_CLEAN_857_SIG_SKY || real*8 || Jy || 1<math>\sigma</math> uncertainty at 857 GHz due to sky confusion
+
|NAME || String || || Source name - see note 1.
|-  
+
|-
|FLUX_CLEAN_857_SIG_DATA || real*8 || Jy || 1<math>\sigma</math> uncertainty at 857 GHz due to measurement error
+
|GLON || Real*8 || deg || Galactic longitude.
|-  
+
|-
|FLUX_CLEAN_857_SIG_GEOM || real*8 || Jy || 1<math>\sigma</math> uncertainty at 857 GHz due to elliptical Gaussian fit accuracy
+
|GLAT || Real*8 || deg || Galactic latitude.
 +
|-
 +
|RA  || Real*8 || deg || Right ascension (J2000) transformed from (GLON,GLAT).
 +
|-
 +
|DEC  || Real*8 || deg || Declination (J2000) transformed from (GLON,GLAT).
 +
|-
 +
|POS_ERR || Real*4 || arcmin || Position uncertainty (approximate 68% confidence interval). See [[#Caveats|Caveats]] below.
 +
|-
 +
|SNR || Real*4 || || Signal-to-noise ratio of the detection.
 +
|-
 +
|SNR_COMPAT || Real*4 || || S/N of the detection in compatibility mode (note 2).
 +
|-
 +
|TS_MIN || Real*4 || || Minimum value of &theta;<sub>s</i in grid in second extension HDU (see below).
 +
|-
 +
|TS_MAX || Real*4 || || Maximum value of &theta;<sub>s</i> in grid in second extension HDU (see below).
 +
|-
 +
|Y_MIN || Real*4 || || Minimum value of <i>Y</i> in grid in second extension HDU (see below).
 +
|-
 +
|Y_MAX || Real*4 || || Maximum value of <i>Y</i> in grid in second extension HDU (see below).
 +
 
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|FLUX_CLEAN_545 || real*8 || Jy || Flux density of the clump at 545 GHz
+
| PIPELINE || String || || Name of detection pipeline.
 +
|- bgcolor="ffdead" 
 +
 
 +
 
 +
! colspan="4" | Ext. 2: EXTNAME = ''PSZ_PROBABILITY'' (IMAGE) - note 3
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|FLUX_CLEAN_545_SIG_SKY || real*8 || Jy || 1<math>\sigma</math> uncertainty at 545 GHz due to sky confusion
+
| NAXIS1 || Integer || 256 || Dim 1
 
|-  
 
|-  
|FLUX_CLEAN_545_SIG_DATA || real*8 || Jy || 1<math>\sigma</math> uncertainty at 545 GHz due to measurement error
+
| NAXIS2 || Integer || 256 || Dim 2
 
|-  
 
|-  
|FLUX_CLEAN_545_SIG_GEOM || real*8 || Jy || 1<math>\sigma</math> uncertainty at 545 GHz due to elliptical Gaussian fit accuracy
+
| NAXIS3 || Integer || Nsources || Dim 3 = Number of sources
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data type || Value || Description
 
|-  
 
|-  
|FLUX_CLEAN_353 || real*8 || Jy || Flux density of the clump at 353 GHz
+
| PIPELINE || String || || Name of detection pipeline.
|-
+
|}
|FLUX_CLEAN_353_SIG_SKY || real*8 || Jy || 1<math>\sigma</math> uncertainty at 353 GHz due to sky confusion
+
 
|-
+
 
|FLUX_CLEAN_353_SIG_DATA || real*8 || Jy || 1<math>\sigma</math> uncertainty at 353 GHz due to measurement error
+
'''Notes'''
|-
+
# Format ''PSZ1 Glll.ll&plusmn;bb.bb'' where <i>l</i> and <i>b</i> are the Galactic coordinates truncated to two decimal places.
|FLUX_CLEAN_353_SIG_GEOM || real*8 || Jy || 1<math>\sigma</math> uncertainty at 353 GHz due to elliptical Gaussian fit accuracy
+
# For PwS, this is the S/N evaluated in a manner compatible with the MMF pipelines. For MMF1 and MMF3, it is identical to S/N.
|-  
+
# Ext. 2 contains a three-dimensional image with the two-dimensional probability distribution in &theta;<sub>s</sub> and <i>Y</i> for each detection. The probability distributions are evaluated on a 256 &times; 256 linear grid between the limits specified in Ext. 1. The limits are determined independently for each detection. The dimension of the 3D image is 256 &times; 256 &times; n, where n is the number of detections.  The first dimension is &theta;<sub>s</sub> and the second dimension is <i>Y</i>.
|FLUX_CLEAN_217 || real*8 || Jy || Flux density of the clump at 217 GHz
+
 
|-  
+
 
|FLUX_CLEAN_217_SIG_SKY || real*8 || Jy || 1<math>\sigma</math> uncertainty at 217 GHz due to sky confusion
+
'''Mask'''
|-
+
 
|FLUX_CLEAN_217_SIG_DATA || real*8 || Jy || 1<math>\sigma</math> uncertainty at 217 GHz due to measurement error
+
The mask used to construct the catalogue is contained in a file: ''{{PLASingleFile|fileType=catdoc | name=COM_PCCS_SZ-unionMask_2048_R1.11.fits| link=COM_PCCS_SZ-unionMask_2048_R1.11.fits}}''.
|-
+
 
|FLUX_CLEAN_217_SIG_GEOM || real*8 || Jy || 1<math>\sigma</math> uncertainty at 217 GHz due to elliptical Gaussian fit accuracy
+
It is in GALACTIC coordinates, NESTED ordering, NSIDE=2048.
|- bgcolor="ffdead" 
+
 
! colspan="4" | Distance
+
 
|- bgcolor="ffdead" 
+
'''Additional information'''
! FITS Keyword || Data Type || Units || Description
+
 
|-
+
A set of comments on the union catalogue is available in
|DIST_KINEMATIC || real*8 || kpc || Distance estimate [1] using kinematics
+
 
|-
+
: ''{{PLASingleFile|fileType=cat | name=COM_DocPCCS_SZ-union-comments_R1.11.txt | link=COM_DocPCCS_SZ-union-comments_R1.11.txt}}''
|DIST_KINEMATIC_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [1] using kinematics
+
 
|-  
+
Additional information on the SZ detections was retrieved from external sources and written into the FITS file
|DIST_OPT_EXT_DR7 || real*8 || kpc || Distance estimate [2] using optical extinction on SDSS DR7
+
 
|-
+
: ''{{PLASingleFile|fileType=cat | name=COM_PCCS_SZ-validation_R1.12.fits | link=COM_PCCS_SZ-validation_R1.12.fits}}''
|DIST_OPT_EXT_DR7_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [2] using optical extinction on SDSS DR7
+
 
|-
+
(for more details see {{PlanckPapers|planck2013-p05a}}). This file contains a single ''BINTABLE'' extension.  The table contains 1 line per source, and the columns and their meaning are given below.
|DIST_OPT_EXT_DR9 || real*8 || kpc || Distance estimate [3] using optical extinction on SDSS DR9
+
 
|-  
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
|DIST_OPT_EXT_DR9_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [3] using optical extinction on SDSS DR9
+
|+ '''FITS file structure'''
|-  
+
|- bgcolor="ffdead" 
|DIST_NIR_EXT_IRDC || real*8 || kpc || Distance estimate  [4] using near-infrared extinction towards IRDCs
+
 
|-  
+
! colspan="4" | Ext. 0:  (BINTABLE)
|DIST_NIR_EXT_IRDC_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate  [4] using near-infrared extinction towards IRDCs
+
|- bgcolor="ffdead" 
|-  
+
! Column Name || Data type || Units || Description
|DIST_NIR_EXT || real*8 || kpc || Distance estimate [5] using near-infrared extinction
+
|-
|-  
+
|INDEX || Int*4 || || Index from union catalogue.
|DIST_NIR_EXT_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [5] using near-infrared extinction
+
|-
|-  
+
|NAME || String || || Source name in union catalogue
|DIST_MOLECULAR_COMPLEX || real*8 || kpc || Distance estimate [6] using molecular complex association
+
|-
|-  
+
|REDSHIFT || Real*4 || || Redshift
|DIST_MOLECULAR_COMPLEX_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [6] using molecular complex association
+
|-
|-
+
|REDSHIFT_SOURCE || Int*4 || || Source for redshift - see note 4.
|DIST_HKP_GCC || real*8 || kpc || Distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
+
|-
|-  
+
|ALT_NAME  || String || || Alternative names.
|DIST_HKP_GCC_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
+
|-
|-  
+
|RA_MCXC  || Real*4 || degrees || Right Ascension of the MCXC identifier.
|DIST_OPTION || int*4 || 0-7 || Option of the best distance estimate used in other physical properties
+
|-
|-  
+
|DEC_MCXC || Real*4 || degrees || Declination of the MCXC identifier.
|DIST_QUALITY || int*4 || 0-4 || Quality Flag of the consistency between distance estimates (see note 5)
+
|-
|-  
+
|YZ_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup> || Compton parameter in R500 from SZ-proxy.
|DIST || real*8 || kpc || Best distance estimate used for further physical properties
+
|-
|-  
+
|ERRP_YZ_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup>  || Error sup. in YZ_500
|DIST_SIG || real*8 || kpc || 1<math>\sigma</math> uncertainty on the best distance estimate
+
|-
|- bgcolor="ffdead" 
+
|ERRM_YZ_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup>  || Error inf. in YZ_500
! colspan="4" | Temperature
+
|-
|- bgcolor="ffdead" 
+
|M_YZ_500 || Real*4 || 10<sup>14</sup> Msol|| Derived mass estimate (M_YZ_500) from SZ proxy.
! FITS Keyword || Data Type || Units || Description
+
|-
|-  
+
|ERRP_M_YZ_500 || Real*4 || 10<sup>14</sup> Msol || Error sup. on M_YZ_500.
|TEMP_CLUMP || real*8 || K || Temperature of the clump with <math>\beta</math> as a free parameter
+
|-
|-  
+
|ERRM_M_YZ_500 || Real*4 || 10<sup>14</sup> Msol || Error sup. on M_YZ_500.
|TEMP_CLUMP_SIG || real*8 || K || 1<math>\sigma</math> uncertainty on the clump temperature with <math>\beta</math> free
+
|-
|-  
+
|S_X || Real*4 || erg/s/cm<sup>2</sup>  || Unabsorbed X-ray flux - see note 1.
|TEMP_CLUMP_LOW1 || real*8 || K || Lower 68% confidence limit of the clump temperature with <math>\beta</math> free
+
|-
|-  
+
|ERR_S_X || Real*4 || erg/s/cm<sup>2</sup>  || Error on unabsorbed X-ray flux.
|TEMP_CLUMP_UP1 || real*8 || K || Upper 68% confidence limit of the clump temperature with <math>\beta</math> free
+
|-
|-  
+
|Y_PSX_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup> || SZ signal for PSZ clusters identified with MCXC clusters- see note 2.
|BETA_CLUMP || real*8 || || Spectral index <math>\beta</math> of the clump
+
|-
|-  
+
|SN_PSX || Real*4 || || Signal to noise for PSZ clusters identified with MCXC clusters - see note 3.
|BETA_CLUMP_SIG || real*8 || || 1<math>\sigma</math> uncertainty (from MCMC) on the emissivity spectral index <math>\beta</math> of the clump
+
|}
|-  
+
 
|BETA_CLUMP_LOW1 || real*8 || || Lower 68% confidence limit of the emissivity spectral index <math>\beta</math> of the clump
+
'''Notes'''
|-
+
# Unabsorbed X-ray flux measured in an aperture of 5 arcmin in the band [0.1-2.4] keV. The aperture is centered on the Planck position, except for candidates associated with a BSC source for which we adopt the X-ray position. For sources with <math>(S/N)_{RASS} < 1\sigma</math>, we only quote an upper limit.
|BETA_CLUMP_UP1 || real*8 || || Upper 68% confidence limit of the emissivity spectral index <math>\beta</math> of the clump
+
# SZ signal re-extracted fixing the size to the X-ray size provided in the MCXC catalogue at the X-ray position, for PSZ clusters identified with MCXC clusters.
|-  
+
# Computed in the Planck data at the X-ray position fixing the size to the X-ray size provided in the MCXC catalogue, for PSZ clusters identified with MCXC clusters.
|TEMP_BETA2_CLUMP || real*8 || K || Temperature of the clump with <math>\beta</math> = 2
+
# Source for redshifts:
|-  
+
    -1 : No redshift available;
|TEMP_BETA2_CLUMP_SIG || real*8 || K || 1<math>\sigma</math> uncertainty on the temperature of the clump with <math>\beta</math> = 2
+
      1 : MCXC updated compilation{{BibCite|Piffaretti2011}};
|-
+
      2 : Databases NED and SIMBAD-CDS;
|TEMP_BETA2_CLUMP_LOW1 || real*8 || K || Lower 68% confidence limit of the clump temperature with <math>\beta</math> = 2
+
      3 : SDSS cluster catalogue{{BibCite|Wen2012}};
|-
+
      4 : SDSS cluster catalogue{{BibCite|Szabo2011}};
|TEMP_BETA2_CLUMP_UP1 || real*8 || K || Upper 68% confidence limit of the clump temperature with <math>\beta</math> = 2
+
      5 : SPT{{BibCite|Vanderlinde2010}}{{BibCite|Williamson2011}}{{BibCite|Andersson2011}}{{BibCite|Plagge2010}}{{BibCite|Reichardt2013}}{{BibCite|Story2011}}{{BibCite|Song2012}};
|-
+
      6 : ACT{{BibCite|Hasselfield2013}}{{BibCite|Marriage2011}}{{BibCite|Menanteau2010}}{{BibCite|Sifon2013}};
|TEMP_WBKG || real*8 || K || Temperature of the warm background with <math>\beta</math> as a free parameter (see note 6)
+
      7 : Search in SDSS galaxy catalogue from Planck Collab.;
|-
+
    20 : XMM-Newton confirmation from Planck Collab.;
|TEMP_WBKG_SIG || real*8 || K || 1<math>\sigma</math> dispersion of the warm background temperature with <math>\beta</math> free
+
    50 : ENO-imaging confirmation from Planck Collab.;
|-
+
    60 : WFI-imaging confirmation from Planck Collab.;
|TEMP_WBKG_LOW1 || real*8 || K || Lower 68% confidence limit of the warm background temperature with <math>\beta</math> free
+
    65 : NTT-spectroscopic confirmation from Planck Collab.;
|-
+
    500 : RTT-spectroscopic confirmation from Planck Collab.;
|TEMP_WBKG_UP1 || real*8 || K || Upper 68% confidence limit of the warm background temperature with <math>\beta</math> free
+
    600 : NOT-spectroscopic confirmation from Planck Collab.;
|-
+
    650 : GEMINI-spectroscopic confirmation from Planck Collab.;
|BETA_WBKG || real*8 || || Spectral index <math>\beta</math> of the warm background (see note 6)
+
    700 : ENO-spectroscopic confirmation from Planck Collab.
|-
+
 
|BETA_WBKG_SIG || real*8 || || 1<math>\sigma</math> uncertainty (from MCMC) of the emissivity spectral index <math>\beta</math> of the warm background
+
'''Caveats'''
|-
+
 
|BETA_WBKG_LOW1 || real*8 || || Lower 68% confidence limit of the emissivity spectral index <math>\beta</math> of the warm background
+
The following issue was found in Feb. 2014 in R1.11 of the MMF3 catalogue: the POS_ERR field values are overestimated by a factor 3.125 on average.  This issue has been resolved in R1.12.  A corrected version of the union catalogue has also been produced (also R1.12)
|-
+
 
|BETA_WBKG_UP1 || real*8 || || Upper 68% confidence limit of the emissivity spectral index <math>\beta</math> of the warm background
+
The approximate 68% (1-sigma) confidence interval in the POS_ERR field is computed as half of the 95% (2&sigma;) confidence interval. Previously this was erroneously described as a 95% confidence interval.
|-
+
 
|TEMP_BETA2_WBKG || real*8 || K || Temperature of the warm background with <math>\beta</math> = 2
+
 
|-
+
==References==
|TEMP_BETA2_WBKG_SIG || real*8 || K || 1<math>\sigma</math> uncertainty on the temperature of the warm background with <math>\beta</math> = 2
+
<References/>
|-
 
|TEMP_BETA2_WBKG_LOW1 || real*8 || K || Lower 68% confidence limit of the warm background temperature with <math>\beta</math> = 2
 
|-
 
|TEMP_BETA2_WBKG_UP1 || real*8 || K || Upper 68% confidence limit of the warm background temperature with <math>\beta</math> = 2
 
|- bgcolor="ffdead" 
 
! colspan="4" | Physical properties
 
|- bgcolor="ffdead" 
 
! FITS Keyword || Data Type || Units || Description
 
|-
 
|NH2 || real*8 || cm<sup>-2</sup> || Column density <math>N_{H_2}</math> of the clump
 
|-
 
|NH2_SIG || real*8 || cm<sup>-2</sup> || 1<math>\sigma</math> uncertainty on the column density
 
|-
 
|NH2_LOW[1,2,3] || real*8 || cm<sup>-2</sup> || Lower 68%, 95% and 99% confidence limit of the column density
 
|-
 
|NH2_UP[1,2,3]  || real*8 || cm<sup>-2</sup> || Upper 68%, 95% and 99% confidence limit of the column density
 
|-
 
|MASS || real*8 || <math>M_{o}</math> || Mass estimate of the clump
 
|-
 
|MASS_SIG  || real*8 || <math>M_{o}</math> || 1<math>\sigma</math> uncertainty on the mass estimate of the clump
 
|-
 
|MASS_LOW[1,2,3]  || real*8 || <math>M_{o}</math> || Lower 68%, 95% and 99% confidence limit of the mass estimate
 
|-
 
|MASS_UP[1,2,3]  || real*8 || <math>M_{0}</math> || Upper 68%, 95% and 99% confidence limit of the mass estimate
 
|-
 
|DENSITY || real*8 || cm<sup>-3</sup> || Mean density of the clump
 
|-
 
|DENSITY_SIG  || real*8 || cm<sup>-3</sup>  || 1<math>\sigma</math> uncertainty on the mean density estimate of the clump
 
|-
 
|DENSITY_LOW[1,2,3]  || real*8 || cm<sup>-3</sup>  || Lower 68%, 95% and 99% confidence limit of the mean density estimate
 
|-
 
|DENSITY_UP[1,2,3]  || real*8 || cm<sup>-3</sup> || Upper 68%, 95% and 99% confidence limit of the mean density estimate
 
|-
 
|SIZE || real*8 || pc || Physical size of the clump
 
|-
 
|SIZE_SIG  || real*8 || pc  || 1<math>\sigma</math> uncertainty on the physical size estimate of the clump
 
|-
 
|SIZE_LOW[1,2,3]  || real*8 || pc  || Lower 68%, 95% and 99% confidence limit of the physical size estimate
 
|-
 
|SIZE_UP[1,2,3]  || real*8 || pc || Upper 68%, 95% and 99% confidence limit of the physical size estimate
 
|-
 
|LUMINOSITY || real*8 || L<sub>o</sub> || Luminosity of the clump
 
|-
 
|LUMINOSITY_SIG  || real*8 || L<sub>o</sub>  || 1<math>\sigma</math> uncertainty on the luminosity estimate of the clump
 
|-
 
|LUMINOSITY_LOW[1,2,3]  || real*8 || L<sub>o</sub>  || Lower 68%, 95% and 99% confidence limit of the luminosity estimate
 
|-
 
|LUMINOSITY_UP[1,2,3]  || real*8 || L<sub>o</sub> || Upper 68%, 95% and 99% confidence limit of the luminosity estimate
 
|- bgcolor="ffdead" 
 
! colspan="4" | Flags
 
|- bgcolor="ffdead" 
 
! FITS Keyword || Data Type || Units || Description
 
|-
 
|XFLAG_LMC || int*4 || 0/1 || 1 if part of the LMC
 
|-
 
|XFLAG_SMC || int*4 || 0/1 || 1 if part of the SMC
 
|-
 
|XFLAG_ECC || int*4 || 0/1 || 1 if present in the ECC
 
|-
 
|XFLAG_PCCS_857 || int*4 || 0/1 || 1 if present in the PCCS 857 GHz band
 
|-
 
|XFLAG_PCCS_545 || int*4 || 0/1 || 1 if present in the PCCS 545 GHz band
 
|-
 
|XFLAG_PCCS_353 || int*4 || 0/1 || 1 if present in the PCCS 353 GHz band
 
|-
 
|XFLAG_PCCS_217 || int*4 || 0/1 || 1 if present in the PCCS 217 GHz band
 
|-
 
|XFLAG_PCCS_143 || int*4 || 0/1 || 1 if present in the PCCS 143 GHz band
 
|-
 
|XFLAG_PCCS_100 || int*4 || 0/1 || 1 if present in the PCCS 100 GHz band
 
|-
 
|XFLAG_PCCS_70 || int*4 || 0/1 || 1 if present in the PCCS 70 GHz band
 
|-
 
|XFLAG_PCCS_44 || int*4 || 0/1 || 1 if present in the PCCS 44 GHz band
 
|-
 
|XFLAG_PCCS_30 || int*4 || 0/1 || 1 if present in the PCCS 30 GHz band
 
|-
 
|XFLAG_PSZ || int*4 || 0/1 || 1 if present in the PCCS PSZ
 
|-
 
|XFLAG_PHZ || int*4 || 0/1 || 1 if present in the PCCS HZ
 
|-
 
|XFLAG_HKP_GCC || int*4 || 0/1 || 1 if present in the Herschel HKP-GCC
 
 
 
|}
 
 
 
  
  
==References==
 
<References />
 
 
 
[[Category:Mission products|005]]
 
[[Category:Mission products|005]]

Latest revision as of 12:58, 26 January 2021

The 2015 compact source catalogues will not be regenerated using data from the 2018 release and remain the most up-to-date products.

(2015) Second Catalogue of Compact Sources (PCCS2 and PCCS2E)[edit]

The second Planck Catalogue of Compact Sources (PCCS2) is a set of single-frequency source catalogues extracted from the Planck full-mission maps in intensity and polarization (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_SkyMap_???_2048_R2.00_full.fits). The catalogues have been constructed as described in PCCS and in section 2 of Planck-2015-A26[1]. The validation of the catalogues is described in section 3 of Planck-2015-A26[1].

The catalogue at 100 GHz and above has been divided into two sub-catalogues: the PCCS2, in which the sources have been detected in regions of the sky where it is possible to estimate the reliability of the detections, either statistically or by using external catalogues; and PCCS2E, in which the detected sources are located in regions of the sky where it is not possible to make an estimate of their reliability.

By definition, the reliability of the whole PCCS2 is ≥ 80%, and a flag is available that allows the user to select a subsample of sources with a higher level of reliability (e.g., 90% or 95%).

The nine Planck full-mission frequency channel maps are used as input to the source detection pipelines. They contain 48 months of data for LFI channels and 29 months of data for HFI channels. Therefore the flux densities of sources obtained from the full-mission maps are the average of at least eight observations for LFI channels or at least four observations for HFI channels. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Tables 1 and 2.

Four different photometry methods have been used. For one of the methods (the native photometry from the Mexican-hat wavelet detection algorithm), the analysis is performed on patches containing tangent-plane projections of the map. For the other methods (aperture photometry, point spread function fitting, and Gaussian fitting), the analysis is performed directly on the full-sky maps.

PCCS2 in intensity.
Sky distribution of the PCCS2 intensity sources for three different channels: 30 GHz (red circles); 143 GHz (blue circles); and 857 GHz (green circles). The size of the circles is related to the brightness of the sources and the beam size of each channel.
PCCS2E in intensity.
Sky distribution of the PCCS2E intensity sources for two different channels: 143 GHz (blue circles); and 857 GHz (green circles).

The analysis in polarization has been performed in a non-blind fashion, looking at the position of the sources previously detected in intensity. As a result, polarization flux densities and polarization angles have been measured for hundreds of sources with a significance >99.99%. This high threshold in significance has been chosen to minimize the possibility of misinterpreting a peak of the polarized background as a source. This implies that, in general, most of the polarized sources are very bright, introducing an additional selection effect.

PCCS2 in polarization.
Sky distribution of the PCCS2 polarization sources in three different channels: 30GHz (red circles); 44GHz (green circles); and 70GHz (blue circles).
Sky distribution of the PCCS2 polarization sources in four different channels: 100GHz (red circles); 143GHz (blue circles); 217GHz (green circles); and 353 GHz (black).
PCCS2E in polarization.
Sky distribution of the PCCS2E polarization sources at three different channels: 100GHz (red circles); 143GHz (blue circles); 217GHz (green circles); and 353 GHz (black).


Table 1: PCCS2 and PCCS2E characteristics.
Channel 30 44 70 100 143 217 353 545 857
Frequency [GHz] 28.4 44.1 70.4 100.0 143.0 217.0 353.0 545.0 857.0
Wavelength [μm] 10561 6807 4260 3000 2098 1382 850 550 350
Number of sources
PCCS2 1560 934 1296 1742 2160 2135 1344 1694 4891
PCCS2E 2487 4139 16842 22665 31068 43290
Union PCCS2+PCCS2E 4229 6299 18977 24009 32762 48181
Number of sources in the extragalactic zonea
PCCS2 745 367 504 1742 2160 2135 1344 1694 4891
PCCS2E 0 0 26 289 839 2097
Union PCCS2+PCSS2E 1742 2160 2161 1633 2533 6988
Flux densities [mJy] in the extragalactic zonea
PCCS2
Minimumb 376 603 444 232 147 127 242 535 720
90% completeness 426 676 489 269 177 152 304 555 791
Uncertainty 87 134 101 55 35 29 55 105 168
PCCS2E
Minimumb 189 350 597 939
90% completeness 144 311 557 927
Uncertainty 35 73 144 278

Table 1 Notes a 30-70 GHz: the extragalactic zone is defined by |b| > 30°. For 100-857 GHz the numbers outside of the Galactic region where the reliability cannot be accurately assessed. Note that for the PCCS2E the only sources that occur in this region lie in the filament mask.
b Minimum flux density of the catalogue in the extragalactic zone after excluding the faintest 10% of sources.

-
Table 2: PCCS2 & PCCS2E polarization characteristics for sources with polarized emission significance > 99.99%
Channel 30 44 70 100 143 217 353
Number of significantly polarized sources in PCCS2 122 30 34 20 25 11 1
Minimum polarized flux densitya [mJy] 117 181 284 138 148 166 453
Polarized flux density uncertainty [mJy] 46 88 91 30 26 30 81
Minimum polarized flux density for 90% completeness [mJy] 199 412 397 135 100 136 347
Minimum polarized flux density for 95% completeness [mJy] 251 468 454 160 111 153 399
Minimum polarized flux density for 100% completeness [mJy] 600 700 700 250 147 257 426
Number of significantly polarized sources in PCCS2E 43 111 325 666
Minimum polarized flux densitya [mJy] 121 87 114 348
Polarized flux density uncertainty [mJy] 52 44 55 178
Minimum polarized flux density for 90% completeness [mJy] 410 613 270 567
Minimum polarized flux density for 95% completeness [mJy] 599 893 464 590
Minimum polarized flux density for 100% completeness [mJy] 835 893 786 958

Table 2 Notes

a Minimum polarized flux density of the catalogue of significantly polarized sources after excluding the faintest 10% of sources.

Catalogues[edit]

The PCCS2 catalogues (at each frequency) are contained in the FITS files

COM_PCCS_030_R2.04.fits
COM_PCCS_044_R2.04.fits
COM_PCCS_070_R2.04.fits
COM_PCCS_100_R2.01.fits
COM_PCCS_143_R2.01.fits
COM_PCCS_217_R2.01.fits
COM_PCCS_353_R2.01.fits
COM_PCCS_545_R2.01.fits
COM_PCCS_857_R2.01.fits .

The PCCS2E catalogues are contained in the FITS files

COM_PCCS_100-excluded_R2.01.fits
COM_PCCS_143-excluded_R2.01.fits
COM_PCCS_217-excluded_R2.01.fits
COM_PCCS_353-excluded_R2.01.fits
COM_PCCS_545-excluded_R2.01.fits
COM_PCCS_857-excluded_R2.01.fits

The structure of these files is as follows.

PCCS2/PCCS2E FITS file structure
Extension 0: Primary header, no data
FITS keyword Data type Units Description
INSTRUME String Instrument (LFI / HFI)
VERSION String Version of PCCS (PCCS2 / PCCS2_E)
DATE String Date file created: yyyy-mm-dd
ORIGIN String Name of organization responsible for the data (LFI-DPC / HFI-DPC)
TELESCOP String Telescope (PLANCK)
CREATOR String Pipeline version
DATE-OBS String days Beginning of the survey: yyyy-mm-dd
DATE-END String days End of the survey: yyyy-mm-dd
FWHM Real*4 arcmin FWHM from an elliptical Gaussian fit to the effective beam
OMEGA_B Real*4 arcmin2 Area of the effective beam
FWHM_EFF Real*4 arcmin FWHM computed from OMEGA_B assuming beam is Gaussian
OMEGA_B1 Real*4 arcmin2 Beam area within a radius of 1 × FWHM_EFF
OMEGA_B2 Real*4 arcmin2 Beam area within a radius of 2 × FWHM_EFF
Extension 1: BINTABLE, EXTNAME = PCCS2_fff (where fff is the frequency channel)
Column Name Data type Units Description
Identification
NAME String Source name (see note 1)
Source position
GLON Real*8 deg Galactic longitude based on extraction algorithm
GLAT Real*8 deg Galactic latitude based on extraction algorithm
RA Real*8 deg Right ascension (J2000) transformed from (GLON,GLAT)
DEC Real*8 deg Declination (J2000) transformed from (GLON,GLAT)
Photometry
DETFLUX Real*4 mJy Flux density of source as determined by detection method
DETFLUX_ERR Real*4 mJy Uncertainty (1 σ) in derived flux density from detection method
APERFLUX Real*4 mJy Flux density of source as determined from aperture photometry
APERFLUX_ERR Real*4 mJy Uncertainty (1 σ) in derived flux density from aperture photometry
PSFFLUX Real*4 mJy Flux density of source as determined from PSF fitting
PSFFLUX_ERR Real*4 mJy Uncertainty (1 σ) in derived flux density from PSF fitting
GAUFLUX Real*4 mJy Flux density of source as determined from 2-D Gaussian fitting
GAUFLUX_ERR Real*4 mJy Uncertainty (1 σ) in derived flux density from 2-D Gaussian fitting
GAU_SEMI1 Real*4 arcmin Gaussian fit along axis 1 (FWHM; see note 2 for axis definition)
GAU_SEMI1_ERR Real*4 arcmin Uncertainty (1 σ) in derived Gaussian fit along axis 1
GAU_SEMI2 Real*4 arcmin Gaussian fit along axis 2 (FWHM)
GAU_SEMI2_ERR Real*4 arcmin Uncertainty (1 σ) in derived Gaussian fit along axis 2
GAU_THETA Real*4 deg Gaussian fit orientation angle (see note 2)
GAU_THETA_ERR Real*4 deg Uncertainty (1 σ) in derived Gaussian fit orientation angle
GAU_FWHM_EFF Real*4 arcmin Gaussian fit effective FWHM
Polarization measurements (30-353 GHz only)
P Real*4 mJy Polarization flux density of the sources as determined by a matched filter (see note 3)
P_ERR Real*4 mJy Uncertainty (1 σ) in derived polarization flux density (see note 3)
ANGLE_P Real*4 degrees Orientation of polarization with respect to NGP (see notes 2 and 3)
ANGLE_P_ERR Real*4 degrees Uncertainty (1 σ) in orientation of polarization (see note 3)
APER_P Real*4 mJy Polarization flux density of the sources as determined by aperture photometry (see note 3)
APER_P_ERR Real*4 mJy Uncertainty (1 σ) in derived polarization flux density (see note 3)
APER_ANGLE_P Real*4 degrees Orientation of polarization with respect to NGP (see notes 2 and 3)
APER_ANGLE_P_ERR Real*4 degrees Uncertainty (1 σ) in orientation of polarization (see note 3)
P_UPPER_LIMIT Real*4 mJy Polarization flux density 99.99% upper limit. This is provided only when the P column is set to NULL; otherwise this column itself contains NULL.
APER_P_UPPER_LIMIT Real*4 mJy Polarization flux density 99.99% upper limit. This is provided only when the APER_P column is set to NULL; otherwise this column itself contains NULL.
Marginal polarization measurements (100-353 GHz only) – see note 4
P_STAT Integer*2 Polarization detection status
PX Real*4 mJy Polarization flux density of the sources as determined by a matched filter using a Bayesian polarization estimator
PX_ERR_LOWER Real*4 mJy PX uncertainty; lower 95% error bar
PX_ERR_UPPER Real*4 mJy PX uncertainty; upper 95% error bar
ANGLE_PX Real*4 deg Orientation of polarization with respect to NGP using Bayesian polarization estimator (see note 2)
ANGLE_PX_ERR_LOWER Real*4 deg ANGLE_PX uncertainty; lower 95% error bar
ANGLE_PX_ERR_UPPER Real*4 deg ANGLE_PX uncertainty; upper 95% error bar
Flags and validation
EXTENDED Integer*2 Extended source flag (see note 5)
EXT_VAL Integer*2 External validation flag (see note 6)
ERCSC String Name of the ERCSC counterpart, if any
PCCS String Name of the PCCS counterpart, if any
Flags and validation (PCCS2 only)
HIGHEST_RELIABILITY_CAT Integer*4 See note 7
Flags and validation (PCCS2E, 100-857 GHz only)
WHICH_ZONE Integer*2 See note 8
Flags and validation (217-857 GHz only)
CIRRUS_N Integer*2 Number of sources (S/N > 5) detected at 857 GHz within a 1° radius.
SKY_BRIGHTNESS Real*4 MJy sr-1 The mean 857 GHz brightness within a 2° radius. This may be used as another indicator of cirrus contamination.
Flux densities at other frequencies (857 GHz only)
APERFLUX_217 Real*4 mJy Estimated flux density at 217 GHz
APERFLUX_ERR_217 Real*4 mJy Uncertainty in flux density at 217 GHz
APERFLUX_353 Real*4 mJy Estimated flux density at 353 GHz
APERFLUX_ERR_353 Real*4 mJy Uncertainty in flux density at 353 GHz
APERFLUX_545 Real*4 mJy Estimated flux density at 545 GHz
APERFLUX_ERR_545 Real*4 mJy Uncertainty in flux density at 545 GHz

Notes

  1. Format is PCCS2 fff Glll.ll±bb.bb for sources in the PCCS2 and PCCS2E fff Glll.ll±bb.bb for sources in the PCCS2E, where "fff" is the frequency channel and l and b the position of the source in Galactic coordinates truncated to two decimal places.
  2. We follow the IAU/IEEE convention (Hamaker & Bregman 1996) for defining the angle of polarization of a source in this catalogue, and this convention is also used for the other angles in the catalogue. The angle is measured from the North Galactic Pole in a clockwise direction from -90° to 90°. Note that this is different than the convention used for the CMB maps.
  3. Provided when the significance of the polarization measurement is > 99.99% and set to NULL otherwise.
  4. The P_STAT flag gives the status of the marginal polarization detection. Possible values are:
    3 – bright, the P field filled in and all PX fields set to NULL;
    2 – significant, the P field is set to NULL, 0 is outside the PX 95% HPD, and all PX fields are filled;
    1 – marginal, the P field is set to NULL, 0 is inside the PX 95% HPD (but the mode of the PX posterior distribution is not 0) and all PX fields are filled;
    0 – no detection, the P field is set to NULL, the mode of the PX posterior distribution is 0, PX_ERRL, ANGLE_PX, ANGLE_PX_ERR_LOWER, and ANGLE_PX_ERR_UPPER are set to NULL.
  5. The EXTENDED flag has the value of "0" if the source is compact and the value of "1" if it is extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criterion for extension being √(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
  6. The EXT_VAL flag gives the status of the external validation. Possible values are:
    3 – the source has a clear counterpart in one of the catalogues used as ancillary data;
    2 – the source does not have a clear counterpart in one of the catalogues used as ancillary data, but it has been detected by the internal multi-frequency method;
    1 – the source does not have a clear counterpart in one of the catalogues used as ancillary data and it has not been detected by the internal multi-frequency method, but it has been detected in a previous Planck source catalogue;
    0 – the source does not have a clear counterpart in one of the catalogues used as ancillary data and has not been detected by the internal multi-frequency method.
  7. The HIGHEST_RELIABILTY_CAT column contains the highest reliability catalogue to which the source belongs. As the full catalogue reliability is ≥ 80%, this is the lowest possible value in this column. Where possible this is provided in steps of 1%, otherwise it is in steps of 5%.
  8. The WHICH_ZONE column encodes the zone in which the source lies:
    1 – source lies inside the filament mask;
    2 – source lies inside the Galactic zone;
    3 – sources lies in both the filament mask and Galactic zone.

Zone map[edit]

For each HFI frequency channel there is an associated map that defines where the quantified-reliability (PCCS2) and unquantified-reliability (PCCS2E) zones are on the sky.

The files are called

COM_PCCS_100-zoneMask_R2.01.fits
COM_PCCS_143-zoneMask_R2.01.fits
COM_PCCS_217-zoneMask_R2.01.fits
COM_PCCS_353-zoneMask_R2.01.fits
COM_PCCS_545-zoneMask_R2.01.fits
COM_PCCS_857-zoneMask_R2.01.fits .

The structure of the files is shown in the following table.

Zone map FITS file structure
Extension 0: Primary header, no data
FITS keyword Data type Units Description
DATE String Date of creation of file
Extension 1: BINTABLE, HEALPix map (see note 1)
FITS keyword Data type Value Description
PIXTYPE String HEALPIX HEALPix pixelation
ORDERING String RING Pixel ordering
NSIDE Int*4 2048 HEALPix resolution parameter
NPIX Int*4 50331648 Number of pixels
COORDSYS String G Coordinate system
FREQ_CHL String Frequency channel

Notes

  1. This FITS extension contains an integer HEALPix map, which encodes the information on which of four possible regions on the sky each pixel belongs to:
    0 – quantified-reliability zone (PCCS2);
    1 – filament mask;
    2 – Galactic zone;
    3 – filament mask and Galactic zone.

S/N threshold map[edit]

For each HFI frequency channel there are a number of maps that contains the S/N threshold used to accept sources into the PCCS2 and PCCS2E catalogues.

For the full catalogue (80% reliability in the quantified reliability zone) they are

COM_PCCS_100-SN-threshold_R2.01.fits
COM_PCCS_143-SN-threshold_R2.01.fits
COM_PCCS_217-SN-threshold_R2.01.fits
COM_PCCS_353-SN-threshold_R2.01.fits
COM_PCCS_545-SN-threshold_R2.01.fits
COM_PCCS_857-SN-threshold_R2.01.fits .

For 85% reliability they are

COM_PCCS_100-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_143-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_217-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_353-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_545-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_857-SN-threshold-85pc-reliability_R2.01.fits .

For 90% reliability they are

COM_PCCS_100-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_143-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_217-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_353-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_545-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_857-SN-threshold-90pc-reliability_R2.01.fits .

For 95% reliability they are

COM_PCCS_100-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_143-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_217-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_353-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_545-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_857-SN-threshold-95pc-reliability_R2.01.fits .

The structure of the files is shown in the following table.

Zone map FITS file structure
Extension 0: Primary header, no data
FITS keyword Data type Units Description
DATE String Date of creation of file
Extension 1: BINTABLE, HEALPix map (see note 1)
FITS keyword Data type Value Description
PIXTYPE String HEALPIX HEALPix pixelation
ORDERING String RING Pixel ordering
NSIDE Int*4 2048 HEALPix resolution parameter
NPIX Int*4 50331648 Number of pixels
COORDSYS String G Coordinate system
FREQ_CHL String Frequency channel

Notes

  1. This FITS extension contains a single precision HEALPix map of the S/N threshold applied in the generation of the catalogue at that position on the sky.

Noise map[edit]

For each HFI frequency channel there is an associated map that contains the detection noise as a function of position on the sky.

The files are called

COM_PCCS_100-noise-level_R2.01.fits
COM_PCCS_143-noise-level_R2.01.fits
COM_PCCS_217-noise-level_R2.01.fits
COM_PCCS_353-noise-level_R2.01.fits
COM_PCCS_545-noise-level_R2.01.fits
COM_PCCS_857-noise-level_R2.01.fits .

The structure of the files shown in the following table.

Zone map FITS file structure
Extension 0: Primary header, no data
FITS keyword Data type Units Description
DATE String Date of creation of file
Extension 1: BINTABLE, HEALPix map (see note 1)
FITS keyword Data type Value Description
PIXTYPE String HEALPIX HEALPix pixelation
ORDERING String RING Pixel ordering
NSIDE Int*4 2048 HEALPix resolution parameter
NPIX Int*4 50331648 Number of pixels
COORDSYS String G Coordinate system
FREQ_CHL String Frequency channel

Notes

  1. This FITS extension contains a single precision HEALPix map of the detection noise at each location on the sky, in units of Jy.


Previous releases: (2013) PCCS and (2011) ERCSC[edit]


Second Planck Release (2013): Description of the PCCS

The Catalogue of Compact Sources


Product description

Sky distribution of the PCCS sources at three different channels: 30GHz (pink circles), 143GHz (magenta circles) and 857GHz (green circles). The dimension of the circles is related to the brightness of the sources and the beam size of each channel.

The PCCS is a set of nine single-frequencies lists of sources extracted from the Planck nominal mission data. By definition its reliability is > 80% and a special effort was made to use simple selection procedures in order to facilitate statistical analyses. With a common detection method for all the channels and the additional three photometries, spectral analysis can also be done safely. The deeper completeness levels and, as a consequence, the higher number of sources compared with its predecessor the ERCSC, will allow the extension of previous studies to more sources and to fainter flux densities. The PCCS is the natural evolution of the ERCSC, but both lack polarization and multi-frequency information. Future releases will take advantage of the full mission data and they will contain information on properties of sources not available in this release, such as polarization, multi-frequency and variability.


Table 1: PCCS characteristics
Channel 30 44 70 100 143 217 353 545 857
Frequency [GHz] 28.4 44.1 70.4 100.0 143.0 217.0 353.0 545.0 857.0
Beam FWHM1 [arcmin] 32.38 27.10 13.30 9.88 7.18 4.87 4.65 4.72 4.39
S/N threshold 4.0 4.0 4.0 4.6 4.7 4.8 4.92/6.03 4.7/7.0 4.9/7.0
# of detections 1256 731 939 3850 5675 16070 17689 26472 35719
# of detections for |b| > 30º) 572 258 332 845 1051 1901 2035 4164 7851
Flux density uncertainty [mJy] 109 198 149 61 38 35 74 132 189
Min flux density4 [mJy] 461 825 566 266 169 149 298 479 671
90% completeness [mJ] 575 1047 776 300 190 180 330 570 680
Position uncertainty5 [arcmin] 1.8 2.1 1.4 1.0 0.7 0.7 0.8 0.5 0.4


Notes

  1. The Planck beams are described in Planck-2013-IV[2] and Planck-2013-VII[3]. This table shows the values which were adopted for the PCCS (derived from the effective beams).
  2. In the extragalactic zone (48% of the sky; see Fig. 2 in Planck-2013-XXVIII[4]).
  3. In the Galactic zone (52% of the sky; see Fig. 2 in Planck-2013-XXVIII[4]).
  4. Minimum flux density of the catalogue at |b| > 30º after excluding the 10% faintest sources.
  5. Positional uncertainty derived by comparison with PACO sample ([5][6][7]) up to 353 GHz and with Herschel samples (HRS, KINGFISH, HeViCS, H-ATLAS) in the other channels.

Before using the PCCS, please read the Cautionary Notes in the PCCS general description section. For full details, see paper Planck-2013-XXVIII[4].

Production process

For a description of the production and validation processes of the PCCS see the corresponding section.

Inputs

The data obtained from the Planck nominal mission between (2009 August 12 and 2010 November 27) have been processed into full-sky maps by the HFI and LFI Data Processing Centres (DPCs). A description of the processing can be found in Planck-2013-II[8] and Planck-2013-VI[9]. The data consist of two complete sky surveys and 60% of the third survey. This implies that the flux densities of sources obtained from the nominal mission maps are the average of at least two observations. The nine Planck frequency channel maps are used as input to the source detection pipelines. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Table 1.

The input data used to generate this product are the following:

Related products

Other products that are related and share some commonalities with the product being described here are the other catalogues:

  1. ERCSC
  2. SZ catalogue

File names

COM_PCCS_030_R1.30.fits
COM_PCCS_044_R1.30.fits
COM_PCCS_070_R1.30.fits
COM_PCCS_100_R1.20.fits
COM_PCCS_143_R1.20.fits
COM_PCCS_217_R1.20.fits
COM_PCCS_353_R1.20.fits
COM_PCCS_545_R1.20.fits
COM_PCCS_857_R1.20.fits

Meta Data

The PCCS source list in each frequency is structured as a FITS binary table having one row for each detected source. The details of the FITS file structure are below

FITS file structure
Extension 0: Primary header, no data
FITS keyword Data type Units Description
INSTRUME String LFI or HFI
VERSION String Version of PCCS
DATE String Date file created:yyyy-mm-dd
ORIGIN String Name of organization responsible for the data (LFI-DPCHFI-DPC)
TELESCOP String PLANCK
CREATOR String Pipeline Version
DATE-OBS String days Start-up time of the survey: yyyy-mm-dd
DATE-END String days Ending time of the survey: yyyy-mm-dd
Extension 1: (BINTABLE)
Column Name Data type Units Description
Identification
NAME String Source name (note 1)
Source Position
GLON Real*8 degrees Galactic longitude based on extraction algorithm
GLAT Real*8 degrees Galactic latitude based on extraction algorithm
RA Real*8 degrees Right ascension (J2000) transformed from (GLON,GLAT)
DEC Real*8 degrees Declination (J2000) transformed from (GLON,GLAT)
Photometry
DETFLUX Real*4 mJy Flux density of source as determined by detection method
DETFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from detection method
APERFLUX Real*4 mJy Flux density of source as determined from the aperture photometry
APERFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from the aperture photometry
PSFFLUX Real*4 mJy Flux density of source as determined from PSF fitting
PSFFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from PSF fitting
GAUFLUX Real*4 mJy Flux density of source as determined from 2-D Gaussian fitting
GAUFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from 2-D Gaussian fitting
GAU_SEMI1 Real*4 arcmin Gaussian fit along axis 1 (FWHM; see note 4 for axis definition)
GAU_SEMI1_ERR Real*4 arcmin Uncertainty (1 sigma) in derived Gaussian fit along axis 1
GAU_SEMI2 Real*4 arcmin Gaussian fit along axis 2 (FWHM)
GAU_SEMI2_ERR Real*4 arcmin Uncertainty (1 sigma) in derived Gaussian fit along axis 2
GAU_THETA Real*4 deg Gaussian fit orientation angle (note 4)
GAU_THETA_ERR Real*4 deg Uncertainty (1 sigma) in derived gaussian fit orientation angle
GAU_FWHM_EFF Real*4 arcmin Gaussian fit effective FWHM
Flags and validation
EXTENDED Integer*2 Extended source flag (note 2)
CIRRUS_N Integer*2 Number of sources detected at 857 GHz within 1 degree
EXT_VAL Integer*2 External validation flag (note 3)
ERCSC String Name of the ERCSC counterpart if any
ONLY 857 GHz Catalogue
APERFLUX_217 Real*4 mJy Estimated flux density at 217 GHz
APERFLUX_ERR_217 Real*4 mJy Uncertainty in source flux density at 217 GHz
APERFLUX_353 Real*4 mJy Estimated flux density at 353 GHz
APERFLUX_ERR_353 Real*4 mJy Uncertainty in source flux density at 353 GHz
APERFLUX_545 Real*4 mJy Estimated flux density at 545 GHz
APERFLUX_ERR_545 Real*4 mJy Uncertainty in source flux density at 545 GHz


Notes

  1. Source names consist of a prefix and a position. The prefix used is PCCS1 fff for the catalogue at fff GHz. The position is in Galactic coordinates and specified as "Glll.ll±bb.bb" where the (l,b) values are truncated to two decimal places. For example, a source detected at (l,b) = (120.237, 4.231) in the 545 GHz Planck map would be labelled PCCS1 545 G120.23±04.23.
  2. The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criteria for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
  3. The EXT_VAL flag takes the value of 0, 1, or 2, based on the following conditions:
    = 2: The source has a clear counterpart in one of the catalogues considered as ancillary data.
    = 1: The source has no clear counterpart in one of the ancillary catalogues but it has been detected by the internal multi-frequency method (LFI channels) or match with neighbouring frequencies, above or below (HFI channels).
    = 0: The source has no clear counterpart in one of the ancillary catalogues and it has not been detected by the internal multi-frequency method or neighbouring frequencies.
  4. The x-axis is defined for each source as parallel to the line of constant colatitude, with the same direction as the longitude. Therefore the position angles are measured anticlockwise from the y-axis.


First Planck Release (2011): Description of the 2011 ERCSC (Early Compact Source, Cold Core and SZ Catalogues )

The ERCSC

The Plank Early Release Compact Source Catalogue was the first Planck product to be publicly released in Jan 2011. It was produced with a very rapid turnaround to facilitate follow-up observations with existing cryogenic observatories such as Herschel. It contained a list of all high reliability sources, both Galactic and extragalactic, that were derived from the first all sky coverage by Planck. i.e., using observations obtained from 12 August 2009 to 6 June 2010. Thus the full sky was covered once, and ~60% of the sky was covered twice. The goals were to achieve a photometric accuracy of 30% and a positional accuracy 1/5 of the beam FWHM in the RMS sense.

The ERCSC consisted of nine source lists, one at each of the nine Planck frequency channels. The number of sources in the lists range from 705 at 30 GHz to 8988 at 857 GHz. No attempt was made to cross-match the sources from the different frequencies due to the wide range of spatial resolutions (33 arcmin at 30 GHz to 4.3 arcmin at 857 GHz) spanned by Planck. Furthermore, a list of Cold Cores of interstellar molecular clouds within the Galaxy and a list of galaxy clusters detected through the Sunyaev- Zel’dovich effect (SZ), were also provided. These consisted of candidate sources that were detected using multifrequency algorithms that use the distinct spectral signature of such sources. The Cold Cores catalogue contained 915 sources while the SZ cluster catalogue consisted of 189 sources

In order to generate the ERCSC, four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is >90%. Reliability is defined as the fraction of sources in the catalog which have measured flux densities which are within 30% of their true flux density. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10σ photometric flux density limit of the catalogue at |b| > 30° is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The sensitivity of the ERCSC is shown in the figure below. The ERCSC sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared-luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs.

The multifrequency information from Planck allows some basic classification of the sources to be undertaken. In the Galactic plane, at frequencies below 100 GHz, the majority of the sources are dominated by synchrotron or free-free emission. At the higher frequencies, the sources are almost exclusively dominated by thermal dust emission. At high Galactic latitudes however, the synchrotron sources dominate the source counts to 217 GHz with dusty sources being the primary source population at 353 GHz and higher. Recent attempts to classify a subset of the Planck 857 GHz sources at high latitudes based on cross-correlations with sources in other catalogs such as WISE and SDSS, found that almost half of them are associated with stars and low-redshift galaxies while a significant fraction (44%) might be interstellar medium features[10].

Full details on the construction, contents and usage of the ERCSC, ECC and ESZ catalogues can be found in Planck-Early-VII[11], Planck-Early-VIII[12], Planck-Early-XXIII[13].


Flux density limits


The figure shows the ERCSC flux density limits, quanitfied as the faintest ERCSC source at |b|<10 deg (dashed black line) and at |b|>30 deg (solid black line), compared to those of other wide area surveys (Planck-Early-VII[11]). Also shown are spectra of known sources of foreground emission as red lines. The ERCSC sensitivity is worse in the Galactic plane due to the strong contribution of ISM emission, especially at submillimeter wavelengths. At face value, the WMAP and Planck flux density limits appear to be comparable at the lowest frequencies, but the Planck ERCSC is much more complete as discussed in Planck-Early-VII[11].

(2015) Bayesian Extraction and Estimation Package (BeeP) reprocessing of PCCS2+PCCS2E at 857 GHz[edit]

BeeP’s catalogue was developed using the data and the methodology described in the companion paper Planck-2020-LV[14].

Traits:

  • It is a catalogue of compact objects.
  • It is the result of a ‘non-blind’ exercise where Planck’s PCCS2+2E catalogue positions at 857 GHz were used. It contains exactly the same number of rows as the original catalogue and no attempt of detecting new sources was made.
  • It is a parametric Bayesian multi-channel algorithm. The source parameter estimates are derived from the posterior distributions of a data model likelihood.
  • It employs Planck all-sky temperature maps at [math]353, 545, 857[/math] GHz channels from the Planck 2015 release and the [math]3000[/math] GHz IRIS map, a reprocessed IRAS map.

The catalogue product is made of three components:

  • A table with source parameter estimates and uncertainty summary statistics: COM_PCCS_BEEP_R2.00.fits.
  • A collection of Spectral Energy Density (SED) figures. Not yet available
  • A collection of figures with the parameter posterior distributions. Not yet available

Table of source parameter estimates.[edit]

The table with the source parameters contains 48181 rows, as many as in Planck 857 GHz channel PCCS2 and PCCSE catalogues combined. Each row has 108 fields (columns). If a field value is ill defined or not available, then its value is set to largest negative value of the double type in the IEEE standard: [math]\approx -1.797693 \times 10^{305}[/math]. The table of source parameter estimates (columns) is divided into 5 sections:

General
Contains fields that are independent of the physical model used to described the source, or background, emission. It holds the reliability assessment fields (see section A.1.2 and 6.2.3 of the companion paper).

  • BeeP position columns were obtained using the MBB SED model.
  • If a likelihood maximum was not found, then MAXFOUND is set to [math]0[/math], otherwise is [math]1[/math].
  • NPSNR is BeeP’s proxy for the Signal-to-Noise Ratio (SNR) in a statistical sense (detection significance) like ‘how many sigmas this detection is’. It cannot be read as the flux density divided by the flux density error bar. A Gaussian homogeneous background is assumed.
  • SRCSIG is BeeP’s detection significance. It is derived from NPSNR with a non-Gaussianity correction based on RELTH applied.
  • EST_QUALITY indicates the expected quality of the source parameter estimates. The highest quality is 5. Then, if a source does not meet the conditions in table, the correspondent penalty is subtracted.
  • The field "NAME" has the exact same source name as in Planck’s 857 GHz channel PCCS2+2E and should be used to reference any source in this catalogue.

Thermal sub-catalogue (see section 6.2.1 of the companion paper)

  • The sources Spectral Energy Density (SED) was modeled after a Modified Black-Body (MBB) with [math]3[/math] parameters: Temperature ([math]T[/math]), Spectral index ([math]\beta[/math]) and Flux density at a reference channel ([math]S_{\textsf{ref}}[/math]).
  • The MBB parameters, together with the source radius and position, make the likelihood parameter set.
  • Colour correction coefficients were included in the likelihood.

‘Free’ amplitude at each channel sub-catalogue
Contains a sub-catalogue of independent flux density measurements (not dependent on a SED physical model) at each of the utilized channels (see section A.1.2 of the companion paper).

  • Main goal was to allow a direct comparison with catalogues obtained at each channel independently. No source SED model was used
  • The likelihood parameter set was the flux density at each channel plus source position and radius. The best fit flux densities at each channel and error bars were computed from the flux density posterior distributions. With the [math]4[/math] pairs {[math]S_\nu,\sigma_{S_\nu}[/math]}, a MBB curve was fitted using a Gaussian likelihood.
  • During the estimation of the initial flux densities at each channel, colour-correction was not used. However when later fitting the MBB parameters colour-correction coefficients were included.

Background thermal properties catalogue (see section 6.3 of the companion paper)

  • Main goal was to provide a measurement of the contrast between the thermal properties of the background and the source.
  • The average brightness around each PCCS2+2E position ([math]32\times32[/math] pixels; [math]\approx 55'\times55'[/math]) and its standard deviation were computed for each individual channel. The map offset levels had previously been corrected.
  • With the [math]4[/math] pairs {[math]B_\nu,\sigma_{B_\nu}[/math]}, a MBB curve with colour correction, was fitted using a Gaussian likelihood.
  • The Signal-to-Noise Ratio Raw (SNRr) was computed by dividing the source average brightness at each channel by the background brightness standard deviation. The source average brightness was estimated by dividing the MBB flux density estimate at that frequency by the total solid angle resulting from the convolution of the beam, at that channel, and the intrinsic source extension.

Source ID and association fields
Adds a BeeP source index. Contains the separation between BeeP’s catalogue positions and those in Planck’s 857 PCCS2+2E and flags potential multiple detections of the same physical object. The field BEEPSRCASS contains either the same index as that of the source or the index of a close neighbour if it is inside a radius of [math]8'[/math] and its NPSNR is higher.

FullSkyTempMol 3 01.png
Sky distribution of the sources Modified Black Body (MBB) model temperatures in the catalogue (colour scale in thermodynamic kelvins). Bottom: Spectral indices of the MBB model.


FullSkyBetaMol 3 01.png
Spectral indices of the MBB model.


FullSkySrcsigMol 3 01.png
Sky distribution of the sources [math]\log_{10}[/math]SRCSIG statistic (colour scale). Sources inside the IRIS mask were not included. Sources inside the IRIS mask were not included.
Flux density corrections Recommended values for the flux density error bar correction [math]c[/math] (mJy)
Set location c (mJy)
PCCS2 Planck’s PCCS2 region 57
PCCS2E [math]\wedge \, |glat| \gt 10^\circ[/math] Planck’s PCCS2E region and [math]|glat| \gt 10^\circ[/math] 168
[math]|glat| \leq 10^\circ[/math] [math]|glat| \leq 10^\circ[/math] 820

Description of the catalogue columns.[edit]

BeeP Columns Description of the fields in the table component of the catalogue.
Field name Type Size Units Description Comments
NAME char 20 PCCS2+2E Source name
PCCS2RA double 8 Degrees J2000 RA in PCCS2+2E
PCCS2DEC double 8 Degrees J2000 DEC in PCCS2+2E
BEEPGLON double 8 Degrees Galactic longitude estimated by BeeP Average of 95% highest likelihood samples
BEEPGLAT double 8 Degrees Galactic latitude estimated by BeeP Average of 95% highest likelihood samples
BEEPRA double 8 Degrees J2000 RA estimated by BeeP Computed from BEEPGLON and BEEPGLAT
BEEPDEC double 8 Degrees J2000 DEC estimated by BeeP Computed from BEEPGLON and BEEPGLAT
PCCS2GLON double 8 Degrees Galactic longitude in PCCS2+2E
PCCS2GLAT double 8 Degrees Galactic latitude in PCCS2+2E
NPSNR double 8 Unitless Source detection significance uncorrected Background assumed Gaussian (see section A.1.2 of PIP LV)
RELTH double 8 Unitless 95% percentile of the likelihood background statistic Used to correct for the background non-gaussinaty (see section A.1.2 of PIP LV)
ACCEPT double 8 Unitless Sample acceptance ratio of the MCMC chain If low ([math]\lt 10\%[/math]) might be indicative of unreliable estimates
INPIX double 8 Unitless Percentage of pixels in-painted in the field Very high numbers might indicate unreliable estimates
MAXFOUND double 8 0 / 1 If a likelihood maximum was found within a radius of 3 pixels from the original location If a maximum is not found this is an indication that BeeP’s position might not be a compact source
SRCSIG double 8 Unitless Source detection significance Corrected for background non-gaussianity (see section A.1.2 of PIP LV)
EST_QUALITY double 8 Unitless Source parameter estimates quality flag [5 - 0]. Quality starts at 5 and the penalties in table [table:QualityPenalties] are applied. Higher values mean higher quality.
POSERR double 8 Arcmin Source position uncertainty. Radius of uncertainty around source best fit position [math]\sigma; \sigma[/math] is the Rayleigh distribution scale factor (see section 6.2.3 of PIP LV)
BETA double 8 Unitless Source spectral index (MBB); Modified Black Body Posterior median value
BETAL2SB double 8 Unitless Source spectral index uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
BETAH2SB double 8 Unitless Source spectral index uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
TEMP double 8 Kelvin Source temperature (MBB); Modified Black Body Posterior median value
TL2SB double 8 Kelvin Source temperature uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
TH2SB double 8 Kelvin Source temperature uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
EXT double 8 Arcmin Source extension before beam convolution This radius is constant across all channels. The extension parameter was obtained with likelihood beam widths (see section A.2.3 of PIP LV); Posterior median value
EXTL2SB double 8 Arcmin Source extension uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
EXTH2SB double 8 Arcmin Source extension uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
R double 8 Arcmin Source radius before beam convolution This radius is constant across all channels. The parameter was computed from EXT and gives an indication of whether the source is extended (see section 6.2.2 of PIP LV)
SREF double 8 Jy Flux density at the reference frequency Reference frequency is [math]857[/math] GHz; Posterior median value
SREFL2SB double 8 Jy Flux density at the reference frequency uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
SREFH2SB double 8 Jy Flux density at the reference frequency uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
S3000 double 8 Jy Flux density at [math]3000[/math] GHz; MBB predicted at [math]3000[/math] GHz Posterior median value
S3000L2SB double 8 Jy Flux density at [math]3000[/math] GHz uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
S3000H2SB double 8 Jy Flux density at [math]3000[/math] GHz uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
S857 double 8 Jy Flux density at [math]857[/math] GHz; MBB predicted at [math]857[/math] GHz Posterior median value
S857L2SB double 8 Jy Flux density at [math]857[/math] GHz uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
S857H2SB double 8 Jy Flux density at [math]857[/math] GHz uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
S545 double 8 Jy Flux density at [math]545[/math] GHz; MBB predicted at [math]545[/math] GHz Posterior median value
S545L2SB double 8 Jy Flux density at [math]545[/math] GHz uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
S545H2SB double 8 Jy Flux density at [math]545[/math] GHz uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
S353 double 8 Jy Flux density at [math]353[/math] GHz; MBB predicted at [math]353[/math] GHz Posterior median value
S353L2SB double 8 Jy Flux density at [math]353[/math] GHz uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
S353H2SB double 8 Jy Flux density at [math]353[/math] GHz uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
BETAMLIKE double 8 Unitless Source spectral index (MBB); Modified Black Body Maximum likelihood estimate
TEMPMLIKE double 8 Kelvin Source temperature (MBB); Modified Black Body Maximum likelihood estimate
SREFMLIKE double 8 Jy Flux density at reference frequency; Modified Black Body Maximum likelihood estimate
FREEGLON double 8 Degrees Galactic longitude (FREE channel amplitudes) Average of 95% highest likelihood samples
FREEGLAT double 8 Degrees Galactic latitude (FREE channel amplitudes) Average of 95% highest likelihood samples
FREES3000 double 8 Jy Flux density at [math]3000[/math] GHz; Estimated directly at the IRIS map Posterior median value
FREES3000L2SB double 8 Jy Flux density at [math]3000[/math] GHz uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
FREES3000H2SB double 8 Jy Flux density at [math]3000[/math] GHz uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
FREES857 double 8 Jy Flux density at [math]857[/math] GHz; Estimated directly at Planck’s [math]857[/math] GHz map Posterior median value
FREES857L2SB double 8 Jy Flux density at [math]857[/math] GHz uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
FREES857H2SB double 8 Jy Flux density at [math]857[/math] GHz uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
FREES545 double 8 Jy Flux density at [math]545[/math] GHz; Estimated directly at Planck’s [math]545[/math] GHz map Posterior median value
FREES545L2SB double 8 Jy Flux density at [math]545[/math] GHz uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
FREES545H2SB double 8 Jy Flux density at [math]545[/math] GHz uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
FREES353 double 8 Jy Flux density at [math]353[/math] GHz; Estimated directly at Planck’s [math]353[/math] GHz map Posterior median value
FREES353L2SB double 8 Jy Flux density at [math]353[/math] GHz uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
FREES353H2SB double 8 Jy Flux density at [math]353[/math] GHz uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
FREEEXT double 8 Arcmin Source extension before beam convolution This radius is constant across all channels. The extension parameter was obtained with likelihood beam widths (see section A.2.3 of PIP LV); Posterior median value
FREEEXTL2SB double 8 Arcmin Source extension uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
FREEEXTH2SB double 8 Arcmin Source extension uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
FREER double 8 Arcmin Source radius before beam convolution This radius is constant across all channels. The parameter was computed from FREEEXT and gives an indication of whether the source is extended (see section 6.2.2 of PIP LV)
FREEBETA double 8 Unitless Source spectral index; Computed from the flux densities estimated at each channel[15] Posterior median value
FREEBETAL2SB double 8 Unitless Source spectral index uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
FREEBETAH2SB double 8 Unitless Source spectral index uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
FREETEMP double 8 Kelvin Source temperature; Computed from the flux densities estimated at each channel Posterior median value
FREETL2SB double 8 Kelvin Source temperature uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
FREETH2SB double 8 Kelvin Source temperature uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
FREESREF double 8 Jy Flux density at the reference frequency; Estimated from the likelihood Reference frequency is [math]857[/math] GHz; Posterior median value
FREESREFL2SB double 8 Jy Flux density at the reference frequency uncertainty lower boundary Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
FREESREFH2SB double 8 Jy Flux density at the reference frequency uncertainty upper boundary Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
FREEBETAMLIKE double 8 Unitless Source spectral index; Computed from the flux densities estimated at each channel Maximum likelihood estimate
FREETEMPMLIKE double 8 Kelvin Source temperature; Computed from the flux densities estimated at each channel Maximum likelihood estimate
FREESREFMLIKE double 8 Jy Flux density at the reference frequency; Computed from the flux densities estimated at each channel Maximum likelihood estimate
FREESCHI2 double 8 Unitless [math]\chi^2[/math] of the maximum likelihood estimates Reduced [math]\chi^2[/math]
BKGB3000 double 8 Jy/pixel[16] Background brightness at [math]3000[/math] GHz Average over the patch ([math]32\times32[/math] pixels)
BKGB30001S double 8 Jy/pixel Background brightness standard deviation at [math]3000[/math] GHz Standard deviation over the patch ([math]32\times32[/math] pixels)
BKGB857