# Difference between revisions of "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 (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 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

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

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 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
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);
2 – Galactic zone;
3 – filament mask and Galactic zone.

#### S/N threshold map

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
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

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
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

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:

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

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 GHz channels from the Planck 2015 release and the 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.

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: . 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 , otherwise is .
• 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 parameters: Temperature (), Spectral index () and Flux density at a reference channel ().
• 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 pairs {}, 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 ( pixels; ) and its standard deviation were computed for each individual channel. The map offset levels had previously been corrected.
• With the pairs {}, 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 and its NPSNR is higher.

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.

Spectral indices of the MBB model.

Sky distribution of the sources 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 (mJy)
Set location c (mJy)
PCCS2 Planck’s PCCS2 region 57
PCCS2E Planck’s PCCS2E region and 168
820

#### Description of the catalogue columns.

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 () 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 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 percentile ()
BETAH2SB double 8 Unitless Source spectral index uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
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 percentile ()
TH2SB double 8 Kelvin Source temperature uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
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 percentile ()
EXTH2SB double 8 Arcmin Source extension uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
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 GHz; Posterior median value
SREFL2SB double 8 Jy Flux density at the reference frequency uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
SREFH2SB double 8 Jy Flux density at the reference frequency uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
S3000 double 8 Jy Flux density at GHz; MBB predicted at GHz Posterior median value
S3000L2SB double 8 Jy Flux density at GHz uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
S3000H2SB double 8 Jy Flux density at GHz uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
S857 double 8 Jy Flux density at GHz; MBB predicted at GHz Posterior median value
S857L2SB double 8 Jy Flux density at GHz uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
S857H2SB double 8 Jy Flux density at GHz uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
S545 double 8 Jy Flux density at GHz; MBB predicted at GHz Posterior median value
S545L2SB double 8 Jy Flux density at GHz uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
S545H2SB double 8 Jy Flux density at GHz uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
S353 double 8 Jy Flux density at GHz; MBB predicted at GHz Posterior median value
S353L2SB double 8 Jy Flux density at GHz uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
S353H2SB double 8 Jy Flux density at GHz uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
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 GHz; Estimated directly at the IRIS map Posterior median value
FREES3000L2SB double 8 Jy Flux density at GHz uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
FREES3000H2SB double 8 Jy Flux density at GHz uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
FREES857 double 8 Jy Flux density at GHz; Estimated directly at Planck’s GHz map Posterior median value
FREES857L2SB double 8 Jy Flux density at GHz uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
FREES857H2SB double 8 Jy Flux density at GHz uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
FREES545 double 8 Jy Flux density at GHz; Estimated directly at Planck’s GHz map Posterior median value
FREES545L2SB double 8 Jy Flux density at GHz uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
FREES545H2SB double 8 Jy Flux density at GHz uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
FREES353 double 8 Jy Flux density at GHz; Estimated directly at Planck’s GHz map Posterior median value
FREES353L2SB double 8 Jy Flux density at GHz uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
FREES353H2SB double 8 Jy Flux density at GHz uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
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 percentile ()
FREEEXTH2SB double 8 Arcmin Source extension uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
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 percentile ()
FREEBETAH2SB double 8 Unitless Source spectral index uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
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 percentile ()
FREETH2SB double 8 Kelvin Source temperature uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
FREESREF double 8 Jy Flux density at the reference frequency; Estimated from the likelihood Reference frequency is GHz; Posterior median value
FREESREFL2SB double 8 Jy Flux density at the reference frequency uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
FREESREFH2SB double 8 Jy Flux density at the reference frequency uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
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 of the maximum likelihood estimates Reduced
BKGB3000 double 8 Jy/pixel[16] Background brightness at GHz Average over the patch ( pixels)
BKGB30001S double 8 Jy/pixel Background brightness standard deviation at GHz Standard deviation over the patch ( pixels)
BKGB857 double 8 Jy/pixel Background brightness at GHz Average over the patch ( pixels)
BKGB8571S double 8 Jy/pixel Background brightness standard deviation at GHz Standard deviation over the patch ( pixels)
BKGB545 double 8 Jy/pixel Background brightness at GHz Average over the patch ( pixels)
BKGB5451S double 8 Jy/pixel Background brightness standard deviation at GHz Standard deviation over the patch ( pixels)
BKGB353 double 8 Jy/pixel Background brightness at GHz Average over the patch ( pixels)
BKGB3531S double 8 Jy/pixel Background brightness standard deviation at GHz Standard deviation over the patch ( pixels)
BKGBETA double 8 Unitless Background spectral index (MBB); Computed from the background brightness estimated at each channel[17] Posterior median value
BKGBETAL2SB double 8 Unitless Background spectral index uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
BKGBETAH2SB double 8 Unitless Background spectral index uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
BKGTEMP double 8 Kelvin Background temperature (MBB) Posterior median value
BKGTL2SB double 8 Kelvin Background temperature uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
BKGTH2SB double 8 Kelvin Background temperature uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
BKGBREF double 8 Jy/pixel Background brightness at the reference frequency; Estimated from the likelihood Reference frequency is GHz; Posterior median value
BKGBREFL2SB double 8 Jy/pixel Background brightness at the reference frequency uncertainty lower boundary Lower boundary is the marginal posterior percentile ()
BKGBREFH2SB double 8 Jy/pixel Background brightness at the reference frequency uncertainty upper boundary Upper boundary is the marginal posterior percentile ()
BKGBETAMLIKE double 8 Unitless Background spectral index (MBB) Maximum likelihood estimate
BKGTEMPMLIKE double 8 Kelvin Background temperature (MBB) Maximum likelihood estimate
BKGBREFMLIKE double 8 Jy Background brightness at the reference frequency Maximum likelihood estimate
BKGCHI2 double 8 Unitless of the maximum likelihood estimates Reduced
SNRR3000 double 8 Unitless Signal to Noise Ratio Raw (SNRr) at GHz Source average brightness divided the background standard deviation brightness
SNRR30001S double 8 Unitless 1 error bar of the SNRr at GHz Source brightness error bar divided the background standard deviation brightness
SNRR857 double 8 Unitless Signal to Noise Ratio Raw at GHz Source average brightness divided the background standard deviation brightness
SNRR8571S double 8 Unitless 1 error bar of the SNRr at GHz Source brightness error bar divided the background standard deviation brightness
SNRR545 double 8 Unitless Signal to Noise Ratio Raw at GHz Source average brightness divided the background standard deviation brightness
SNRR5451S double 8 Unitless 1 error bar of the SNRr at GHz Source brightness error bar divided the background standard deviation brightness
SNRR353 double 8 Unitless Signal to Noise Ratio Raw at GHz Source average brightness divided the background standard deviation brightness
SNRR3531S double 8 Unitless 1 error bar of the SNRr at GHz Source brightness error bar divided the background standard deviation brightness
SRCINDEX double 8 Unitless Source index
SRCSEP double 8 Arcmin Separation between BeeP’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 radius with higher NPSNR

#### 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 (POSERR) and flux density (SREFH2SB, SREFL2SB) estimates may be over-optimistic for objects with high NPSNR. 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: where POSERR 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.

##### Flux density correction

where is one of the constants in table 1 and can be given either by

for a symmetric error bar, or
and
if the non-symmetrical character of the uncertainty needs to be preserved.

Example of a symmetrical correction: Source PCCS2 857 G002.95+57.96 (NPSNR). where we have used the correction constant for the ‘PCCS2 region’, mJy.
In figures 11 and B.7, we show, in red and blue, the effect of applying the symmetrical correction.

#### Spectral Energy Density (SED) plots

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 and regions, respectively, of the full posterior density. Blue diamonds are the PCCS2+2E flux-density estimates (APERFLUX). The green diamonds are: in the upper panel BeeP’s estimate of the flux density at 857 GHz, and in the middle panel BeeP’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 and regions, respectively, of the full posterior density. Blue diamonds are the PCCS2+2E flux-density estimates (APERFLUX). The green diamonds are: in the upper panel BeeP’s estimate of the flux density at 857 GHz, and in the middle panel BeeP’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.

Another component of the catalogue is a collection of figures, one for each row, that displays the SED curves