Difference between revisions of "Catalogues"

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 zone^a
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 zone^a
PCCS2
Minimum^b	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
Minimum^b	—	—	—	—	—	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 density^a [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 density^a [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

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.
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.
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:
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.
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.
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.
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%.
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

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

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

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

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).
In the extragalactic zone (48% of the sky; see Fig. 2 in Planck-2013-XXVIII^[4]).
In the Galactic zone (52% of the sky; see Fig. 2 in Planck-2013-XXVIII^[4]).
Minimum flux density of the catalogue at |b| > 30º after excluding the 10% faintest sources.
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-DPC – HFI-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

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.
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:
= 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.
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: . 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.

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**
Set	location	c (mJy)
PCCS2	Planck’s PCCS2 region	57
PCCS2E	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**
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	double	8	Jy/pixel	Background brightness at [math]857[/math] GHz	Average over the patch ([math]32\times32[/math] pixels)
BKGB8571S	double	8	Jy/pixel	Background brightness standard deviation at [math]857[/math] GHz	Standard deviation over the patch ([math]32\times32[/math] pixels)
BKGB545	double	8	Jy/pixel	Background brightness at [math]545[/math] GHz	Average over the patch ([math]32\times32[/math] pixels)
BKGB5451S	double	8	Jy/pixel	Background brightness standard deviation at [math]545[/math] GHz	Standard deviation over the patch ([math]32\times32[/math] pixels)
BKGB353	double	8	Jy/pixel	Background brightness at [math]353[/math] GHz	Average over the patch ([math]32\times32[/math] pixels)
BKGB3531S	double	8	Jy/pixel	Background brightness standard deviation at [math]353[/math] GHz	Standard deviation over the patch ([math]32\times32[/math] 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 [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
BKGBETAH2SB	double	8	Unitless	Background spectral index uncertainty upper boundary	Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
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 [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
BKGTH2SB	double	8	Kelvin	Background temperature uncertainty upper boundary	Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
BKGBREF	double	8	Jy/pixel	Background brightness at the reference frequency; Estimated from the likelihood	Reference frequency is [math]857[/math] GHz; Posterior median value
BKGBREFL2SB	double	8	Jy/pixel	Background brightness at the reference frequency uncertainty lower boundary	Lower boundary is the marginal posterior [math]2.275\%[/math] percentile ([math]-2 \sigma[/math])
BKGBREFH2SB	double	8	Jy/pixel	Background brightness at the reference frequency uncertainty upper boundary	Upper boundary is the marginal posterior [math]97.725\%[/math] percentile ([math]+2 \sigma[/math])
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	[math]\chi^2[/math] of the maximum likelihood estimates	Reduced [math]\chi^2[/math]
SNRR3000	double	8	Unitless	Signal to Noise Ratio Raw (SNRr) at [math]3000[/math] GHz	Source average brightness divided the background standard deviation brightness
SNRR30001S	double	8	Unitless	1 [math]\sigma[/math] error bar of the SNRr at [math]3000[/math] GHz	Source brightness error bar divided the background standard deviation brightness
SNRR857	double	8	Unitless	Signal to Noise Ratio Raw at [math]857[/math] GHz	Source average brightness divided the background standard deviation brightness
SNRR8571S	double	8	Unitless	1 [math]\sigma[/math] error bar of the SNRr at [math]857[/math] GHz	Source brightness error bar divided the background standard deviation brightness
SNRR545	double	8	Unitless	Signal to Noise Ratio Raw at [math]545[/math] GHz	Source average brightness divided the background standard deviation brightness
SNRR5451S	double	8	Unitless	1 [math]\sigma[/math] error bar of the SNRr at [math]545[/math] GHz	Source brightness error bar divided the background standard deviation brightness
SNRR353	double	8	Unitless	Signal to Noise Ratio Raw at [math]353[/math] GHz	Source average brightness divided the background standard deviation brightness
SNRR3531S	double	8	Unitless	1 [math]\sigma[/math] error bar of the SNRr at [math]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 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 [math]8'[/math] radius with higher NPSNR

Position and flux density correction[edit]

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[edit]

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[edit]

where [math]c[/math] is one of the constants in table 1 and [math]\sigma_{cat}[/math] 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[math]= 32.43[/math]). where we have used the correction constant for the ‘PCCS2 region’, [math]c= 57[/math] 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[edit]

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 for each of the models. There are three different panels in each figure,

SOURCE: Is the PCCS2+2E name of the source.
BEEPGLON and BEEPGLAT: Are the Galactic longitude and latitude computed by BeeP using the MBB SED model.
SRCSIG, NPSNR and EST_QUALITY are the fields defining the reliability of the source and the estimation quality (see companion paper section 5.4).
Upper panel - MBB SED curves.

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 BeeP’s posterior. In purple, if the sample was inside the [math]68\%[/math] HPD^[18] 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 BeeP’s estimate of the reference flux density (at 857 GHz).

Middle panel - ‘Free’ channel amplitudes.

The green diamonds are BeeP’s posterior medians of the flux densities at each channel^[19]. 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 (APERFLUX).

Lower panel - Background/Foreground contrast parameters.

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 BeeP’s SNRr: Source average brightness divided by the background brightness standard deviation in that patch.

The TEMP and BETA numerical parameter values, shown in all panels, are the marginalised posterior medians.
The [math]\chi^2[/math] values are the reduced [math]\chi^2[/math] of the maximum likelihood solution.

Parameter posterior distributions (‘corner plots’)[edit]

This component of the catalogue is another collection of figures showing the MBB parameter posterior distributions of BeeP’s likelihood in the form of a ‘corner’ plot (see figure 5).

SOURCE: Is the PCCS2+2E name of the source.
GLON and GLAT: Are the Galactic longitude and latitude in the PCCS2+2E catalogue. These are the [math](0,0)[/math] coordinates of the parameters [math]dX[/math] and [math]dY[/math].
SRCSIG, NPSNR and EST_QUALITY are the fields defining the reliability of the source and the estimation quality (see companion paper section 5.4).
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]2.5, 50.0, 97.5[/math]} percentiles.
The violet line is the PCCS2+2E catalogue flux density at the [math]857[/math] GHz channel (APERFLUX).

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 GHz channel. There is one of these plots for each source in BeeP’s catalogue (APERFLUX).

(2015) Planck Catalogue of Galactic Cold Clumps[edit]

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 Planck-2015-A28^[20].

The all-sky distribution of the PGCC sources is plotted below on the 857-GHz emission shown in logarithmic scale between 10^-2 to 10² MJy sr^-1.

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^-2 and 10² MJy sr^-1.

All-sky distribution of the PGCC sources with FLUX_QUALITY=1.

All-sky distribution of the PGCC sources with FLUX_QUALITY=2.

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 Planck-2015-A28^[20]. 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 1σ;
DIST_QUALITY=3, multiple distance estimates which are not consistent within 1σ;
DIST_QUALITY=4, single upper limits.

The all-sky distribution of sources with robust distance estimates is shown below.

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 HFI_PCCS_GCC_R2.02.fits. Its structure is shown in the following table.

**FITS file structure**
Identification
FITS Keyword	Data type	Units	Description
NAME	String		Source Name
SNR	real*8		Maximum S/N over the 857, 545, and 353 GHz Planck cold residual maps
SNR_857	real*8		S/N of the cold residual detection at 857 GHz
SNR_545	real*8		S/N of the cold residual detection at 545 GHz
SNR_353	real*8		S/N of the cold residual detection at 353 GHz
Source position
FITS Keyword	Data type	Units	Description
GLON	real*8	deg	Galactic longitude based on morphology fitting
GLAT	real*8	deg	Galactic latitude based on morphology fitting
RA	real*8	deg	Right ascension (J2000) in degrees transformed from (GLON, GLAT)
DEC	real*8	deg	Declination (J2000) in degrees transformed from (GLON, GLAT)
Morphology
FITS Keyword	Data type	Units	Description
GAU_MAJOR_AXIS	real*8	arcmin	FWHM along the major axis of the elliptical Gaussian
GAU_MAJOR_AXIS_SIG	real*8	arcmin	1σ uncertainty on the FWHM along the major axis
GAU_MINOR_AXIS	real*8	arcmin	FWHM along the minor axis of the elliptical Gaussian
GAU_MINOR_AXIS_SIG	real*8	arcmin	1σ uncertainty on the FWHM along the minor axis
GAU_POSITION_ANGLE	real*8	rad	Position angle of the elliptical Gaussian (see note 1)
GAU_POSITION_ANGLE_SIG	real*8	rad	1σ uncertainty on the position angle
Photometry
FITS Keyword	Data type	Units	Description
FLUX_3000_CLUMP	real*8	Jy	Flux density of the clump at 3 THz
FLUX_3000_CLUMP_SIG	real*8	Jy	1σ uncertainty on the flux density of the clump at 3 THz
FLUX_857_CLUMP	real*8	Jy	Flux density of the clump at 857 GHz
FLUX_857_CLUMP_SIG	real*8	Jy	1σ uncertainty on the flux density of the clump at 857 GHz
FLUX_545_CLUMP	real*8	Jy	Flux density of the clump at 545 GHz
FLUX_545_CLUMP_SIG	real*8	Jy	1σ uncertainty on the flux density of the clump at 545 GHz
FLUX_353_CLUMP	real*8	Jy	Flux density of the clump at 353 GHz
FLUX_353_CLUMP_SIG	real*8	Jy	1σ uncertainty on the flux density of the clump at 353 GHz
FLUX_3000_WBKG	real*8	Jy	Flux density of the warm background at 3 THz (see note 2)
FLUX_3000_WBKG_SIG	real*8	Jy	1σ uncertainty on the flux density of warm background at 3 THz
FLUX_857_WBKG	real*8	Jy	Flux density of the warm background at 857 GHz
FLUX_857_WBKG_SIG	real*8	Jy	1σ uncertainty on the flux density of the warm background at 857 GHz
FLUX_545_WBKG	real*8	Jy	Flux density of the warm background at 545 GHz
FLUX_545_WBKG_SIG	real*8	Jy	1σ uncertainty on the flux density of the warm background at 545 GHz
FLUX_353_WBKG	real*8	Jy	Flux density of the warm background at 353 GHz
FLUX_353_WBKG_SIG	real*8	Jy	1σ uncertainty on the flux density of the warm background at 353 GHz
FLUX_QUALITY	int*4	1-3	Category of flux density reliability (see note 3)
FLUX_BLENDING	int*4	0/1	1 if blending issue with flux density estimate (see note 4)
FLUX_BLENDING_IDX	int*8		Catalogue index of the closest source responsible for blending
FLUX_BLENDING_ANG_DIST	real*8	arcmin	Angular distance to the closest source responsible for blending
FLUX_BLENDING_BIAS_3000	real*8	%	Relative bias of the flux density at 3 THz due to blending
FLUX_BLENDING_BIAS_857	real*8	%	Relative bias of the flux density at 857 GHz due to blending
FLUX_BLENDING_BIAS_545	real*8	%	Relative bias of the flux density at 545 GHz due to blending
FLUX_BLENDING_BIAS_353	real*8	%	Relative bias of the flux density at 353 GHz due to blending
Distance
FITS Keyword	Data type	Units	Description
DIST_KINEMATIC	real*8	kpc	Distance estimate [1] using kinematics
DIST_KINEMATIC_SIG	real*8	kpc	1σ uncertainty on the distance estimate [1] using kinematics
DIST_OPT_EXT_DR7	real*8	kpc	Distance estimate [2] using optical extinction on SDSS DR7
DIST_OPT_EXT_DR7_SIG	real*8	kpc	1σ uncertainty on the distance estimate [2] using optical extinction on SDSS DR7
DIST_OPT_EXT_DR9	real*8	kpc	Distance estimate [3] using optical extinction on SDSS DR9
DIST_OPT_EXT_DR9_SIG	real*8	kpc	1σ uncertainty on the distance estimate [3] using optical extinction on SDSS DR9
DIST_NIR_EXT_IRDC	real*8	kpc	Distance estimate [4] using near-IR extinction towards IRDCs
DIST_NIR_EXT_IRDC_SIG	real*8	kpc	1σ uncertainty on the distance estimate [4] using near-IR extinction towards IRDCs
DIST_NIR_EXT	real*8	kpc	Distance estimate [5] using near-IR extinction
DIST_NIR_EXT_SIG	real*8	kpc	1σ uncertainty on the distance estimate [5] using near-IR extinction
DIST_MOLECULAR_COMPLEX	real*8	kpc	Distance estimate [6] using molecular complex association
DIST_MOLECULAR_COMPLEX_SIG	real*8	kpc	1σ uncertainty on the distance estimate [6] using molecular complex association
DIST_HKP_GCC	real*8	kpc	Distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
DIST_HKP_GCC_SIG	real*8	kpc	1σ uncertainty on the distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
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	1σ uncertainty on the best distance estimate
Temperature
FITS Keyword	Data type	Units	Description
TEMP_CLUMP	real*8	K	Temperature of the clump with β as a free parameter
TEMP_CLUMP_SIG	real*8	K	1σ uncertainty on the clump temperature with β free
TEMP_CLUMP_LOW1	real*8	K	Lower 68% confidence limit of the clump temperature with β free
TEMP_CLUMP_UP1	real*8	K	Upper 68% confidence limit of the clump temperature with β free
BETA_CLUMP	real*8		Spectral index β of the clump
BETA_CLUMP_SIG	real*8		1σ uncertainty (from MCMC) on the emissivity spectral index β of the clump
BETA_CLUMP_LOW1	real*8		Lower 68% confidence limit of the emissivity spectral index β of the clump
BETA_CLUMP_UP1	real*8		Upper 68% confidence limit of the emissivity spectral index β of the clump
TEMP_BETA2_CLUMP	real*8	K	Temperature of the clump with β = 2
TEMP_BETA2_CLUMP_SIG	real*8	K	1σ uncertainty on the temperature of the clump with β = 2
TEMP_BETA2_CLUMP_LOW1	real*8	K	Lower 68% confidence limit of the clump temperature with β = 2
TEMP_BETA2_CLUMP_UP1	real*8	K	Upper 68% confidence limit of the clump temperature with β = 2
TEMP_WBKG	real*8	K	Temperature of the warm background with β as a free parameter (see note 6)
TEMP_WBKG_SIG	real*8	K	1σ dispersion of the warm background temperature with β free
TEMP_WBKG_LOW1	real*8	K	Lower 68% confidence limit of the warm background temperature with β free
TEMP_WBKG_UP1	real*8	K	Upper 68% confidence limit of the warm background temperature with β free
BETA_WBKG	real*8		Spectral index β of the warm background (see note 6)
BETA_WBKG_SIG	real*8		1σ uncertainty (from MCMC) of the emissivity spectral index β of the warm background
BETA_WBKG_LOW1	real*8		Lower 68% confidence limit of the emissivity spectral index β of the warm background
BETA_WBKG_UP1	real*8		Upper 68% confidence limit of the emissivity spectral index β of the warm background
TEMP_BETA2_WBKG	real*8	K	Temperature of the warm background with β = 2
TEMP_BETA2_WBKG_SIG	real*8	K	1σ uncertainty on the temperature of the warm background with β = 2
TEMP_BETA2_WBKG_LOW1	real*8	K	Lower 68% confidence limit of the warm background temperature with β = 2
TEMP_BETA2_WBKG_UP1	real*8	K	Upper 68% confidence limit of the warm background temperature with β = 2
Physical properties
FITS Keyword	Data type	Units	Description
NH2	real*8	cm^-2	Column density N_H₂ of the clump
NH2_SIG	real*8	cm^-2	1σ uncertainty on the column density
NH2_LOW[1,2,3]	real*8	cm^-2	Lower 68%, 95%, and 99% confidence limit of the column density
NH2_UP[1,2,3]	real*8	cm^-2	Upper 68%, 95%, and 99% confidence limit of the column density
MASS	real*8	M_☉	Mass estimate of the clump
MASS_SIG	real*8	M_☉	1σ uncertainty on the mass estimate of the clump
MASS_LOW[1,2,3]	real*8	M_☉	Lower 68%, 95%, and 99% confidence limit of the mass estimate
MASS_UP[1,2,3]	real*8	M_☉	Upper 68%, 95%, and 99% confidence limit of the mass estimate
DENSITY	real*8	cm^-3	Mean density of the clump
DENSITY_SIG	real*8	cm^-3	1σ uncertainty on the mean density estimate of the clump
DENSITY_LOW[1,2,3]	real*8	cm^-3	Lower 68%, 95%, and 99% confidence limit of the mean density estimate
DENSITY_UP[1,2,3]	real*8	cm^-3	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	1σ 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_☉	Luminosity of the clump
LUMINOSITY_SIG	real*8	L_☉	1σ uncertainty on the luminosity estimate of the clump
LUMINOSITY_LOW[1,2,3]	real*8	L_☉	Lower 68%, 95%, and 99% confidence limit of the luminosity estimate
LUMINOSITY_UP[1,2,3]	real*8	L_☉	Upper 68%, 95%, and 99% confidence limit of the luminosity estimate
Flags
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

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[edit]

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 Planck-2015-XXXIX^[21]. 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 Planck-2014-XXVIII^[22].

The all-sky distribution of the PHZ sources is shown below on an orthographic projection.

All-sky distribution of the 2151 PHZ sources in orthographic projection.

The PHz source list is contained in the FITS file HFI_PCCS_HZ_R2.00.fits. Its structure is as follows.

**FITS file structure**
Identification
FITS Keyword	Data type	Units	Description
NAME	String		Source name
SNR_X545	real*8		S/N in the 545 GHz excess map
SNR_D857	real*8		S/N in the 857 GHz cleaned map
SNR_D545	real*8		S/N in the 545 GHz cleaned map
SNR_D353	real*8		S/N in the 353 GHz cleaned map
Source position
FITS Keyword	Data type	Units	Description
GLON	real*8	deg	Galactic longitude based on morphology fitting
GLAT	real*8	deg	Galactic latitude based on morphology fitting
RA	real*8	deg	Right ascension (J2000) in degrees transformed from (GLON, GLAT)
DEC	real*8	deg	Declination (J2000) in degrees transformed from (GLON, GLAT)
Morphology
FITS Keyword	Data type	Units	Description
GAU_MAJOR_AXIS	real*8	arcmin	FWHM along the major axis of the elliptical Gaussian
GAU_MAJOR_AXIS_SIG	real*8	arcmin	1σ uncertainty on the FWHM along the major axis
GAU_MINOR_AXIS	real*8	arcmin	FWHM along the minor axis of the elliptical Gaussian
GAU_MINOR_AXIS_SIG	real*8	arcmin	1σ uncertainty on the FWHM along the minor axis
GAU_POSITION_ANGLE	real*8	rad	Position angle of the elliptical Gaussian (see note 1)
GAU_POSITION_ANGLE_SIG	real*8	rad	1σ uncertainty on the position angle
Photometry
FITS Keyword	Data type	Units	Description
FLUX_CLEAN_857	real*8	Jy	Flux density of the clump at 857 GHz
FLUX_CLEAN_857_SIG_SKY	real*8	Jy	1σ uncertainty at 857 GHz due to sky confusion
FLUX_CLEAN_857_SIG_DATA	real*8	Jy	1σ uncertainty at 857 GHz due to measurement error
FLUX_CLEAN_857_SIG_GEOM	real*8	Jy	1σ 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	1σ uncertainty at 545 GHz due to sky confusion
FLUX_CLEAN_545_SIG_DATA	real*8	Jy	1σ uncertainty at 545 GHz due to measurement error
FLUX_CLEAN_545_SIG_GEOM	real*8	Jy	1σ 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	1σ uncertainty at 353 GHz due to sky confusion
FLUX_CLEAN_353_SIG_DATA	real*8	Jy	1σ uncertainty at 353 GHz due to measurement error
FLUX_CLEAN_353_SIG_GEOM	real*8	Jy	1σ 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	1σ uncertainty at 217 GHz due to sky confusion
FLUX_CLEAN_217_SIG_DATA	real*8	Jy	1σ uncertainty at 217 GHz due to measurement error
FLUX_CLEAN_217_SIG_GEOM	real*8	Jy	1σ uncertainty at 217 GHz due to elliptical Gaussian fit accuracy
Physical Properties
FITS Keyword	Data type	Units	Description
PROB_COLCOL	real*8		Colour-colour selection probability
EBV_MEAN	real*8		Mean extinction E(B − V)_xgal within the source PSF
EBV_APER	real*8		Aperture estimate of the extinction E(B − V)_xgal within the source PSF
EBV_APER_SIG	real*8		1σ uncertainty of the aperture extinction E(B − V)_xgal within the source PSF
ZPHOT_[25,30,35,40,45,50]K	real*8		Submm photometric redshift estimate with T_xgal = 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 χ² of the best fit
LFIR_[25,30,35,40,45,50]K	real*8	L_☉	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	L_☉	Lower limit of the 68 % confidence level
LFIR_[25,30,35,40,45,50]K_UP	real*8	L_☉	Upper limit of the 68 % confidence level
SFR_[25,30,35,40,45,50]K	real*8	M_☉yr^-1	Star Formation Rate estimate with T_{xgal = 25, 30, 35, 40, 45, and 50 K}
SFR_[25,30,35,40,45,50]K_LOW	real*8	M_☉yr^-1	Lower limit of the 68 % confidence level
SFR_[25,30,35,40,45,50]K_UP	real*8	M_☉yr^-1	Upper limit of the 68 % confidence level
Flags
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

(2015) Second SZ Catalogue[edit]

The Planck SZ catalogue is constructed as described in SZ catalogue and in sections 2 and 3 of Planck-2015-A27^[23]. 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 Planck-2015-A27^[23].

The size of a detected object is given in terms of the scale size, θ_s, and the flux is given in terms of the total integrated Comptonization parameter, Y = Y_5R500. 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 Y to Y₅₀₀ is also provided in the header.

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.

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 θ_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. 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, M_SZ, as calculated using a Y-M scaling relation and an assumed redshift, in order to break the Y-θ_s 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.

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 θ₅₀₀ and Y₅₀₀. 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.

Union catalogue[edit]

The union catalogue is contained in HFI_PCCS_SZ-union_R2.08.fits.

Extension 0: primary header, no data
FITS keyword	Data type	Units	Description
INSTRUME	String		Instrument (HFI)
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 α parameter
PP_BETA	Real*4		GNFW pressure profile β parameter
PP_GAMMA	Real*4		GNFW pressure profile γ parameter
PP_C500	Real*4		GNFW pressure profile c₅₀₀ parameter
PP_Y2YFH	Real*4		Conversion factor from Y to Y₅₀₀
Extension 1: BINTABLE, EXTNAME = PSZ2_UNION
Column Name	Data type	Units	Description
INDEX	Int*4		Index used to cross-reference with individual catalogues
NAME	String		Source name (see note 1)
GLON	Real*8	deg	Galactic longitude
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 the detection
PIPELINE	Int*4		Pipeline from which information is taken (reference pipeline): 1= MMF1; 2 = MMF3; 3 = PwS
PIPE_DET	Int*4		Pipelines that detect this object (see note 2)
PCCS2	Bool		Indicates whether detection matches with any in PCCS2 catalogues
PSZ	Int*4		Index of matching detection in PSZ1, or -1 if new detection
IR_FLAG	Int*1		Flag denoting heavy IR contamination
Q_NEURAL	Real*4		Neural network quality flag (see note 3)
Y5R500	Real*4	10^-3 arcmin²	Mean marginal Y_5R500 as determined by reference pipeline
Y5R500_ERR	Real*4	10^-3 arcmin²	Uncertainty on Y_5R500 as determined by reference pipeline
VALIDATION	Int*4		External validation status (see note 4)
REDSHIFT_ID	String		External identifier of cluster associated with redshift measurement (see note 5)
REDSHIFT	Real*4		Redshift of cluster (see note 5)
MSZ	Real*4	10¹⁴ M_☉	SZ mass proxy (see note 6)
MSZ_ERR_UP	Real*4	10¹⁴ M_☉	Upper bound of 68% SZ mass proxy confidence interval (see note 6)
MSZ_ERR_LOW	Real*4	10¹⁴ M_☉	Lower bound of 68% SZ mass proxy confidence interval (see note 6)
MCXC	String		Identifier of X-ray counterpart in the MCXC, if one is present
REDMAPPER	String		Identifier of optical counterpart in the RedMAPPer catalogue, if one is present
ACT	String		Identifier of SZ counterpart in the ACT catalogues, if one is present
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 PSZ2 Glll.ll±bb.b where l and b 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-Q_bad, 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.
M_SZ 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); and -10 = not analysed.
Defined in the paper.

Individual catalogues[edit]

The individual pipeline catalogues are contained in the FITS files

HFI_PCCS_SZ-MMF1_R2.08.fits (MMF1 pipeline)
HFI_PCCS_SZ-MMF3_R2.08.fits (MMF3 pipeline)
HFI_PCCS_SZ-PwS_R2.08.fits (PowellSnakes pipeline).

Their structure is shown in the following table.

**FITS file structure**
Extension 0: Primary header, no data
FITS keyword	Data type	Units	Description
INSTRUME	String		Instrument (HFI)
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 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 α parameter
PP_BETA	Real*4		GNFW pressure profile β parameter
PP_GAMMA	Real*4		GNFW pressure profile γ parameter
PP_C500	Real*4		GNFW pressure profile c₅₀₀ parameter
PP_Y2YFH	Real*4		Conversion factor from Y to Y₅₀₀
Extension 1: BINTABLE, EXTNAME = PSZ2_INDIVIDUAL
Column name	Data type	Units	Description
INDEX	Int*4		Index from union catalogue
NAME	String		Source name (see note 1)
GLON	Real*8	deg	Galactic longitude
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 θ_s in grid in second extension HDU (see note 2)
TS_MAX	Real*4		Maximum value of θ_s in grid in second extension HDU (see note 2)
Y_MIN	Real*4		Minimum value of Y in grid in second extension HDU (see note 2)
Y_MAX	Real*4		Maximum value of Y in grid in second extension HDU (see note 2)
Keyword	Data type	Value	Description
PIPELINE	String		Name of detection pipeline
Extension 2: IMAGE, EXTNAME = PSZ2_PROBABILITY (see note 2)
Keyword	Data type	Value	Description
NAXIS1	Integer	256	Dimension 1
NAXIS2	Integer	256	Dimension 2
NAXIS3	Integer	N_det	Dimension 3 = Number of detections
Keyword	Data type	Value	Description
PIPELINE	String		Name of detection pipeline
Extension 3: IMAGE, EXTNAME = PSZ2_MSZ_ARRAY (see note 3)
Keyword	Data type	Value	Description
NAXIS1	Integer	100	Dimension 1
NAXIS2	Integer	4	Dimension 2
NAXIS3	Integer	N_det	Dimension 3 = Number of detections
Keyword	Data type	Value	Description
PIPELINE	String		Name of detection pipeline

Notes

Format PSZ2 Glll.ll±bb.bb where l and b are the Galactic coordinates truncated to two decimal places.
Extension 2 contains a three-dimensional image with the two-dimensional probability distribution in θ_s and Y for each detection. The probability distributions are evaluated on a 256 × 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 × 256 × N_det, where N_det is the number of detections. The first dimension is θ_s and the second dimension is Y.
Extension 3 contains a three-dimensional image with the information on the M_SZ observable per cluster as a function of assumed redshift. The image dimensions are 100 × 4 × N_det, where N_det 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_SZ values; the second element is the M_SZ lower 68% confidence bound; the third element is the M_SZ estimate; and the fourth element is the M_SZ upper 68% confidence bound, all in units of 10¹⁴ M_☉. 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[edit]

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.

**FITS file structure**
Extension 0: Primary header, no data
FITS keyword	Data type	Units	Description
INSTRUME	String		Instrument (HFI)
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 time of the survey: yyyy-mm-dd
DATE-END	String		End time of the survey: yyyy-mm-dd
PROCVER	String		Data version
JOIN	String		Join type (UNION, INTERSEC, MMF1, MMF3, PwS)
MASK	String		Mask name (SURVEY, COSMOLOG)
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
Extension 2: IMAGE, EXTNAME = SELFUNC (see note 2)
Keyword	Data type	Value	Description
NAXIS1	Integer	30	Dimension 1
NAXIS2	Integer	32	Dimension 2
NAXIS3	Integer	12	Dimension 3
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)
Extension 3: IMAGE, EXTNAME = YGRID (see note 3)
Keyword	Data type	Value	Description
NAXIS1	Integer	30	Dimension 1
Keyword	Data type	Value	Description
COL1	String	CY500	Grid values of Y₅₀₀
Extension 4: IMAGE, EXTNAME = TGRID (see note 4)
Keyword	Data type	Value	Description
NAXIS1	Integer	32	Dimension 1
Keyword	Data type	Value	Description
COL1	String	T500	Grid values of θ₅₀₀
Extension 5: IMAGE, EXTNAME = SNR_THRESH (see note 5)
Keyword	Data type	Value	Description
NAXIS1	Integer	12	Dimension 1
Keyword	Data type	Value	Description
COL1	String	S/N	Grid values of S/N threshold

Notes

Extension 1 contains a mask defining the survey region, given by an N_side = 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.
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 × 32 × 12. The first dimension is Y₅₀₀, the second dimension is θ₅₀₀ 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 (Y₅₀₀, θ₅₀₀) bin.
Extension 3 contains the Y₅₀₀ grid values for the completeness data cube in the second extension. It has length 30 and spans the range from 1.12480 × 10^-4 arcmin² to 7.20325 × 10^-2 arcmin² in logarithmic steps.
Extension 4 contains the θ₅₀₀ 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.

Previous releases: (2013) PSZ1[edit]

Second Planck Release (2013): Description of the Planck SZ Catalogue

The Planck SZ catalogue is constructed as described in SZ catalogue and in section 2 of Planck-2013-XXIX^[24].

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 Planck-2013-XXIX^[24].

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, θ_s, and the flux is given in terms of the total integrated Comptonization parameter, Y = Y_5r₅₀₀. 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 Y₅₀₀ is also written in the header.

The full information on the degeneracy between θ_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.

Union Catalogue

The union catalogue is contained in COM_PCCS_SZ-union_R1.12.fits.

Extension 0: Primary header, no data
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 α parameter.
PP_BETA	Real*4		GNFW pressure profile β parameter.
PP_GAMMA	Real*4		GNFW pressure profile γ parameter.
PP_C500	Real*4		GNFW pressure profile c₅₀₀ parameter.
PP_Y2YFH	Real*4		Conversion factor from Y to Y₅₀₀.
Extension 1: data extension (BINTABLE)
Column Name	Data type	Units	Description
INDEX	Int*4		Index. Used to cross-reference with individual catalogues.
NAME	String		Source name (note 1).
GLON	Real*8	degrees	Galactic longitude.
GLAT	Real*8	degrees	Galactic latitude.
RA	Real*8	degrees	Right ascension (J2000) transformed from (GLON,GLAT).
DEC	Real*8	degrees	Declination (J2000) transformed from (GLON,GLAT).
POS_ERR	Real*4	arcmin	Position uncertainty (approximate 68% confidence interval). See 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.
COMMENT	Bool		Detection has a comment in the associated text file (note 4).

Notes

format is PSZ1 Glll.ll+mn;bb.b where l nd b are the Galactic and truncated to 2 decimal places.
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.
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 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.

Individual Catalogues

The individual pipeline catalogues are contained in the FITS files

COM_PCCS_SZ-MMF1_R1.11.fits (Matched Multi-Filter method #1)
COM_PCCS_SZ-MMF3_R1.12.fits (Matched Multi-Filter method #3)
COM_PCCS_SZ-PwS_R1.11.fits (Powell Snakes method)

Their structure is as follows:

**FITS file structure**
Ext. 0: Primary header, no data
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 α parameter.
PP_BETA	Real*4		GNFW pressure profile β parameter.
PP_GAMMA	Real*4		GNFW pressure profile γ parameter.
PP_C500	Real*4		GNFW pressure profile c₅₀₀ parameter.
PP_Y2YFH	Real*4		Conversion factor from Y to Y₅₀₀.
Ext. 1: EXTNANE = PSZ_INDIVIDUAL (BINTABLE)
Column Name	Data type	Units	Description
INDEX	Int*4		Index from union catalogue.
NAME	String		Source name - see note 1.
GLON	Real*8	deg	Galactic longitude.
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 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 θ_{s</i in grid in second extension HDU (see below).}
TS_MAX	Real*4		Maximum value of θ_{s in grid in second extension HDU (see below).}
Y_MIN	Real*4		Minimum value of Y in grid in second extension HDU (see below).
Y_MAX	Real*4		Maximum value of Y in grid in second extension HDU (see below).
Keyword	Data type	Value	Description
PIPELINE	String		Name of detection pipeline.
Ext. 2: EXTNAME = PSZ_PROBABILITY (IMAGE) - note 3
Keyword	Data type	Value	Description
NAXIS1	Integer	256	Dim 1
NAXIS2	Integer	256	Dim 2
NAXIS3	Integer	Nsources	Dim 3 = Number of sources
Keyword	Data type	Value	Description
PIPELINE	String		Name of detection pipeline.

Notes

Format PSZ1 Glll.ll±bb.bb where l and b are the Galactic coordinates truncated to two decimal places.
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 θ_s and Y for each detection. The probability distributions are evaluated on a 256 × 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 × 256 × n, where n is the number of detections. The first dimension is θ_s and the second dimension is Y.

Mask

The mask used to construct the catalogue is contained in a file: COM_PCCS_SZ-unionMask_2048_R1.11.fits.

It is in GALACTIC coordinates, NESTED ordering, NSIDE=2048.

Additional information

A set of comments on the union catalogue is available in

COM_DocPCCS_SZ-union-comments_R1.11.txt

Additional information on the SZ detections was retrieved from external sources and written into the FITS file

COM_PCCS_SZ-validation_R1.12.fits

(for more details see Planck-2013-XXIX^[24]). This file contains a single BINTABLE extension. The table contains 1 line per source, and the columns and their meaning are given below.

**FITS file structure**
Ext. 0: (BINTABLE)
Column Name	Data type	Units	Description
INDEX	Int*4		Index from union catalogue.
NAME	String		Source name in union catalogue
REDSHIFT	Real*4		Redshift
REDSHIFT_SOURCE	Int*4		Source for redshift - see note 4.
ALT_NAME	String		Alternative names.
RA_MCXC	Real*4	degrees	Right Ascension of the MCXC identifier.
DEC_MCXC	Real*4	degrees	Declination of the MCXC identifier.
YZ_500	Real*4	10^-4 arcmin²	Compton parameter in R500 from SZ-proxy.
ERRP_YZ_500	Real*4	10^-4 arcmin²	Error sup. in YZ_500
ERRM_YZ_500	Real*4	10^-4 arcmin²	Error inf. in YZ_500
M_YZ_500	Real*4	10¹⁴ Msol	Derived mass estimate (M_YZ_500) from SZ proxy.
ERRP_M_YZ_500	Real*4	10¹⁴ Msol	Error sup. on M_YZ_500.
ERRM_M_YZ_500	Real*4	10¹⁴ Msol	Error sup. on M_YZ_500.
S_X	Real*4	erg/s/cm²	Unabsorbed X-ray flux - see note 1.
ERR_S_X	Real*4	erg/s/cm²	Error on unabsorbed X-ray flux.
Y_PSX_500	Real*4	10^-4 arcmin²	SZ signal for PSZ clusters identified with MCXC clusters- see note 2.
SN_PSX	Real*4		Signal to noise for PSZ clusters identified with MCXC clusters - see note 3.

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} \lt 1\sigma[/math], we only quote an upper limit.
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.
Source for redshifts:

    -1 : No redshift available;
     1 : MCXC updated compilation^[25];
     2 : Databases NED and SIMBAD-CDS;
     3 : SDSS cluster catalogue^[26];
     4 : SDSS cluster catalogue^[27];
     5 : SPT^[28]^[29]^[30]^[31]^[32]^[33]^[34];
     6 : ACT^[35]^[36]^[37]^[38];
     7 : Search in SDSS galaxy catalogue from Planck Collab.;
    20 : XMM-Newton confirmation from Planck Collab.;
    50 : ENO-imaging confirmation from Planck Collab.;
    60 : WFI-imaging confirmation from Planck Collab.;
    65 : NTT-spectroscopic confirmation from Planck Collab.;
   500 : RTT-spectroscopic confirmation from Planck Collab.;
   600 : NOT-spectroscopic confirmation from Planck Collab.;
   650 : GEMINI-spectroscopic confirmation from Planck Collab.;
   700 : ENO-spectroscopic confirmation from Planck Collab.

Caveats

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)

The approximate 68% (1-sigma) confidence interval in the POS_ERR field is computed as half of the 95% (2σ) confidence interval. Previously this was erroneously described as a 95% confidence interval.

References[edit]

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↑ A Gaussian likelihood was created using the [math]4[/math] flux densities and error bars measured at each channel.
↑ Pixel [math]\approx 2.95[/math] arcmin[math]^2[/math]
↑ A Gaussian likelihood was created using the [math]4[/math] background brightness and error bars measured at each channel.
↑ Highest Probability Density region (HPD). For a complete definition see .
↑ Sources inside the IRIS mask do not include a flux density at 3000 GHz.
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[planck2014-a35-1] 1.0^1.1 Planck 2015 results. XXVI. The second Planck catalogue of compact sources, Planck Collaboration, 2016, A&A, 594, A26.

[planck2013-p02d-2] Planck 2013 results. IV. Low Frequency Instrument beams and window functions, Planck Collaboration, 2014, A&A, 571, A4.

[planck2013-p03c-3] Planck 2013 results. VII. HFI time response and beams, Planck Collaboration, 2014, A&A, 571, A7.

[planck2013-p05-4] 4.0^4.1^4.2 Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources, Planck Collaboration, 2014, A&A, 571, A28.

[.5B.5B:Template:PATCABright.5D.5D-5] The Planck-ATCA Co-eval Observations project: the brightsample, M. Massardi, A. Bonaldi, L. Bonavera, M. López-Caniego, G. de Zotti, R. D. Ekers, MNRAS, 415, 1597-1610, (2011).

[.5B.5B:Template:PATCAfaint.5D.5D-6] The Planck-ATCA Coeval Observations project: the faintsample, L. Bonavera, M. Massardi, A. Bonaldi, J. González-Nuevo, G. de Zotti, R. D. Ekers, MNRAS, 416, 559-566, (2011).

[.5B.5B:Template:PATCASpec.5D.5D-7] The Planck-ATCA Co-eval Observations project: the spectrallyselected sample, A. Bonaldi, L. Bonavera, M. Massardi, G. De Zotti, MNRAS, 428, 1845-1854, (2013).

[planck2013-p02-8] Planck 2013 results. II. Low Frequency Instrument data processing, Planck Collaboration, 2014, A&A, 571, A2.

[planck2013-p03-9] Planck 2013 results. VI. High Frequency Instrument Data Processing, Planck Collaboration, 2014, A&A, 571, A6.

[.5B.5B:Template:Johnson2013.5D.5D-10] Classification of Compact Submillimeter Sources in the Planck Archive, C. H. Johnson, C. Border, K. O'Connor, D. Rothrock, R. Chary, M. Bingham, M. Clark, M. Ernst, S. Gilbert, S. Koop, M. Maddaus, I. Miller, A. O'Bryan, T. Ravelomanantsoa, D. San Miguel, L. Schmidt, E. Searls, W. Tong, O. Torres, A. Zeidner, NITARP, in American Astronomical Society Meeting Abstracts American Astronomical Society Meeting Abstracts, 221, 352.18, (2013).

[planck2011-1-10-11] 11.0^11.1^11.2 Planck early results. VII. The Early Release Compact Source Catalogue, Planck Collaboration VII, A&A, 536, A7, (2011).

[planck2011-5-1a-12] Planck early results. VIII. The all-sky early Sunyaev-Zeldovich cluster sample, Planck Collaboration VIII, A&A, 536, A8, (2011).

[planck2011-7-7b-13] Planck early results. XXIII. The Galactic cold core population revealed by the first all-sky survey, Planck Collaboration XXIII, A&A, 536, A23, (2011).

[planck2020-LV-14] Planck intermediate results. LV. Reliability and thermal properties of high-frequency sources in the Second Planck Catalogue of Compact Sources, Planck Collaboration Int. LV, Accepted by A&A, 2020.

[15] A Gaussian likelihood was created using the [math]4[/math] flux densities and error bars measured at each channel.

[16] Pixel [math]\approx 2.95[/math] arcmin[math]^2[/math]

[17] A Gaussian likelihood was created using the [math]4[/math] background brightness and error bars measured at each channel.

[18] Highest Probability Density region (HPD). For a complete definition see .

[19] Sources inside the IRIS mask do not include a flux density at 3000 GHz.

[planck2014-a37-20] 20.0^20.1 Planck 2015 results. XXVIII. The Planck catalogue of Galactic cold clumps, Planck Collaboration, 2016, A&A, 594, A28.

[planck2015-XXXIX-21] Planck intermediate results. XXXIX. The Planck list of high-redshift source candidates, Planck Collaboration Int. XXXIX A&A, 596, A100, (2016).

[planck2014-XXVIII-22] Planck intermediate results. XXVIII. Interstellar gas and dustin the Chamaeleon clouds as seen by Fermi LAT and Planck, Planck Collaboration Int. XXVIII, A&A, 582, A30, (2015).

[planck2014-a36-23] 23.0^23.1 Planck 2015 results. XXVII. The second Planck catalogue of Sunyaev-Zeldovich sources, Planck Collaboration, 2016, A&A, 594, A27.

[planck2013-p05a-24] 24.0^24.1^24.2 Planck 2013 results. XXIX. The Planck Catalogue of Sunyaev-Zeldovich sources, Planck Collaboration, 2014, A&A, 571, A29.

[.5B.5B:Template:Piffaretti2011.5D.5D-25] The MCXC: a meta-catalogue of x-ray detected clusters of galaxies, R. Piffaretti, M. Arnaud, G. W. Pratt, E. Pointecouteau, J.-B. Melin, A&A, 534, A109, (2011).

[.5B.5B:Template:Wen2012.5D.5D-26] A Catalog of 132,684 Clusters of Galaxies Identified from Sloan Digital Sky Survey III, Z. L. Wen, J. L. Han, F. S. Liu, ApJS, 199, 34, (2012).

[.5B.5B:Template:Szabo2011.5D.5D-27] An Optical Catalog of Galaxy Clusters Obtained from an Adaptive Matched Filter Finder Applied to Sloan Digital Sky Survey Data Release 6, T. Szabo, E. Pierpaoli, F. Dong, A. Pipino, J. Gunn, ApJ, 736, 21, (2011).

[.5B.5B:Template:Vanderlinde2010.5D.5D-28] Galaxy Clusters Selected with the Sunyaev-Zel'dovich Effect from 2008 South Pole Telescope Observations, K. Vanderlinde, T. M. Crawford, T. de Haan, J. P. Dudley, L. Shaw, P. A. R. Ade, K. A. Aird, B. A. Benson, L. E. Bleem, M. Brodwin, J. E. Carlstrom, C. L. Chang, A. T. Crites, S. Desai, M. A. Dobbs, R. J. Foley, E. M. George, M. D. Gladders, N. R. Hall, N. W. Halverson, F. W. High, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, M. Joy, R. Keisler, L. Knox, A. T. Lee, E. M. Leitch, A. Loehr, M. Lueker, D. P. Marrone, J. J. McMahon, J. Mehl, S. S. Meyer, J.J. Mohr, T. E. Montroy, C.-C. Ngeow, S. Padin, T. Plagge, C. Pryke, C. L. Reichardt, A. Rest, J. Ruel, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, J. Song, H. G. Spieler, B. Stalder, Z. Staniszewski, A. A. Stark, C. W. Stubbs, A. van Engelen, J. D. Vieira, R. Williamson, Y. Yang, O. Zahn, A. Zenteno, ApJ, 722, 1180-1196, (2010).

[.5B.5B:Template:Williamson2011.5D.5D-29] A Sunyaev-Zel'dovich-selected Sample of the Most Massive Galaxy Clusters in the 2500 deg$^{2}$ South Pole Telescope Survey, R. Williamson, B. A. Benson, F. W. High, K. Vanderlinde, P. A. R. Ade, K. A. Aird, K. Andersson, R. Armstrong, M. L. N. Ashby, M. Bautz, G. Bazin, E. Bertin, L. E. Bleem, M. Bonamente, M. Brodwin, J. E. Carlstrom, C. L. Chang, S. C. Chapman, A. Clocchiatti, T. M. Crawford, A. T. Crites, T. de Haan, S. Desai, M. A. Dobbs, J. P. Dudley, G. G. Fazio, R. J. Foley, W. R. Forman, G. Garmire, E. M. George, M. D. Gladders, A. H. Gonzalez, N. W. Halverson, G. P. Holder, W. L. Holzapfel, S. Hoover, J. D. Hrubes, C. Jones, M. Joy, R. Keisler, L. Knox, A. T. Lee, E. M. Leitch, M. Lueker, D. Luong-Van, D. P. Marrone, J. J. McMahon, J. Mehl, S. S. Meyer, J. J. Mohr, T. E. Montroy, S. S. Murray, S. Padin, T. Plagge, C. Pryke, C. L. Reichardt, A. Rest, J. Ruel, J. E. Ruhl, B. R. Saliwanchik, A. Saro, K. K. Schaffer, L. Shaw, E. Shirokoff, J. Song, H. G. Spieler, B. Stalder, S. A. Stanford, Z. Staniszewski, A. A. Stark, K. Story, C. W. Stubbs, J. D. Vieira, A. Vikhlinin, A. Zenteno, ApJ, 738, 139, (2011).

[.5B.5B:Template:Andersson2011.5D.5D-30] X-Ray Properties of the First Sunyaev-Zel'dovich Effect Selected Galaxy Cluster Sample from the South Pole Telescope, K. Andersson, B. A. Benson, P. A. R. Ade, K. A. Aird, B. Armstrong, M. Bautz, L. E. Bleem, M. Brodwin, J. E. Carlstrom, C. L. Chang, T. M. Crawford, A. T. Crites, T. de Haan, S. Desai, M. A. Dobbs, J. P. Dudley, R. J. Foley, W. R. Forman, G. Garmire, E. M. George, M. D. Gladders, N. W. Halverson, F. W. High, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, C. Jones, M. Joy, R. Keisler, L. Knox, A. T. Lee, E. M. Leitch, M. Lueker, D. P. Marrone, J. J. McMahon, J. Mehl, S. S. Meyer, J. J. Mohr, T. E. Montroy, S. S. Murray, S. Padin, T. Plagge, C. Pryke, C. L. Reichardt, A. Rest, J. Ruel, J. E. Ruhl, K. K. Schaffer, L. Shaw, E. Shirokoff, J. Song, H. G. Spieler, B. Stalder, Z. Staniszewski, A. A. Stark, C. W. Stubbs, K. Vanderlinde, J. D. Vieira, A. Vikhlinin, R. Williamson, Y. Yang, O. Zahn, A. Zenteno, ApJ, 738, 48, (2011).

[.5B.5B:Template:Plagge2010.5D.5D-31] Sunyaev-Zel'dovich Cluster Profiles Measured with the South Pole Telescope, T. Plagge, B. A. Benson, P. A. R. Ade, K. A. Aird, L. E. Bleem, J. E. Carlstrom, C. L. Chang, H.-M. Cho, T. M. Crawford, A. T. Crites, T. de Haan, M. A. Dobbs, E. M. George, N. R. Hall, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, M. Joy, R. Keisler, L. Knox, A. T. Lee, E. M. Leitch, M. Lueker, D. Marrone, J. J. McMahon, J. Mehl, S. S. Meyer, J. J. Mohr, T. E. Montroy, S. Padin, C. Pryke, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, L. Shaw, E. Shirokoff, H. G. Spieler, B. Stalder, Z. Staniszewski, A. A. Stark, K. Vanderlinde, J. D. Vieira, R. Williamson, O. Zahn, ApJ, 716, 1118-1135, (2010).

[.5B.5B:Template:Reichardt2013.5D.5D-32] Galaxy Clusters Discovered via the Sunyaev-Zel'dovich Effect in the First 720 Square Degrees of the South Pole Telescope Survey, C. L. Reichardt, B. Stalder, L. E. Bleem, T. E. Montroy, K. A. Aird, K. Andersson, R. Armstrong, M. L. N. Ashby, M. Bautz, M. Bayliss, G. Bazin, B. A. Benson, M. Brodwin, J. E. Carlstrom, C. L. Chang, H. M. Cho, A. Clocchiatti, T. M. Crawford, A. T. Crites, T. de Haan, S. Desai, M. A. Dobbs, J. P. Dudley, R. J. Foley, W. R. Forman, E. M. George, M. D. Gladders, A. H. Gonzalez, N. W. Halverson, N. L. Harrington, F. W. High, G. P. Holder, W. L. Holzapfel, S. Hoover, J. D. Hrubes, C. Jones, M. Joy, R. Keisler, L. Knox, A. T. Lee, E. M. Leitch, J. Liu, M. Lueker, D. Luong-Van, A. Mantz, D. P. Marrone, M. McDonald, J. J. McMahon, J. Mehl, S. S. Meyer, L. Mocanu, J. J. Mohr, S. S. Murray, T. Natoli, S. Padin, T. Plagge, C. Pryke, A. Rest, J. Ruel, J. E. Ruhl, B. R. Saliwanchik, A. Saro, J. T. Sayre, K. K. Schaffer, L. Shaw, E. Shirokoff, J. Song, H. G. Spieler, Z. Staniszewski, A. A. Stark, K. Story, C. W. Stubbs, R. Suhada, A. van Engelen, K. Vanderlinde, J. D. Vieira, A. Vikhlinin, R. Williamson, O. Zahn, A. Zenteno, ApJ, 763, 127, (2013).

[.5B.5B:Template:Story2011.5D.5D-33] South Pole Telescope Detections of the Previously Unconfirmed Planck Early Sunyaev-Zel'dovich Clusters in the Southern Hemisphere, K. Story, K. A. Aird, K. Andersson, R. Armstrong, G. Bazin, B. A. Benson, L. E. Bleem, M. Bonamente, M. Brodwin, J. E. Carlstrom, C. L. Chang, A. Clocchiatti, T. M. Crawford, A. T. Crites, T. de Haan, S. Desai, M. A. Dobbs, J. P. Dudley, R. J. Foley, E. M. George, M. D. Gladders, A. H. Gonzalez, N. W. Halverson, F. W. High, G. P. Holder, W. L. Holzapfel, S. Hoover, J. D. Hrubes, M. Joy, R. Keisler, L. Knox, A. T. Lee, E. M. Leitch, M. Lueker, D. Luong-Van, D. P. Marrone, J. J. McMahon, J. Mehl, S. S. Meyer, J. J. Mohr, T. E. Montroy, S. Padin, T. Plagge, C. Pryke, C. L. Reichardt, A. Rest, J. Ruel, J. E. Ruhl, B. R. Saliwanchik, A. Saro, K. K. Schaffer, L. Shaw, E. Shirokoff, J. Song, H. G. Spieler, B. Stalder, Z. Staniszewski, A. A. Stark, C. W. Stubbs, K. Vanderlinde, J. D. Vieira, R. Williamson, A. Zenteno, ApJ, 735, L36, (2011).

[.5B.5B:Template:Song2012.5D.5D-34] Redshifts, Sample Purity, and BCG Positions for the Galaxy Cluster Catalog from the First 720 Square Degrees of the South Pole Telescope Survey, J. Song, A. Zenteno, B. Stalder, S. Desai, L. E. Bleem, K. A. Aird, R. Armstrong, M. L. N. Ashby, M. Bayliss, G. Bazin, B. A. Benson, E. Bertin, M. Brodwin, J. E. Carlstrom, C. L. Chang, H. M. Cho, A. Clocchiatti, T. M. Crawford, A. T. Crites, T. de Haan, M. A. Dobbs, J. P. Dudley, R. J. Foley, E. M. George, D. Gettings, M. D. Gladders, A. H. Gonzalez, N. W. Halverson, N. L. Harrington, F. W. High, G. P. Holder, W. L. Holzapfel, S. Hoover, J. D. Hrubes, M. Joy, R. Keisler, L. Knox, A. T. Lee, E. M. Leitch, J. Liu, M. Lueker, D. Luong-Van, D. P. Marrone, M. McDonald, J. J. McMahon, J. Mehl, S. S. Meyer, L. Mocanu, J. J. Mohr, T. E. Montroy, T. Natoli, D. Nurgaliev, S. Padin, T. Plagge, C. Pryke, C. L. Reichardt, A. Rest, J. Ruel, J. E. Ruhl, B. R. Saliwanchik, A. Saro, J. T. Sayre, K. K. Schaffer, L. Shaw, E. Shirokoff, R. Suhada, H. G. Spieler, S. A. Stanford, Z. Staniszewski, A. A. Stark, K. Story, C. W. Stubbs, A. van Engelen, K. Vanderlinde, J. D. Vieira, R. Williamson, O. Zahn, ApJ, 761, 22, (2012).

[.5B.5B:Template:Hasselfield2013.5D.5D-35] The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data, M. Hasselfield, M. Hilton, T. A. Marriage, G. E. Addison, L. F. Barrientos, N. Battaglia, E. S. Battistelli, J. R. Bond, D. Crichton, S. Das, M. J. Devlin, S. R. Dicker, J. Dunkley, R. Dünner, J. W. Fowler, M. B. Gralla, A. Hajian, M. Halpern, A. D. Hincks, R. Hlozek, J. P. Hughes, L. Infante, K. D. Irwin, A. Kosowsky, D. Marsden, F. Menanteau, K. Moodley, M. D. Niemack, M. R. Nolta, L. A. Page, B. Partridge, E. D. Reese, B. L. Schmitt, N. Sehgal, B. D. Sherwin, J. Sievers, C. Sifóon, D. N. Spergel, S. T. Staggs, D. S. Swetz, E. R. Switzer, R. Thornton, H. Trac, E. J. Wollack, J. Cosmology Astropart. Phys., 7, 8, (2013).

[.5B.5B:Template:Marriage2011.5D.5D-36] The Atacama Cosmology Telescope: Sunyaev-Zel'dovich-Selected Galaxy Clusters at 148 GHz in the 2008 Survey, T. A. Marriage, V. Acquaviva, P. A. R. Ade, P. Aguirre, M. Amiri, J. W. Appel, L. F. Barrientos, E. S. Battistelli, J. R. Bond, B. Brown, B. Burger, J. Chervenak, S. Das, M. J. Devlin, S. R. Dicker, W. Bertrand Doriese, J. Dunkley, R. Dünner, T. Essinger-Hileman, R. P. Fisher, J. W. Fowler, A. Hajian, M. Halpern, M. Hasselfield, C. Hernández-Monteagudo, G. C. Hilton, M. Hilton, A. D. Hincks, R. Hlozek, K. M. Huffenberger, D. Handel Hughes, J. P. Hughes, L. Infante, K. D. Irwin, J. Baptiste Juin, M. Kaul, J. Klein, A. Kosowsky, J. M. Lau, M. Limon, Y.-T. Lin, R. H. Lupton, D. Marsden, K. Martocci, P. Mauskopf, F. Menanteau, K. Moodley, H. Moseley, C. B. Netterfield, M. D. Niemack, M. R. Nolta, L. A. Page, L. Parker, B. Partridge, H. Quintana, E. D. Reese, B. Reid, N. Sehgal, B. D. Sherwin, J. Sievers, D. N. Spergel, S. T. Staggs, D. S. Swetz, E. R. Switzer, R. Thornton, H. Trac, C. Tucker, R. Warne, G. Wilson, E. Wollack, Y. Zhao, ApJ, 737, 61, (2011).

[.5B.5B:Template:Menanteau2010.5D.5D-37] The Atacama Cosmology Telescope: Physical Properties and Purity of a Galaxy Cluster Sample Selected via the Sunyaev-Zel'dovich Effect, F. Menanteau, J. González, J.-B. Juin, T. A. Marriage, E. D. Reese, V. Acquaviva, P. Aguirre, J. W. Appel, A. J. Baker, L. F. Barrientos, E. S. Battistelli, J. R. Bond, S. Das, A. J. Deshpande, M. J. Devlin, S. Dicker, J. Dunkley, R. Dünner, T. Essinger-Hileman, J. W. Fowler, A. Hajian, M. Halpern, M. Hasselfield, C. Hernández-Monteagudo, M. Hilton, A. D. Hincks, R. Hlozek, K. M. Huffenberger, J. P. Hughes, L. Infante, K. D. Irwin, J. Klein, A. Kosowsky, Y.-T. Lin, D. Marsden, K. Moodley, M. D. Niemack, M. R. Nolta, L. A. Page, L. Parker, B. Partridge, N. Sehgal, J. Sievers, D. N. Spergel, S. T. Staggs, D. Swetz, E. Switzer, R. Thornton, H. Trac, R. Warne, E. Wollack, Apj, 723, 1523-1541, (2010).

[.5B.5B:Template:Sifon2013.5D.5D-38] The Atacama Cosmology Telescope: Dynamical Masses and Scaling Relations for a Sample of Massive Sunyaev-Zel'dovich Effect Selected Galaxy Clusters, C. Sifón, F. Menanteau, M. Hasselfield, T. A. Marriage, J. P. Hughes, L. F. Barrientos, J. González, L. Infante, G. E. Addison, A. J. Baker, N. Battaglia, J. R. Bond, D. Crichton, S. Das, M. J. Devlin, J. Dunkley, R. Dünner, M. B. Gralla, A. Hajian, M. Hilton, A. D. Hincks, A. B. Kosowsky, D. Marsden, K. Moodley, M. D. Niemack, M. R. Nolta, L. A. Page, B. Partridge, E. D. Reese, N. Sehgal, J. Sievers, D. N. Spergel, S. T. Staggs, R. J. Thornton, H. Trac, E. J. Wollack, ApJ, 772, 25, (2013).

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@@ Line 1: / Line 1: @@
-==The Catalogue of Compact Sources==
+{{DISPLAYTITLE:Catalogues}}
-===Product description===
+The 2015 compact source catalogues will not be regenerated using data from the 2018 release and remain the most up-to-date products.
-The PCCS2 and the PCCS2E are single-frequencies lists of sources extracted from the Planck full mission maps in total intensity and polarization. In the PCCS, the analaysis was done on the total intensity nominal mission maps, covering 15.5 months of data. In the PCCS2/PCCS2E, the full mission maps  in total intensity and polarization have been used, covering 48 months of observations.
+<div class="toccolours" style="background-color: #FFDAB9" >
-The analysis in polarization has been performed in a non-blind fashion, looking at the position of the sources previously detected in total intensity. As a result, polarization flux densities and polarization angles have been measured for hundreds of sources.
+=== (2015) Second Catalogue of Compact Sources  (PCCS2 and PCCS2E)===
-The main difference between the PCCS2 and PCCS2E is that the sources in the PCCS2 have been validated, either statistically or with external catalogues, while the PCCS2E contains all the remaining sources where an estimate of their reliability has not been made. By definition the reliability of the PCCS2 is > 80%, but a new flag has been added to the catalogues that will allow the users to select their desired level of reliability (e.g., 90%, 95%, etc.)
+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, 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%).
-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 projected flat patches. For the others, Point Spread Function fitting, Gaussian fitting and Aperture photoemtry, the analysis is performed on the sphere directly on the maps.
+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.
-The deeper completeness levels and, as a consequence, the higher number of sources compared with its predecessors the PCCS 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.
+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.
-[File:PCCS_POL_30_44_70.png|800px|thumb|center|Sky distribution of the PCCS" sources at three different channels: 30GHz (red circles), 44GHz (green circles) and
+<center><small>'''PCCS2 in intensity.'''</small></center>
-GHz (blue 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><small>'''PCCS2E in intensity.'''</small></center>
+[[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.
+<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 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 in four different channels: 100GHz (red circles); 143GHz (blue circles); 217GHz (green circles); and 353 GHz (black).]]
+<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); 217GHz (green circles); and 353 GHz (black).]]
+{| border="1" cellpadding="3" cellspacing="0" align="center" width=750px
+|+ <small>'''Table 1: PCCS2 and PCCS2E characteristics.'''</small>
+|- bgcolor="ffdead"
+! 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 [&mu;m]''' || 10561 || 6807 || 4260 || 3000 || 2098 || 1382 || 850 || 550 || 350
+|-
+!colspan="10" |Number of sources
+|-
+| PCCS2  || 1560 || 934 || 1296 || 1742 || 2160 || 2135 || 1344 || 1694 || 4891
+|-
+| PCCS2E || &mdash; || &mdash; || &mdash; || 2487 || 4139 || 16842 || 22665 || 31068 || 43290
+|-
+| Union PCCS2+PCCS2E  || &mdash; || &mdash; || &mdash; || 4229 || 6299 || 18977 || 24009 || 32762 || 48181
+|-
+!colspan="10" |Number of sources in the extragalactic zone<sup>a</sup>
+|-
+| PCCS2  || 745 || 367 || 504 || 1742 || 2160 ||  2135 ||  1344 ||  1694 ||  4891
+|-
+| PCCS2E || &mdash; || &mdash; ||  &mdash; ||    0 ||    0 ||    26 ||   289 ||   839 ||  2097
+|-
+| 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="1" |PCCS2
+|-
+| Minimum<sup>b</sup> ||  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
+|-
+!colspan="1" |PCCS2E
+|-
+| Minimum<sup>b</sup> || &mdash; || &mdash; || &mdash; || &mdash;  || &mdash; ||   189 ||   350 ||   597 ||   939
+|-
+| 90% completeness ||  &mdash; ||  &mdash; || &mdash; || &mdash; || &mdash; ||   144 ||   311 ||   557 ||   927
+|-
+| Uncertainty || &mdash; ||  &mdash; ||   &mdash; || &mdash; || &mdash; ||    35 ||    73 ||   144 ||   278
+|-
+|}
+'''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>
+'''<sup>b</sup>''' 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
+|+ <small>'''Table 2: PCCS2 & PCCS2E polarization characteristics for sources with polarized emission significance > 99.99%'''</small>
+|- bgcolor="ffdead"
+!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 density<sup>a</sup>  [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  ||  &mdash;  || &mdash;  || &mdash;  ||   43  ||  111  ||  325  ||  666
+|-
+|Minimum polarized flux density<sup>a</sup> [mJy]  || &mdash; || &mdash; || &mdash;  ||  121  ||   87  ||  114  ||  348
+|-
+|Polarized flux density uncertainty [mJy]  || &mdash;  ||  &mdash; || &mdash; ||   52  ||   44  ||   55  ||  178
+|-
+|Minimum polarized flux density for 90% completeness [mJy]  ||  &mdash;  ||  &mdash;  ||  &mdash;   ||  410  ||  613  ||  270  ||  567
+|-
+|Minimum polarized flux density for 95% completeness [mJy]  ||  &mdash;  ||  &mdash;  ||  &mdash;  ||  599  ||  893  ||  464  ||  590
+|-
+|Minimum polarized flux density for 100% completeness [mJy]  || &mdash;  || &mdash;  ||  &mdash;  ||  835  ||  893  ||  786  ||  958
+|-
+|}
+'''Table 2 Notes'''
+'''<sup>a</sup>''' 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
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_030_R2.04.fits|link=COM_PCCS_030_R2.04.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_044_R2.04.fits|link=COM_PCCS_044_R2.04.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_070_R2.04.fits|link=COM_PCCS_070_R2.04.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_100_R2.01.fits|link=COM_PCCS_100_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_143_R2.01.fits|link=COM_PCCS_143_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_217_R2.01.fits|link=COM_PCCS_217_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_857_R2.01.fits|link=COM_PCCS_857_R2.01.fits}} .
+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_143-excluded_R2.01.fits|link=COM_PCCS_143-excluded_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_217-excluded_R2.01.fits|link=COM_PCCS_217-excluded_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_353-excluded_R2.01.fits|link=COM_PCCS_353-excluded_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_545-excluded_R2.01.fits|link=COM_PCCS_545-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.
+{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
+|+ <small>'''PCCS2/PCCS2E FITS file structure'''</small>
+|- bgcolor="ffdead"
+!colspan="4" | Extension 0: Primary header, no data
+|- bgcolor="ffdead"
+! 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 || arcmin<sup>2</sup> || Area of the effective beam
+|-
+| FWHM_EFF || Real*4 || arcmin || FWHM computed from OMEGA_B assuming beam is Gaussian
+|-
+| OMEGA_B1 || Real*4 || arcmin<sup>2</sup> || Beam area within a radius of 1 &times; FWHM_EFF
+|-
+| OMEGA_B2 || Real*4 || arcmin<sup>2</sup> || Beam area within a radius of 2 &times; FWHM_EFF
+|- bgcolor="ffdead"
+!colspan="4" | Extension 1:  BINTABLE, EXTNAME = PCCS2_''fff'' (where ''fff'' is the frequency channel)
+|-bgcolor="ffdead"
+! Column Name || Data type || Units || Description
+|-bgcolor="ffdead"
+!colspan="4"|Identification
+|-
+|NAME || String || || Source name (see note 1)
+|-bgcolor="ffdead"
+!colspan="4"|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)
+|-bgcolor="ffdead"
+!colspan="4"|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 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_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 2 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 (see note 2)
+|-
+|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
+|-bgcolor="ffdead"
+!colspan="4"|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 &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_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_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_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 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.
+|-bgcolor="ffdead"
+!colspan="4"|Marginal polarization measurements (100-353 GHz only) &ndash; 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
+|-bgcolor="ffdead"
+!colspan="4"|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
+|-bgcolor="ffdead"
+!colspan="4"|Flags and validation (PCCS2 only)
+|-
+|HIGHEST_RELIABILITY_CAT || Integer*4 || || See note 7
+|-bgcolor="ffdead"
+!colspan="4"|Flags and validation (PCCS2E, 100-857 GHz only)
+|-
+|WHICH_ZONE || Integer*2 || || See note 8
+|-bgcolor="ffdead"
+!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&deg; radius.
+|-
+|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"
+!colspan="4"| 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'''
+# 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 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.
+# The P_STAT flag gives the status of the marginal polarization detection. Possible values are:
+#: 3 &ndash; bright, the P field filled in and all PX fields set to NULL;
+#: 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, 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, 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" 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:
+#: 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;
+#: 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 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 WHICH_ZONE column encodes the zone in which the source lies:
+#: 1 &ndash; source lies inside the filament mask;
+#: 2 &ndash; source lies inside the Galactic zone;
+#: 3 &ndash; 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
+: {{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_143-zoneMask_R2.01.fits|link=COM_PCCS_143-zoneMask_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_217-zoneMask_R2.01.fits|link=COM_PCCS_217-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_857-zoneMask_R2.01.fits|link=COM_PCCS_857-zoneMask_R2.01.fits}} .
+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"
+|+ <small>'''Zone map FITS file structure'''</small>
+|- bgcolor="ffdead"
+!colspan="4" | Extension 0: Primary header, no data
+|- bgcolor="ffdead"
+! FITS keyword || Data type || Units || Description
+|-
+|DATE || String ||  || Date of creation of file
+|- 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
+|-
+|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'''
+# 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);
+#: 1 &ndash; filament mask;
+#: 2 &ndash; Galactic zone;
+#: 3 &ndash; 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
+: {{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_143-SN-threshold_R2.01.fits|link=COM_PCCS_143-SN-threshold_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_217-SN-threshold_R2.01.fits|link=COM_PCCS_217-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_857-SN-threshold_R2.01.fits|link=COM_PCCS_857-SN-threshold_R2.01.fits}} .
+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_143-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_143-SN-threshold-85pc-reliability_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_217-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_217-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_857-SN-threshold-85pc-reliability_R2.01.fits|link=COM_PCCS_857-SN-threshold-85pc-reliability_R2.01.fits}} .
+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_143-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_143-SN-threshold-90pc-reliability_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_217-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_217-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_857-SN-threshold-90pc-reliability_R2.01.fits|link=COM_PCCS_857-SN-threshold-90pc-reliability_R2.01.fits}} .
+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_143-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_143-SN-threshold-95pc-reliability_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_217-SN-threshold-95pc-reliability_R2.01.fits|link=COM_PCCS_217-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_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 shown in the following table.
+{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
+|+ <small>'''Zone map FITS file structure'''</small>
+|- bgcolor="ffdead"
+!colspan="4" | Extension 0: Primary header, no data
+|- bgcolor="ffdead"
+! FITS keyword || Data type || Units || Description
+|-
+|DATE || String ||  || Date of creation of file
+|- 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
+|-
+|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'''
+# 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
+: {{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_143-noise-level_R2.01.fits|link=COM_PCCS_143-noise-level_R2.01.fits}}
+: {{PLASingleFile|fileType=cat|name=COM_PCCS_217-noise-level_R2.01.fits|link=COM_PCCS_217-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_857-noise-level_R2.01.fits|link=COM_PCCS_857-noise-level_R2.01.fits}} .
+The structure of the files shown in the following table.
+{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
+|+ <small>'''Zone map FITS file structure'''</small>
+|- bgcolor="ffdead"
+!colspan="4" | Extension 0: Primary header, no data
+|- bgcolor="ffdead"
+! FITS keyword || Data type || Units || Description
+|-
+|DATE || String ||  || Date of creation of file
+|- 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
+|-
+|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'''
+# 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 ====
+<hr>
+<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #EEE8AA;width:95%">
+'''Second Planck Release (2013): Description of the PCCS'''
+<div class="mw-collapsible-content">
+The Catalogue of Compact Sources
+'''Product description'''
+[[File:PCCS_skydist.png|400px|thumb|right|Sky distribution of the PCCS sources at three different channels: 30GHz (pink circles), 143GHz (magenta circles) and
+GHz (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.
@@ Line 28: / 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
 |-
-|'''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
@@ Line 46: / Line 534: @@
 '''Notes'''
-# The Planck beams are described in {{PlanckPapers|planck2013-p02d}}; {{PlanckPapers|planck2013-p03c}}. This table shows the values which were adopted for the PCCS (derived from the effective beams).
+# The Planck beams are described in {{PlanckPapers|planck2013-p02d}} and {{PlanckPapers|planck2013-p03c}}. This table shows the values which were adopted for the PCCS (derived from the effective beams).
 # In the extragalactic zone (48% of the sky; see Fig. 2 in {{PlanckPapers|planck2013-p05}}).
 # In the Galactic zone (52% of the sky; see Fig. 2 in {{PlanckPapers|planck2013-p05}}).
@@ Line 54: / Line 542: @@
 Before using the PCCS, please read the Cautionary Notes in the PCCS general description [[Compact Source catalogues|section]]. For full details, see paper {{PlanckPapers|planck2013-p05}}.
-===Production process===
+'''Production process'''
 For a description of the production and validation processes of the PCCS see the corresponding [[Compact Source catalogues|section]].
-===Inputs===
+'''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 {{PlanckPapers|planck2013-p02}}{{PlanckPapers|planck2013-p03}}. 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 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 {{PlanckPapers|planck2013-p02}} and {{PlanckPapers|planck2013-p03}}. 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:
@@ Line 66: / Line 556: @@
 * [[Effective Beams | effective beams]]
-===Related products===
+'''Related products'''
 Other products that are related and share some commonalities with the product being described here are the other catalogues:
 # [[Catalogues#The ERCSC | ERCSC]]
 # [[Catalogues#The SZ catalogues | SZ catalogue]]
-===File names===
+'''File names'''
 : {{PLASingleFile|fileType=cat|name=COM_PCCS_030_R1.30.fits|link=COM_PCCS_030_R1.30.fits}}
 : {{PLASingleFile|fileType=cat|name=COM_PCCS_044_R1.30.fits|link=COM_PCCS_044_R1.30.fits}}
@@ Line 82: / Line 574: @@
 : {{PLASingleFile|fileType=cat|name=COM_PCCS_857_R1.20.fits|link=COM_PCCS_857_R1.20.fits}}
-===Meta Data ===
+'''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
@@ Line 90: / Line 583: @@
 !colspan="4" | Extension 0: Primary header, no data
 |- bgcolor="ffdead"
-! FITS Keyword || Data Type || Units || Description
+! FITS keyword || Data type || Units || Description
 |-
 |INSTRUME || String || || LFI or HFI
@@ Line 110: / Line 603: @@
 !colspan="4" | Extension 1:  (BINTABLE)
 |-bgcolor="ffdead"
-! Column Name || Data Type || Units || Description
+! Column Name || Data type || Units || Description
 |-bgcolor="ffdead"
 !colspan="4"|Identification
 |-
-|NAME || String || || Source name (Note 1)
+|NAME || String || || Source name (note 1)
 |-bgcolor="ffdead"
 !colspan="4"|Source Position
@@ Line 144: / Line 637: @@
 |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
@@ Line 152: / Line 645: @@
 |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
@@ Line 160: / Line 653: @@
 !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
 |-
-|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
@@ Line 185: / Line 678: @@
 '''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 EXT_VAL flag takes the value of 0, 1, or 2, based on the following conditions:
@@ Line 194: / Line 687: @@
-== The SZ catalogues ==
+</div>
+</div>
+<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 )'''
+<div class="mw-collapsible-content">
+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 |<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}}.
+Full details on the construction, contents and usage of the ERCSC, ECC and ESZ catalogues can be found in {{PlanckPapers|planck2011-1-10}}, {{PlanckPapers|planck2011-5-1a}},  {{PlanckPapers|planck2011-7-7b}}.
+[[File:Ercscsensfig.png | 500px | center | thumb |'''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 ({{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>
+<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 ===
+<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 />
+Traits:<br />
+* 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 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)
+|-
+| PCCS2
+| Planck’s PCCS2 region
+|align="right"| 57
+|-
+| PCCS2E <math display="inline">\wedge \, |glat| > 10^\circ</math>
+| Planck’s PCCS2E region and <math display="inline">|glat| > 10^\circ</math>
+|align="right"| 168
+|-
+| <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
+|-
+|
+|
+|
+|
+|
+|
+|-
+| 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 <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
+|-
+| BEEPDEC
+| double
+| 8
+| Degrees
+| J2000 DEC estimated by <span class="sans-serif">BeeP</span>
+| 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 display="inline">< 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 <span class="sans-serif">BeeP</span>’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|[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 display="inline">\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 display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
+|-
+| BETAH2SB
+| 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>)
+|-
+| 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 display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
+|-
+| TH2SB
+| 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>)
+|-
+| 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
+|-
+| 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>)
+|-
+| 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>)
+|-
+| 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
+|-
+| 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>)
+|-
+| 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>)
+|-
+| 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 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>)
+|-
+| 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>)
+|-
+| 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
+|-
+| 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>)
+|-
+| FREES857H2SB
+| 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>)
+|-
+| FREES545
+| double
+| 8
+| Jy
+| Flux density at <math display="inline">545</math> GHz; Estimated directly at Planck’s <math display="inline">545</math> GHz map
+| Posterior median value
+|-
+| FREES545L2SB
+| 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>)
+|-
+| FREES545H2SB
+| 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>)
+|-
+| FREES353
+| double
+| 8
+| Jy
+| Flux density at <math display="inline">353</math> GHz; Estimated directly at Planck’s <math display="inline">353</math> GHz map
+| Posterior median value
+|-
+| FREES353L2SB
+| 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>)
+|-
+| FREES353H2SB
+| 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>)
+|-
+| 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 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
+|-
+| 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 display="inline">\chi^2</math> of the maximum likelihood estimates
+| Reduced <math display="inline">\chi^2</math>
+|-
+|
+|
+|
+|
+|
+|
+|-
+| 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)
+|-
+| 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)
+|-
+| 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
+|-
+| 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>)
+|-
+| 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>)
+|-
+| 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 <math display="inline">2.275\%</math> percentile (<math display="inline">-2 \sigma</math>)
+|-
+| 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>)
+|-
+| 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
+|-
+| 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>)
+|-
+| 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>)
+|-
+| 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
+| <math display="inline">\chi^2</math> of the maximum likelihood estimates
+| Reduced <math display="inline">\chi^2</math>
+|-
+| SNRR3000
+| double
+| 8
+| Unitless
+| Signal to Noise Ratio Raw (SNRr) at <math display="inline">3000</math> GHz
+| Source average brightness divided the background standard deviation brightness
+|-
+| SNRR30001S
+| double
+| 8
+| Unitless
+| 1 <math display="inline">\sigma</math> error bar of the SNRr at <math display="inline">3000</math> GHz
+| Source brightness error bar divided the background standard deviation brightness
+|-
+| SNRR857
+| double
+| 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.
+===== Flux density correction =====
+<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
+<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 />
+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.
+==== Spectral Energy Density (SED) plots ====
+[[File:xSupPicts-COM_PCCS_857_R2_01__PCCS2_857_G171_77_59_53_s.png|500px|center|none]]
+<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>
+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,
+* <span class="sans-serif">SOURCE</span>: Is the PCCS2+2E name of the source.
+* <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.
+* <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 />
+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 />
+* Middle panel - ‘Free’ channel amplitudes.<br />
+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 />
+* 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.
+* 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.
+==== Parameter posterior distributions (‘''corner plots''’) ====
+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]]).
+* <span class="sans-serif">SOURCE</span>: Is the PCCS2+2E name of the source.
+* <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).
+* 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
+|-
+|NAME || String || || Source Name
+|-
+|SNR || real*8 || || Maximum S/N over the 857, 545, and 353 GHz Planck cold residual maps
+|-
+|SNR_857 || real*8 || || S/N of the cold residual detection at 857 GHz
+|-
+|SNR_545 || real*8 || || S/N of the cold residual detection at 545 GHz
+|-
+|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
+|-
+|GLON || real*8 || deg || Galactic longitude based on morphology fitting
+|-
+|GLAT || real*8 || deg || Galactic latitude based on morphology fitting
+|-
+|RA || real*8 || deg || Right ascension (J2000) in degrees transformed from (GLON, GLAT)
+|-
+|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
+|-
+|GAU_MAJOR_AXIS_SIG || real*8 || arcmin || 1&sigma; uncertainty on the FWHM along the major axis
+|-
+|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
+|-
+|GAU_POSITION_ANGLE || real*8 || rad || Position angle of the elliptical Gaussian (see note 1)
+|-
+|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
+|-
+|FLUX_3000_CLUMP || real*8 || Jy || Flux density of the clump at 3 THz
+|-
+|FLUX_3000_CLUMP_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the clump at 3 THz
+|-
+|FLUX_857_CLUMP || real*8 || Jy || Flux density of the clump at 857 GHz
+|-
+|FLUX_857_CLUMP_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the clump at 857 GHz
+|-
+|FLUX_545_CLUMP || real*8 || Jy || Flux density of the clump at 545 GHz
+|-
+|FLUX_545_CLUMP_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the clump at 545 GHz
+|-
+|FLUX_353_CLUMP || real*8 || Jy || Flux density of the clump at 353 GHz
+|-
+|FLUX_353_CLUMP_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the clump at 353 GHz
+|-
+|FLUX_3000_WBKG || real*8 || Jy || Flux density of the warm background at 3 THz (see note 2)
+|-
+|FLUX_3000_WBKG_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of warm background at 3 THz
+|-
+|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
+|-
+|FLUX_545_WBKG || real*8 || Jy || Flux density of the warm background at 545 GHz
+|-
+|FLUX_545_WBKG_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the warm background at 545 GHz
+|-
+|FLUX_353_WBKG || real*8 || Jy || Flux density of the warm background at 353 GHz
+|-
+|FLUX_353_WBKG_SIG || real*8 || Jy || 1&sigma; uncertainty on the flux density of the warm background at 353 GHz
+|-
+|FLUX_QUALITY || int*4 || 1-3 || Category of flux density reliability (see note 3)
+|-
+|FLUX_BLENDING || int*4 || 0/1 || 1 if blending issue with flux density estimate (see note 4)
+|-
+|FLUX_BLENDING_IDX || int*8 || || Catalogue index of the closest source responsible for blending
+|-
+|FLUX_BLENDING_ANG_DIST || real*8 || arcmin || Angular distance to the closest source responsible for blending
+|-
+|FLUX_BLENDING_BIAS_3000 || real*8 || % || Relative bias of the flux density at 3 THz due to blending
+|-
+|FLUX_BLENDING_BIAS_857 || real*8 ||  % || Relative bias of the flux density at 857 GHz due to blending
+|-
+|FLUX_BLENDING_BIAS_545 || real*8 ||  % || Relative bias of the flux density at 545 GHz due to blending
+|-
+|FLUX_BLENDING_BIAS_353 || real*8 ||  % || Relative bias of the flux density at 353 GHz due to blending
+|- bgcolor="ffdead"
+! colspan="4" | Distance
+|- bgcolor="ffdead"
+! FITS Keyword || Data type || Units || Description
+|-
+|DIST_KINEMATIC || real*8 || kpc || Distance estimate [1] using kinematics
+|-
+|DIST_KINEMATIC_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [1] using kinematics
+|-
+|DIST_OPT_EXT_DR7 || real*8 || kpc || Distance estimate [2] using optical extinction on SDSS DR7
+|-
+|DIST_OPT_EXT_DR7_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [2] using optical extinction on SDSS DR7
+|-
+|DIST_OPT_EXT_DR9 || real*8 || kpc || Distance estimate [3] using optical extinction on SDSS DR9
+|-
+|DIST_OPT_EXT_DR9_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [3] using optical extinction on SDSS DR9
+|-
+|DIST_NIR_EXT_IRDC || real*8 || kpc || Distance estimate  [4] using near-IR extinction towards IRDCs
+|-
+|DIST_NIR_EXT_IRDC_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate  [4] using near-IR extinction towards IRDCs
+|-
+|DIST_NIR_EXT || real*8 || kpc || Distance estimate [5] using near-IR extinction
+|-
+|DIST_NIR_EXT_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [5] using near-IR extinction
+|-
+|DIST_MOLECULAR_COMPLEX || real*8 || kpc || Distance estimate [6] using molecular complex association
+|-
+|DIST_MOLECULAR_COMPLEX_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [6] using molecular complex association
+|-
+|DIST_HKP_GCC || real*8 || kpc || Distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
+|-
+|DIST_HKP_GCC_SIG || real*8 || kpc || 1&sigma; uncertainty on the distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
+|-
+|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
+|-
+|TEMP_BETA2_CLUMP || real*8 || K || Temperature of the clump with &beta; = 2
+|-
+|TEMP_BETA2_CLUMP_SIG || real*8 || K || 1&sigma; uncertainty on the temperature of the clump with &beta; = 2
+|-
+|TEMP_BETA2_CLUMP_LOW1 || real*8 || K || Lower 68% confidence limit of the clump temperature with &beta; = 2
+|-
+|TEMP_BETA2_CLUMP_UP1 || real*8 || K || Upper 68% confidence limit of the clump temperature with &beta; = 2
+|-
+|TEMP_WBKG || real*8 || K || Temperature of the warm background with &beta; as a free parameter (see note 6)
+|-
+|TEMP_WBKG_SIG || real*8 || K || 1&sigma; dispersion of the warm background temperature with &beta; free
+|-
+|TEMP_WBKG_LOW1 || real*8 || K || Lower 68% confidence limit of the warm background temperature with &beta; free
+|-
+|TEMP_WBKG_UP1 || real*8 || K || Upper 68% confidence limit of the warm background temperature with &beta; free
+|-
+|BETA_WBKG || real*8 || || Spectral index &beta; of the warm background (see note 6)
+|-
+|BETA_WBKG_SIG || real*8 || || 1&sigma; uncertainty (from MCMC) of the emissivity spectral index &beta; of the warm background
+|-
+|BETA_WBKG_LOW1 || real*8 || || Lower 68% confidence limit of the emissivity spectral index &beta; of the warm background
+|-
+|BETA_WBKG_UP1 || real*8 || || Upper 68% confidence limit of the emissivity spectral index &beta; of the warm background
+|-
+|TEMP_BETA2_WBKG || real*8 || K || Temperature of the warm background with &beta; = 2
+|-
+|TEMP_BETA2_WBKG_SIG || real*8 || K || 1&sigma; uncertainty on the temperature of the warm background with &beta; = 2
+|-
+|TEMP_BETA2_WBKG_LOW1 || real*8 || K || Lower 68% confidence limit of the warm background temperature with &beta; = 2
+|-
+|TEMP_BETA2_WBKG_UP1 || real*8 || K || Upper 68% confidence limit of the warm background temperature with &beta; = 2
+|- bgcolor="ffdead"
+! colspan="4" | Physical properties
+|- bgcolor="ffdead"
+! FITS Keyword || Data type || Units || Description
+|-
+|NH2 || real*8 || cm<sup>-2</sup> || Column density <i>N</i><sub>H<sub>2</sub></sub> of the clump
+|-
+|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
+|-
+|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 || <i>M</i><sub>&#9737;</sub> || Mass estimate of the clump
+|-
+|MASS_SIG  || real*8 || <i>M</i><sub>&#9737;</sub> || 1&sigma; uncertainty on the mass estimate of the clump
+|-
+|MASS_LOW[1,2,3]  || real*8 || <i>M</i><sub>&#9737;</sub> || Lower 68%, 95%, and 99% confidence limit of the mass estimate
+|-
+|MASS_UP[1,2,3]  || real*8 || <i>M</i><sub>&#9737;</sub> || 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&sigma; 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&sigma; 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 || <i>L</i><sub>&#9737;</sub> || Luminosity of the clump
+|-
+|LUMINOSITY_SIG  || real*8 || <i>L</i><sub>&#9737;</sub> || 1&sigma; uncertainty on the luminosity estimate of the clump
+|-
+|LUMINOSITY_LOW[1,2,3]  || real*8 || <i>L</i><sub>&#9737;</sub>  || Lower 68%, 95%, and 99% confidence limit of the luminosity estimate
+|-
+|LUMINOSITY_UP[1,2,3]  || real*8 || <i>L</i><sub>&#9737;</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
+|}
+'''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.]]
+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 }}.
+Its structure is as follows.
+{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=1000px
+|+ '''FITS file structure'''
+|- bgcolor="ffdead"
+! colspan="4" | Identification
+|- bgcolor="ffdead"
+! FITS Keyword || Data type || Units || Description
+|-
+|NAME || String || || Source name
+|-
+|SNR_X545 || real*8 || || S/N in the 545 GHz excess map
+|-
+|SNR_D857 || real*8 || || S/N in the 857 GHz cleaned map
+|-
+|SNR_D545 || real*8 || || S/N in the 545 GHz cleaned map
+|-
+|SNR_D353 || real*8 || || S/N in the 353 GHz cleaned map
+|- bgcolor="ffdead"
+! colspan="4" | Source position
+|- bgcolor="ffdead"
+! FITS Keyword || Data type || Units || Description
+|-
+|GLON || real*8 || deg || Galactic longitude based on morphology fitting
+|-
+|GLAT || real*8 || deg || Galactic latitude based on morphology fitting
+|-
+|RA || real*8 || deg || Right ascension (J2000) in degrees transformed from (GLON, GLAT)
+|-
+|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
+|-
+|GAU_MAJOR_AXIS_SIG || real*8 || arcmin || 1&sigma; uncertainty on the FWHM along the major axis
+|-
+|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
+|-
+|GAU_POSITION_ANGLE || real*8 || rad || Position angle of the elliptical Gaussian (see note 1)
+|-
+|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
+|-
+|FLUX_CLEAN_857 || real*8 || Jy || Flux density of the clump at 857 GHz
+|-
+|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
+|}
+== (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.
+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.
+==== Union catalogue ====
+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}}''.
+{| 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
+|-
+|INSTRUME || String || || Instrument (HFI)
+|-
+| 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 <i>c</i><sub>500</sub> parameter
+|-
+| PP_Y2YFH || Real*4 || || Conversion factor from <i>Y</i> to <i>Y</i><sub>500</sub>
+|- bgcolor="ffdead"
+!colspan="4" | Extension 1: BINTABLE, EXTNAME = PSZ2_UNION
+|- bgcolor="ffdead"
+! Column Name || Data type || Units || Description
+|-
+|INDEX || Int*4 || || Index used to cross-reference with individual catalogues
+|-
+|NAME || String || || Source name (see note 1)
+|-
+|GLON || Real*8 || deg || Galactic longitude
+|-
+|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 the detection
+|-
+|PIPELINE || Int*4 || || Pipeline from which information is taken (reference pipeline): 1= MMF1; 2 = MMF3; 3 = PwS
+|-
+|PIPE_DET || Int*4 || || Pipelines that detect this object (see note 2)
+|-
+|PCCS2 || Bool || || Indicates whether detection matches with any in PCCS2 catalogues
+|-
+|PSZ || Int*4 || || Index of matching detection in PSZ1, or -1 if new detection
+|-
+|IR_FLAG || Int*1 || || Flag denoting heavy IR contamination
+|-
+|Q_NEURAL || Real*4 || || Neural network quality flag (see note 3)
+|-
+|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
+|-
+|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
+|-
+|VALIDATION || Int*4 || || External validation status (see note 4)
+|-
+|REDSHIFT_ID || String || || External identifier of cluster associated with redshift measurement (see note 5)
+|-
+|REDSHIFT || Real*4 || || Redshift of cluster (see note 5)
+|-
+|MSZ || Real*4 || 10<sup>14</sup>&nbsp;<i>M</i><sub>&#9737;</sub> || SZ mass proxy (see note 6)
+|-
+|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)
+|-
+|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)
+|-
+|MCXC || String || || Identifier of X-ray counterpart in the MCXC, if one is present
+|-
+|REDMAPPER || String || || Identifier of optical counterpart in the RedMAPPer catalogue, if one is present
+|-
+|ACT || String || || Identifier of SZ counterpart in the ACT catalogues, if one is present
+|-
+|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
+|-
+|INSTRUME || String || || Instrument (HFI)
+|-
+| 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 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
+|-
+| PP_Y2YFH || Real*4 || || Conversion factor from <i>Y</i> to <i>Y</i><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
+|-
+|NAME || String || || Source name (see note 1)
+|-
+|GLON || Real*8 || deg || Galactic longitude
+|-
+|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
+|-
+| 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
+|-
+| NAXIS1 || Integer || 256 || Dimension 1
+|-
+| NAXIS2 || Integer || 256 || Dimension 2
+|-
+| NAXIS3 || Integer || <i>N</i><sub>det</sub> || Dimension 3 = Number of detections
+|- bgcolor="ffdead"
+! Keyword || Data type || Value || Description
+|-
+| PIPELINE || String || || Name of detection pipeline
+|- bgcolor="ffdead"
+! colspan="4" | Extension 3: IMAGE, EXTNAME = PSZ2_MSZ_ARRAY (see note 3)
+|- bgcolor="ffdead"
+! Keyword || Data type || Value || Description
+|-
+| NAXIS1 || Integer || 100 || Dimension 1
+|-
+| NAXIS2 || Integer || 4 || Dimension 2
+|-
+| NAXIS3 || Integer || <i>N</i><sub>det</sub> || Dimension 3 = Number of detections
+|- bgcolor="ffdead"
+! Keyword || Data type || Value || Description
+|-
+| 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
+|-
+|INSTRUME || String || || Instrument (HFI)
+|-
+| 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 time of the survey: yyyy-mm-dd
+|-
+| DATE-END || String || || End time of the survey: yyyy-mm-dd
+|-
+| 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
+|-
+|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"
+! 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"
+! colspan="4" | Extension 3: IMAGE, EXTNAME = YGRID (see note 3)
+|- 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 <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
+|-
+| NAXIS1 || Integer || 32 || Dimension 1
+|- bgcolor="ffdead"
+! Keyword || Data type || Value || Description
+|-
+| 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
+|-
+| NAXIS1 || Integer || 12 || Dimension 1
+|- bgcolor="ffdead"
+! Keyword || Data type || Value || Description
+|-
+| COL1 || String || S/N || Grid values of S/N threshold
+|}
+'''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.
+# 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.
+# 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.
+=== Previous releases: (2013) PSZ1 ===
+<div class="toccolours mw-collapsible mw-collapsed" style="background-color: #EEE8AA;width:95%">
+'''Second Planck Release (2013): Description of the Planck SZ Catalogue'''
+<div class="mw-collapsible-content">
 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}}.
@@ Line 203: / Line 2,508: @@
 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, $\theta_\mathrm{s}$, 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.
+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 $\theta_\mathrm{s}$ 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.
+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====
+'''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}}''.
@@ Line 216: / Line 2,522: @@
 !colspan="4" | Extension 0: Primary header, no data
 |- bgcolor="ffdead"
-! FITS Keyword || Data Type || Units || Description
+! FITS Keyword || Data type || Units || Description
 |-
 |INSTRUME || String || || Instrument.
@@ Line 236: / Line 2,542: @@
 | PROCVER || String || || Data version.
 |-
-| PP_ALPHA || Real*4 || || GNFW pressure profile $\alpha$ parameter.
+| PP_ALPHA || Real*4 || || GNFW pressure profile &alpha; parameter.
 |-
-| PP_BETA || Real*4 || || GNFW pressure profile $\beta$ parameter.
+| PP_BETA || Real*4 || || GNFW pressure profile &beta; parameter.
 |-
-| PP_GAMMA || Real*4 || || GNFW pressure profile $\gamma$ parameter.
+| PP_GAMMA || Real*4 || || GNFW pressure profile &gamma; parameter.
 |-
-| PP_C500 || Real*4 || || GNFW pressure profile $c_{500}$ parameter.
+| PP_C500 || Real*4 || || GNFW pressure profile <i>c</i><sub>500</sub> parameter.
 |-
-| PP_Y2YFH || Real*4 || || Conversion factor from $Y$ to $Y_{500}$.
+| 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
+! Column Name || Data type || Units || Description
 |-
 |INDEX || Int*4 || || Index. Used to cross-reference with individual catalogues.
 |-
-|NAME || String || || Source name, (Note 1)
+|NAME || String || || Source name (note 1).
 |-
 |GLON || Real*8 || degrees || Galactic longitude.
@@ Line 273: / Line 2,579: @@
 |PCCS || Bool || || Indicates whether detection matches any PCCS source.
 |-
-|VALIDATION || Int*4 || || External validation status (Note 3)
+|VALIDATION || Int*4 || || External validation status (note 3)
 |-
 |ID_EXT || String|| || External identifier of cluster.
@@ Line 281: / Line 2,587: @@
 |COSMO || Bool || || Detection is in the cosmology sample.
 |-
-|COMMENT|| Bool || || Detection has a comment in the associated text file (Note 4).
+|COMMENT|| Bool || || Detection has a comment in the associated text file (note 4).
 |}
 '''Notes'''
-# format is ''PSZ1 Glll.ll+mn;bb.b'' where (l,b) are the Galactic and truncated to 2 decimal places.
+# 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.
 # 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.
 # 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.
-====Individual Catalogues====
+'''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)
@@ Line 304: / Line 2,612: @@
 ! colspan="4" | Ext. 0: Primary header, no data
 |- bgcolor="ffdead"
-! FITS Keyword || Data Type || Units || Description
+! FITS Keyword || Data type || Units || Description
 |-
 |INSTRUME || String || || Instrument.
@@ Line 324: / Line 2,632: @@
 | PROCVER || String || || Data version.
 |-
-| PP_ALPHA || Real*4 || || GNFW pressure profile $\alpha$ parameter.
+| PP_ALPHA || Real*4 || || GNFW pressure profile &alpha; parameter.
 |-
-| PP_BETA || Real*4 || || GNFW pressure profile $\beta$ parameter.
+| PP_BETA || Real*4 || || GNFW pressure profile &beta; parameter.
 |-
-| PP_GAMMA || Real*4 || || GNFW pressure profile $\gamma$ parameter.
+| PP_GAMMA || Real*4 || || GNFW pressure profile &gamma; parameter.
 |-
-| PP_C500 || Real*4 || || GNFW pressure profile $c_{500}$ parameter.
+| PP_C500 || Real*4 || || GNFW pressure profile <i>c</i><sub>500</sub> parameter.
 |-
-| PP_Y2YFH || Real*4 || || Conversion factor from $Y$ to $Y_{500}$.
+| PP_Y2YFH || Real*4 || || Conversion factor from <i>Y</i> to <i>Y</i><sub>500</sub>.
 |- bgcolor="ffdead"
@@ Line 338: / Line 2,646: @@
 ! colspan="4" | Ext. 1: EXTNANE = ''PSZ_INDIVIDUAL'' (BINTABLE)
 |- bgcolor="ffdead"
-! Column Name || Data Type || Units || Description
+! Column Name || Data type || Units || Description
 |-
 |INDEX || Int*4 || || Index from union catalogue.
 |-
-|NAME || String || || Source name - see Note1
+|NAME || String || || Source name - see note 1.
 |-
-|GLON || Real*8 || degrees || Galactic longitude.
+|GLON || Real*8 || deg || Galactic longitude.
 |-
-|GLAT || Real*8 || degrees || Galactic latitude.
+|GLAT || Real*8 || deg || Galactic latitude.
 |-
-|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).
 |-
 |POS_ERR || Real*4 || arcmin || Position uncertainty (approximate 68% confidence interval). See [[#Caveats|Caveats]] below.
@@ Line 356: / Line 2,664: @@
 |SNR || Real*4 || || Signal-to-noise ratio of the detection.
 |-
-|SNR_COMPAT || Real*4 || || SNR of the detection in compatibility mode (Note 2)
+|SNR_COMPAT || Real*4 || || S/N of the detection in compatibility mode (note 2).
 |-
-|TS_MIN || Real*4 || || Minimum value of $\theta_\mathrm{s}$ in grid in second extension HDU (see below).
+|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 $\theta_\mathrm{s}$ 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 $Y$ 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 $Y$ 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
+! Keyword || Data type || Value || Description
 |-
 | PIPELINE || String || || Name of detection pipeline.
@@ Line 373: / Line 2,681: @@
-! colspan="4" | Ext. 2: EXTNAME = ''PSZ_PROBABILITY'' (IMAGE) - Note 3
+! colspan="4" | Ext. 2: EXTNAME = ''PSZ_PROBABILITY'' (IMAGE) - note 3
 |- bgcolor="ffdead"
-! Keyword || Data Type || Value || Description
+! Keyword || Data type || Value || Description
 |-
 | NAXIS1 || Integer || 256 || Dim 1
@@ Line 383: / Line 2,691: @@
 | NAXIS3 || Integer || Nsources || Dim 3 = Number of sources
 |- bgcolor="ffdead"
-! Keyword || Data Type || Value || Description
+! Keyword || Data type || Value || Description
 |-
 | PIPELINE || String || || Name of detection pipeline.
 |}
 '''Notes'''
-# Format ''PSZ1 Glll.ll&plusmn;bb.bb'' where (l, b) are the Galactic coordinates truncated to 2 decimal places.
+# Format ''PSZ1 Glll.ll&plusmn;bb.bb'' where <i>l</i> and <i>b</i> are the Galactic coordinates truncated to two decimal places.
-# 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.
+# 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 $\theta_\mathrm{s}$ 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 $Y$.
+# 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>.
+'''Mask'''
+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}}''.
+ It is in GALACTIC coordinates, NESTED ordering, NSIDE=2048.
-====Mask====
-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}}''. <span style="color:red">
-It is in GALACTIC coordinates, NESTED ordering, NSIDE=2048.
-====Additional information====
+'''Additional information'''
 A set of comments on the union catalogue is available in
@@ Line 415: / Line 2,728: @@
 ! colspan="4" | Ext. 0:  (BINTABLE)
 |- bgcolor="ffdead"
-! Column Name || Data Type || Units || Description
+! Column Name || Data type || Units || Description
 |-
 |INDEX || Int*4 || || Index from union catalogue.
@@ Line 423: / Line 2,736: @@
 |REDSHIFT || Real*4 ||  || Redshift
 |-
-|REDSHIFT_SOURCE || Int*4 ||  || Source for redshift - see Note 4.
+|REDSHIFT_SOURCE || Int*4 ||  || Source for redshift - see note 4.
 |-
 |ALT_NAME   || String ||  || Alternative names.
@@ Line 443: / Line 2,756: @@
 |ERRM_M_YZ_500 || Real*4 || 10<sup>14</sup> Msol || Error sup. on M_YZ_500.
 |-
-|S_X || Real*4 || erg/s/cm<sup>2</sup>  || Unabsorbed X-ray flux - see Note 1.
+|S_X || Real*4 || erg/s/cm<sup>2</sup>  || Unabsorbed X-ray flux - see note 1.
 |-
 |ERR_S_X || Real*4 || erg/s/cm<sup>2</sup>  || Error on unabsorbed X-ray flux.
 |-
-|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.
+|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.
 |-
-|SN_PSX || Real*4 ||  || Signal to noise for PSZ clusters identified with MCXC clusters - see Note 3.
+|SN_PSX || Real*4 ||  || Signal to noise for PSZ clusters identified with MCXC clusters - see note 3.
 |}
@@ Line 457: / Line 2,770: @@
 # 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:
-      -1 : No redshift available
+      -1 : No redshift available;
-: MCXC updated compilation{{BibCite|Piffaretti2011}}
+: MCXC updated compilation{{BibCite|Piffaretti2011}};
-: Databases NED and SIMBAD-CDS
+: Databases NED and SIMBAD-CDS;
-: SDSS cluster catalogue{{BibCite|Wen2012}}
+: SDSS cluster catalogue{{BibCite|Wen2012}};
-: SDSS cluster catalogue{{BibCite|Szabo2011}}
+: SDSS cluster catalogue{{BibCite|Szabo2011}};
-: SPT{{BibCite|Vanderlinde2010}}{{BibCite|Williamson2011}}{{BibCite|Andersson2011}}{{BibCite|Plagge2010}}{{BibCite|Reichardt2013}}{{BibCite|Story2011}}{{BibCite|Song2012}}
+: SPT{{BibCite|Vanderlinde2010}}{{BibCite|Williamson2011}}{{BibCite|Andersson2011}}{{BibCite|Plagge2010}}{{BibCite|Reichardt2013}}{{BibCite|Story2011}}{{BibCite|Song2012}};
-: ACT{{BibCite|Hasselfield2013}}{{BibCite|Marriage2011}}{{BibCite|Menanteau2010}}{{BibCite|Sifon2013}}
+: ACT{{BibCite|Hasselfield2013}}{{BibCite|Marriage2011}}{{BibCite|Menanteau2010}}{{BibCite|Sifon2013}};
-: Search in SDSS galaxy catalogue from Planck Collab.
+: Search in SDSS galaxy catalogue from Planck Collab.;
-: XMM-Newton confirmation from Planck Collab.
+: XMM-Newton confirmation from Planck Collab.;
-: ENO-imaging confirmation from Planck Collab.
+: ENO-imaging confirmation from Planck Collab.;
-: WFI-imaging confirmation from Planck Collab.
+: WFI-imaging confirmation from Planck Collab.;
-: NTT-spectroscopic confirmation from Planck Collab.
+: NTT-spectroscopic confirmation from Planck Collab.;
-: RTT-spectroscopic confirmation from Planck Collab.
+: RTT-spectroscopic confirmation from Planck Collab.;
-: NOT-spectroscopic confirmation from Planck Collab.
+: NOT-spectroscopic confirmation from Planck Collab.;
-: GEMINI-spectroscopic confirmation from Planck Collab.
+: GEMINI-spectroscopic confirmation from Planck Collab.;
 : ENO-spectroscopic confirmation from Planck Collab.
-===Caveats===
+'''Caveats'''
 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)
-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.
+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.
-== 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  c ryogenic 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 $|b| > 30$ 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}}.
-Full details on the construction, contents and usage of the ERCSC, ECC and ESZ catalogues can be found in {{PlanckPapers|planck2011-1-10}}, {{PlanckPapers|planck2011-5-1a}}, {{PlanckPapers|planck2011-7-7b}}.
-[[File:Ercscsensfig.png | 500px | center | thumb |'''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 ({{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}}.
 ==References==
-<References />
+<References/>
 [[Category:Mission products|005]]

Difference between revisions of "Catalogues"

Latest revision as of 12:58, 26 January 2021

Contents

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

Catalogues[edit]

Zone map[edit]

S/N threshold map[edit]

Noise map[edit]

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

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

Table of source parameter estimates.[edit]

Description of the catalogue columns.[edit]

Position and flux density correction[edit]

Position correction[edit]

Flux density correction[edit]

Spectral Energy Density (SED) plots[edit]

Parameter posterior distributions (‘corner plots’)[edit]

(2015) Planck Catalogue of Galactic Cold Clumps[edit]

(2015) Planck list of high-redshift source candidates[edit]

(2015) Second SZ Catalogue[edit]

Union catalogue[edit]

Individual catalogues[edit]

Selection function[edit]

Previous releases: (2013) PSZ1[edit]

References[edit]

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