Catalogues

Catalogue of Compact Sources

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. The catalogues have been constructed as described in PCCS and in section 2 of Planck-2015-A26. The validation of the catalogues is described in section 3 of Planck-2015-A26.

The PCCS2 is divided into two sub-catalogues in each frequency channel. The main PCCS2 catalogues consist of the sources detected in regions of the sky where it is possible to estimate the reliability of the detections, either statistically or by using external catalogues. Sources detected in regions of the sky where it is not possible to make an estimate of their reliability have been excluded from the main catalogue, but have been made available as the PCCS2E. By definition, the reliability of the 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 8 observations for LFI channels or at least 4 observations for HFI channels. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Tables 1 and 2.

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

PCCS2E in Intensity

Sky distribution of the PCCS2E intensity sources at three different channels: 30 GHz (red circles), 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 at three different channels: 30GHz (red circles), 44GHz (green circles) and 70GHz (blue circles).

Sky distribution of the PCCS2 polarization sources at three different channels: 100GHz (red circles), 143GHz (blue circles) and 217GHz (green circles) and 353 GHz (black).

PCCS2E in Polarization

Sky distribution of the PCCS2E polarization sources at three different channels: 30GHz (red circles), 44GHz (green circles) and 70GHz (blue circles).

Sky distribution of the PCCS2E polarization sources at three different channels: 100GHz (red circles), 143GHz (blue circles) and 217GHz (green circles) and 353 GHz (black).

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	1435	830	1101	1742	2160	2135	1344	1694	4891
PCCS2E	125	104	195	2487	4139	16842	22665	31068	43290
Union PCCS2+PCCS2E	1560	934	1296	4229	6299	18977	24009	32762	48181
Number of sources in the extragalactic zonea.
PCCS2	723	346	441	1742	2160	2135	1344	1694	4891
PCCS2E	22	21	63	0	0	26	289	839	2097
Union PCCS2+PCSS2E	745	367	504	1742	2160	2161	1633	2533	6988
Flux densities [mJy] in the extragalactic zonea .
PCCS2
minimumb	378	621	456	232	147	127	242	535	720
90% completeness	427	692	501	269	177	152	304	555	791
uncertainty	78	127	92	55	35	29	55	105	168
PCCS2E
minimumb	356	494	398	—	—	189	350	597	939
90% completeness	468	708	501	—	—	144	311	557	927
uncertainty	86	134	95	—	—	35	73	144	278

Table 1 Notes

a 30-70 GHz: the extragalactic zone is given by |b| > 30°. 100-857 GHz: outside of galactic region where the reliability cannot be accurately assessed. Note that for the PCCS2E the only sources which occur in this region lie in the filament mask.

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	113	29	33	20	25	11	1
Minimum polarized flux densitya [mJy]	117	181	284	138	148	166	453
Polarized flux density uncertainty [mJy]	46	88	91	30	26	30	81
Minimum polarized flux density completeness 90% [mJy]	199	412	397	135	100	136	347
Minimum polarized flux density completeness 95% [mJy]	251	468	454	160	111	153	399
Minimum polarized flux density completeness 100% [mJy]	600	700	700	250	147	257	426
Number of significantly polarized sources in PCCS2E	9	1	1	43	111	325	666
Minimum polarized flux densitya [mJy]	101	2922	398	121	87	114	348
Polarized flux density uncertainty [mJy]	44	254	116	52	44	55	178
Minimum polarized flux density completeness 90% [mJy]	—	—	—	410	613	270	567
Minimum polarized flux density completeness 95% [mJy]	—	—	—	599	893	464	590
Minimum polarized flux density completeness 100% [mJy]	—	—	—	835	893	786	958

Table 2 Notes

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

Catalogues

The PCCS2 catalogues are contained in the FITS files:

COM_PCCS_030_R2.02.fits

COM_PCCS_044_R2.02.fits

COM_PCCS_070_R2.02.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

and the PCCS2E catalogues are contained in the FITS files:

COM_PCCS_030-excluded_R2.02.fits

COM_PCCS_044-excluded_R2.02.fits

COM_PCCS_070-excluded_R2.02.fits

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	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 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
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 P column is set to NULL; otherwise this column itself contains a NULL.
APER_P_UPPER_LIMIT	Real*4	mJy	Polarization flux density 99.99% upper limit. This is provided only when APER_P column is set to NULL; otherwise this column itself contains a 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 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	degrees	Orientation of polarization with respect to NGP using Bayesian polarization estimator (see note 2)
ANGLE_PX_ERR_LOWER	Real*4	degrees	ANGLE_PX uncertainty; lower 95% error bar
ANGLE_PX_ERR_UPPER	Real*4	degrees	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-degree radius.
SKY_BRIGHTNESS	Real*4	MJy/sr	The mean 857 GHz brightness within a 2-degree radius. This may be used as another indicator of cirrus contamination.
Flux densities at other frequencies (857 GHz only)
APERFLUX_217	Real*4	mJy	Estimated flux density at 217 GHz
APERFLUX_ERR_217	Real*4	mJy	Uncertainty in flux density at 217 GHz
APERFLUX_353	Real*4	mJy	Estimated flux density at 353 GHz
APERFLUX_ERR_353	Real*4	mJy	Uncertainty in flux density at 353 GHz
APERFLUX_545	Real*4	mJy	Estimated flux density at 545 GHz
APERFLUX_ERR_545	Real*4	mJy	Uncertainty in flux density at 545 GHz

Notes

1. Format is PCCS2 fff Glll.ll±bb.bb for sources in the PCCS2 and PCCS2E fff Glll.ll±bb.bb for sources in the PCCS2E, where fff is the frequency channel and (l, b) is the position of the source in Galactic coordinates truncated to two decimal places.
2. We follow the IAU/IEEE convention (Hamaker & Bregman 1996) for defining the angle of polarization of a source, and this convention is also used for the other angles in the catalogue. The angle is measured from the North Galactic Pole in a clockwise direction from -90 to 90 degrees.
3. Provided when the significance of the polarization measurement is > 99.99% and set to NULL otherwise.
4. The P_STAT flag gives the status of the marginal polarization detection, possible values are:

   3 – Bright: P field filled in; all PX fields set to NULL.

   2 – Significant: P field is set to NULL; 0 is outside the PX 95% HPD; all PX fields are filled.

   1 – Marginal: P field is set to NULL; 0 is inside the PX 95% HPD, but mode of PX posterior distribution is not 0; all PX fields are filled.

   0 – No detection: P field is set to NULL; mode of PX posterior distribution is 0; PX_ERRL, ANGLE_PX, ANGLE_PX_ERR_LOWER, and ANGLE_PX_ERR_UPPER are set to NULL.

5. The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criterion for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
6. The EXT_VAL flag gives the status of the external validation, possible values are:

   3 – The source has a clear counterpart in one of the catalogues used as ancillary data.

   2 – The source does not have a clear counterpart in one of the catalogues used as ancillary data but it has been detected by the internal multi-frequency method.

   1 – The source does not have a clear counterpart in one of the catalogues used as ancillary data and it has not been detected by the internal multi-frequency method, but it has been detected in a previous Planck source catalogue.

   0 – The source does not have a clear counterpart in one of the catalogues used as ancillary data and it has not been detected by the internal multi-frequency method.

7. The HIGHEST_RELIABILTY_CAT column contains the highest reliability catalogue to which the source belongs. As the full catalogue reliability is ≥ 80%, this is the lowest possible value in this column. Where possible this is provided in steps of 1% otherwise it is in steps of 5%.
8. The WHICH_ZONE column encodes the zone in which the source lies:

   1 – source lies inside filament mask.

   2 – source lies inside Galactic zone.

   3 – sources lies in both filament mask and Galactic zone.

Zone map

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

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 as follows:

Zone map FITS file structure

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

Notes

1. This FITS extension contains an integer HEALPix map which encodes the information on which of 4 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

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

For 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 as follows:

Zone map FITS file structure

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

Notes

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

Noise map

For each HFI frequency channel there is an associated map which 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 is as follows:

Zone map FITS file structure

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

Notes

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

SZ Catalogue

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

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 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 ratio of the detections, and information on the size and flux of the detections. The entries are cross-referenced to the detections in the union catalogue. The full information on the degeneracy between 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. It is provided in this form so it can be combined with a model or external data to produce tighter constraints on the parameters. The individual catalogues also contain Planck measurements of the SZ mass observable, M_SZ, as calculated using a Y-M scaling relation and an assumed redshift 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 contains 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

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	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 (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 which 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 infrared contamination
Q_NEURAL	Real*4		Neural network quality flag (see note 3)
Y5R500	Real*4	10-3 arcmin2	Mean marginal Y5R500 as determined by reference pipeline
Y5R500_ERR	Real*4	10-3 arcmin2	Uncertainty on Y5R500 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 Msol	SZ mass proxy (see note 6)
MSZ_ERR_UP	Real*4	1014 Msol	Upper bound of 68% SZ mass proxy confidence interval (see note 6)
MSZ_ERR_LOW	Real*4	1014 Msol	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

1. Format is PSZ2 Glll.ll±bb.b where (l,b) are the Galactic coordinates truncated to 2 decimal places.
2. The three least significant decimal digits are used to represent detection or non-detection by the pipelines. Order of the digits: hundreds = MMF1; tens = MMF3; units = PwS. If it is detected then the corresponding digit is set to 1, otherwise it is set to 0.
3. Neural network quality flag is 1-Q_bad, following the definitions in Aghanim et al. 2014.
4. Summary of the external validation, encoding the most robust external identification: 10 = ENO follow-up; 11 = RTT follow-up; 12 = PanSTARRs; 13 = RedMAPPer non-blind; 14 = SDSS high-z; 15 = AMI; 16 = WISE; 20 = legacy identification from the PSZ1; 21 = MCXC; 22 = SPT; 23 = ACT; 24 = RedMAPPer; 25 = legacy identification from PSZ1 with externally updated redshift; 30 = NED; -1 = no known external counterpart.
5. Redshift source is the most robust external identification listed in the VALIDATION field.
6. 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.
7. Assigned by visual inspection: 0 = no significant galaxy overdensity; 1 = possible galaxy overdensity; 2 = probable galaxy overdensity; 3 = significant galaxy overdensity detected; -1 = possible galaxy overdensity (affected by bright star artefacts); -2 = no significant galaxy overdensity (affected by bright star artefacts); -3 = no assessment possible (affected by bright star artefacts); -10 = not analysed.
8. Defined in the paper.

Individual catalogues

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 as follows:

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	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 (95% confidence interval)
SNR	Real*4		Signal-to-noise ratio of detection
TS_MIN	Real*4		Minimum value of θs in grid in second extension HDU (see note 2)
TS_MAX	Real*4		Maximum value of θs 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	Ndet	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	Ndet	Dimension 3 = Number of detections
Keyword	Data Type	Value	Description
PIPELINE	String		Name of detection pipeline

Notes

1. Format PSZ2 Glll.ll±bb.bb where (l, b) are the Galactic coordinates truncated to 2 decimal places.
2. 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.
3. 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_sol. 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:

• HFI_PCCS_SZ-selfunc-union-survey_R2.08.fits (union catalogue, survey mask)
• HFI_PCCS_SZ-selfunc-union-cosmology_R2.08.fits (union catalogue, cosmology mask)
• HFI_PCCS_SZ-selfunc-intersec-survey_R2.08.fits (intersection catalogue, survey mask)
• HFI_PCCS_SZ-selfunc-intersec-cosmolog_R2.08.fits (intersection catalogue, cosmology mask)
• HFI_PCCS_SZ-selfunc-MMF1-survey_R2.08.fits (MMF1 catalogue, survey mask)
• HFI_PCCS_SZ-selfunc-MMF1-cosmolog_R2.08.fits (MMF1 catalogue, cosmology mask)
• HFI_PCCS_SZ-selfunc-MMF3-survey_R2.08.fits (MMF3 catalogue, survey mask)
• HFI_PCCS_SZ-selfunc-MMF3-cosmolog_R2.08.fits (MMF3 catalogue, cosmology mask)
• HFI_PCCS_SZ-selfunc-PwS-survey_R2.08.fits (PowellSnakes catalogue, survey mask)
• HFI_PCCS_SZ-selfunc-PwS-cosmolog_R2.08.fits (PowellSnakes catalogue, cosmology mask)

Their structure is as follows:

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

1. 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 of the survey region have value 0.0.
2. Extension 2 contains a three-dimensional image containing the survey completeness probability distribution for various S/N thresholds. The information is stored in an image of size 30 × 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 percent and lie in the range 0-100 and denote the detection probability of a cluster in the given (Y₅₀₀, θ₅₀₀) bin.
3. 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.
4. 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.
5. 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.

Catalogue of Planck Galactic Cold Clumps

The catalogue of Planck Galactic Cold Clumps (PGCC) is a list of 13188 Galactic sources and 54 sources located in the Small and Large Magellanic Clouds. The sources have been identified in Planck data as sources colder than their environment. It has been buit using the 48 months Planck data at 857, 545, and 353 GHz combined with the 3 THz IRAS data, as it is described in Planck-2015-A28.

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

All-sky distribution of the PGCC sources.

Sources are divided into three categories based on the reliability of the flux density estimates in IRAS 3 THz and Planck 857, 545, and 353 GHz bands.

• FLUX_QUALITY=1 : sources with flux density estimates S/N > 1 in all bands ;
• FLUX_QUALITY=2 : sources with flux density estimates S/N > 1 only in 857, 545, and 353 GHz Planck bands, considered as very cold source candidates ;
• FLUX_QUALITY=3 : sources without any reliable flux density estimates, listed as poor candidates.

The all-sky distributions of the PGCC sources per FLUX_QUALITY category are shown below on top of the 857 GHz map in grey scale shown in logarithmic scale between 10^-2 to 10² MJy/sr.

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 on 5574 PGCC sources using seven different methods/technics, as described in Planck-2015-A28. A flag is raised 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[math]\sigma[/math] ;
• DIST_QUALITY=3 : Multiple distance estimates which are not consistent within 1[math]\sigma[/math] ;
• DIST_QUALITY=4 : Single upper limits.

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

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. It structure is as follows:

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	1[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] 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	1[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] 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 3000 GHz 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	1[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] uncertainty on the distance estimate [3] using optical extinction on SDSS DR9
DIST_NIR_EXT_IRDC	real*8	kpc	Distance estimate [4] using near-infrared extinction towards IRDCs
DIST_NIR_EXT_IRDC_SIG	real*8	kpc	1[math]\sigma[/math] uncertainty on the distance estimate [4] using near-infrared extinction towards IRDCs
DIST_NIR_EXT	real*8	kpc	Distance estimate [5] using near-infrared extinction
DIST_NIR_EXT_SIG	real*8	kpc	1[math]\sigma[/math] uncertainty on the distance estimate [5] using near-infrared extinction
DIST_MOLECULAR_COMPLEX	real*8	kpc	Distance estimate [6] using molecular complex association
DIST_MOLECULAR_COMPLEX_SIG	real*8	kpc	1[math]\sigma[/math] 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[math]\sigma[/math] 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[math]\sigma[/math] uncertainty on the best distance estimate
Temperature
FITS Keyword	Data Type	Units	Description
TEMP_CLUMP	real*8	K	Temperature of the clump with [math]\beta[/math] as a free parameter
TEMP_CLUMP_SIG	real*8	K	1[math]\sigma[/math] uncertainty on the clump temperature with [math]\beta[/math] free
TEMP_CLUMP_LOW1	real*8	K	Lower 68% confidence limit of the clump temperature with [math]\beta[/math] free
TEMP_CLUMP_UP1	real*8	K	Upper 68% confidence limit of the clump temperature with [math]\beta[/math] free
BETA_CLUMP	real*8		Spectral index [math]\beta[/math] of the clump
BETA_CLUMP_SIG	real*8		1[math]\sigma[/math] uncertainty (from MCMC) on the emissivity spectral index [math]\beta[/math] of the clump
BETA_CLUMP_LOW1	real*8		Lower 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the clump
BETA_CLUMP_UP1	real*8		Upper 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the clump
TEMP_BETA2_CLUMP	real*8	K	Temperature of the clump with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_SIG	real*8	K	1[math]\sigma[/math] uncertainty on the temperature of the clump with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_LOW1	real*8	K	Lower 68% confidence limit of the clump temperature with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_UP1	real*8	K	Upper 68% confidence limit of the clump temperature with [math]\beta[/math] = 2
TEMP_WBKG	real*8	K	Temperature of the warm background with [math]\beta[/math] as a free parameter (see note 6)
TEMP_WBKG_SIG	real*8	K	1[math]\sigma[/math] dispersion of the warm background temperature with [math]\beta[/math] free
TEMP_WBKG_LOW1	real*8	K	Lower 68% confidence limit of the warm background temperature with [math]\beta[/math] free
TEMP_WBKG_UP1	real*8	K	Upper 68% confidence limit of the warm background temperature with [math]\beta[/math] free
BETA_WBKG	real*8		Spectral index [math]\beta[/math] of the warm background (see note 6)
BETA_WBKG_SIG	real*8		1[math]\sigma[/math] uncertainty (from MCMC) of the emissivity spectral index [math]\beta[/math] of the warm background
BETA_WBKG_LOW1	real*8		Lower 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the warm background
BETA_WBKG_UP1	real*8		Upper 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the warm background
TEMP_BETA2_WBKG	real*8	K	Temperature of the warm background with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_SIG	real*8	K	1[math]\sigma[/math] uncertainty on the temperature of the warm background with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_LOW1	real*8	K	Lower 68% confidence limit of the warm background temperature with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_UP1	real*8	K	Upper 68% confidence limit of the warm background temperature with [math]\beta[/math] = 2
Physical properties
FITS Keyword	Data Type	Units	Description
NH2	real*8	cm-2	Column density [math]N_{H_2}[/math] of the clump
NH2_SIG	real*8	cm-2	1[math]\sigma[/math] 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	[math]M_{o}[/math]	Mass estimate of the clump
MASS_SIG	real*8	[math]M_{o}[/math]	1[math]\sigma[/math] uncertainty on the mass estimate of the clump
MASS_LOW[1,2,3]	real*8	[math]M_{o}[/math]	Lower 68%, 95% and 99% confidence limit of the mass estimate
MASS_UP[1,2,3]	real*8	[math]M_{0}[/math]	Upper 68%, 95% and 99% confidence limit of the mass estimate
DENSITY	real*8	cm-3	Mean density of the clump
DENSITY_SIG	real*8	cm-3	1[math]\sigma[/math] 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	1[math]\sigma[/math] uncertainty on the physical size estimate of the clump
SIZE_LOW[1,2,3]	real*8	pc	Lower 68%, 95% and 99% confidence limit of the physical size estimate
SIZE_UP[1,2,3]	real*8	pc	Upper 68%, 95% and 99% confidence limit of the physical size estimate
LUMINOSITY	real*8	Lo	Luminosity of the clump
LUMINOSITY_SIG	real*8	Lo	1[math]\sigma[/math] uncertainty on the luminosity estimate of the clump
LUMINOSITY_LOW[1,2,3]	real*8	Lo	Lower 68%, 95% and 99% confidence limit of the luminosity estimate
LUMINOSITY_UP[1,2,3]	real*8	Lo	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, counted clockwise.
• 2: The warm bakcground flux densities are computed using the same solid angle as for the clumps flux densities, but on the warm conponent map.
• 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 on the clumpds flux densities to get a corrected estimate. It has been obtained on a very simple modelling of clumps morphology and the local environment. It has therefore to be taken very carefully.
• 5: See text above for a full description of the DIST_QUALITY flag.
• 6: Temperature and spectral index of the warm background are based on the warm background flux density estimates obtained on the same solid angle used for clumps