Catalogues

Catalogue of Compact Sources

Product description

The second version of the Planck Catalogue of Compact Sources (PCCS2 and PCCS2E) is a set of single-frequency lists of sources extracted from the Planck full-mission maps in intensity and polarization.

The main difference between the PCCS2 and PCCS2E is that the sources in the PCCS2 have been validated, either statistically or by using external catalogues, while the PCCS2E contains the remaining sources for which it has not been possible to estimate their reliability. 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%).

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.

The deeper completeness levels and, as a consequence, the higher number of sources compared with its predecessors the PCCS and the ERCSC, allows the extension of previous studies to more sources and to fainter flux densities.

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.

Before using the PCCS2, please read the cautionary notes in the paper .

Production process

For a description of the production and validation process of the PCCS2 see the corresponding section.

Inputs

The nine Planck 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. This implies that 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 5 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 input data used to generate this product are the following:

• Full-mission frequency maps
• RIMO
• Effective beams

Catalogues

The PCCS2 catalogues are contained in the FITS files:

COM_PCCS_030_R2.30.fits

COM_PCCS_044_R2.30.fits

COM_PCCS_070_R2.30.fits

COM_PCCS_100_R2.20.fits

COM_PCCS_143_R2.20.fits

COM_PCCS_217_R2.20.fits

COM_PCCS_353_R2.20.fits

COM_PCCS_545_R2.20.fits

COM_PCCS_857_R2.20.fits

and the PCCS2E catalogues are contained in the FITS files:

COM_PCCSE_030_R2.30.fits

COM_PCCSE_044_R2.30.fits

COM_PCCSE_070_R2.30.fits

COM_PCCSE_100_R2.20.fits

COM_PCCSE_143_R2.20.fits

COM_PCCSE_217_R2.20.fits

COM_PCCSE_353_R2.20.fits

COM_PCCSE_545_R2.20.fits

COM_PCCSE_857_R2.20.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		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 beam
OMEGA_B	Real*4	arcmin2	Area of the main 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)
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
Polarization Measurements (30-353 GHz only)
P	Real*4	mJy	Polarization flux density of the sources as determined by a matched filter (Note 4)
P_ERR	Real*4	mJy	Uncertainty (1 sigma) in derived polarization flux density (Note 4)
ANGLE_P	Real*4	degrees	Orientation of polarization with respect to NGP (Notes 4 and 5)
ANGLE_P_ERR	Real*4	degrees	Uncertainty (1 sigma) in orientation of polarization (Note 4)
APER_P	Real*4	mJy	Polarization flux density of the sources as determined by aperture photometry (Note 4)
APER_P_ERR	Real*4	mJy	Uncertainty (1 sigma) in derived polarization flux density (Note 4)
APER_ANGLE_P	Real*4	degrees	Orientation of polarization with respect to NGP (Notes 4 and 5)
APER_ANGLE_P_ERR	Real*4	degrees	Uncertainty (1 sigma) in orientation of polarization (Note 4)
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)
P_STAT	Integer*2		Polarization detection status (Note 6)
PX	Real*4	mJy	Polarization flux density of the sources as determined by a matched filter; Bayesian polarization estimator (Note 6)
PX_ERR_LOWER	Real*4	mJy	PX uncertainty; lower 95% error bar (Note 6)
PX_ERR_UPPER	Real*4	mJy	PX uncertainty; upper 95% error bar (Note 6)
ANGLE_PX	Real*4	degrees	Orientation of polarization with respect to NGP; Bayesian polarization estimator (Notes 5 and 6)
ANGLE_PX_ERR_LOWER	Real*4	degrees	ANGLE_PX uncertainty; lower 95% error bar (Note 6)
ANGLE_PX_ERR_UPPER	Real*4	degrees	ANGLE_PX uncertainty; upper 95% error bar (Note 6)
Flags and validation
EXTENDED	Integer*2		Extended source flag (Note 2)
EXT_VAL	Integer*2		External validation flag (Note 3)
ERCSC	String		Name of the ERCSC counterpart, if any
PCCS	String		Name of the PCCS counterpart, if any
HIGHEST_RELIABILITY_CAT	Integer*4		See Note 8
Flags and validation (100-857 GHz only)
WHICH_ZONE	Integer*2		See Note 7
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. Source names consist of a prefix and a position. The prefix used is PCCS2 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 map would be labelled PCCS2 545 G120.23+04.23.
2. The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criteria for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
3. The EXT_VAL flag takes the value of 0, 1, 2, or 3 based on the following conditions:

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

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

4. Provided when the significance of the polarization measurement is > 99.99% and set to NULL otherwise.
5. We follow the IAU/IEEE convention (Hamaker & Bregman 1996) for defining the angle of polarization of a source. The polarization angle is measured from the North Galactic Pole in a clockwise direction from -90 to 90 degrees.
6. The PX fields are only available for the 100-353 GHz channels. All PX fields contain NULL each time a bright detection is found and the P field contains a value different from 0.

   Polarization detection status (P_STAT):

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

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

   1 – Marginal. P field set to NULL; 0 is inside of the PX 95% HPD, but mode of PX posterior distribution is different from 0; All PX fields are filled.

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

7. 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). NOTE: this column is only present when the version keyword in the primary header is set to PCCS2_E.
8. 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%. NOTE: this column is only present when the version keyword in the primary header is set to PCCS2.

Zone map

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

The files are called:

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
NSIDE	Integer		Nside of HEALPix map
ORDERING	String		Ordering of pixels
FREQ_CHL	String		Frequency channel

The FITS extension contains an integer HEALPix map which encodes the information of the 4 possible regions on the sky (0 – quantified-reliability zone, 1 – filament mask, 2 – galactic zone, 3 – filament mask and galactic zone).

S/N threshold map

For each HFI frequency channel there is an associated map which contains the S/N threshold used to accept sources into the PCCS2 and PCCS2E catalogues.

The files are called:

The structure of the files is as follows:

S/N threshold map FITS file structure

Extension 0: Primary header, no data
FITS Keyword	Data Type	Units	Description
NSIDE	Integer		Nside of HEALPix map
ORDERING	String		Ordering of pixels
FREQ_CHL	String		Frequency channel

The 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:

The structure of the files is as follows:

Noise map FITS file structure

Extension 0: Primary header, no data
FITS Keyword	Data Type	Units	Description
NSIDE	Integer		Nside of HEALPix map
ORDERING	String		Ordering of pixels
FREQ_CHL	String		Frequency channel

The FITS extension contains a single precision HEALPix map of the detection noise at each location on the sky.

SZ Catalogue

The Planck SZ catalogue is constructed as described in SZ catalogue and in section 2 of . 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 sections 3-6 of .

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 67% 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_R2.07.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; 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); -10 no assessment possible (affected by bright star artefacts).
8. Defined in the paper.

Individual catalogues

The individual pipeline catalogues are contained in the FITS files

• HFI_PCCS_SZ-MMF1_R2.07.fits (Matched Multi-Filter method #1)
• HFI_PCCS_SZ-MMF3_R2.07.fits (Matched Multi-Filter method #3)
• HFI_PCCS_SZ-PwS_R2.07.fits (Powell Snakes method)

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: EXTNAME = PSZ2_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	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: EXTNAME = PSZ2_PROBABILITY (IMAGE) – 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: EXTNAME = PSZ2_MSZ_ARRAY (IMAGE) – 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 PSZ1 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.

Galactic Cold Core Catalogue

TBW - Montier

Catalogue of High-Redshift Sources

TBW - Montier