Catalogues

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Catalogue of Compact Sources[edit]

Product description[edit]

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 [1].

Production process[edit]

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

Inputs[edit]

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:

Catalogues[edit]

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[edit]

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[edit]

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[edit]

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[edit]

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

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[2].

The union catalogue contains the coordinates and the signal-to-noise ratio of the detections and a summary of the external validation information, including external identification of a cluster and its redshift if it is available.

The individual catalogues contain the coordinates and the signal-to-noise ratio of the detections, and information on the size and flux of the detections. The entries are cross-referenced to the detections in the union catalogue.

The size of a detection is given in terms of the scale size, $\theta_\mathrm{s}$, 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 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.


Union Catalogue[edit]

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 $\alpha$ parameter.
PP_BETA Real*4 GNFW pressure profile $\beta$ parameter.
PP_GAMMA Real*4 GNFW pressure profile $\gamma$ parameter.
PP_C500 Real*4 GNFW pressure profile $c_{500}$ parameter.
PP_Y2YFH Real*4 Conversion factor from $Y$ to $Y_{500}$.
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

  1. format is PSZ1 Glll.ll+mn;bb.b where (l,b) are the Galactic and 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. values are: 1 = candidate of class 1; 2 = candidate of class 2; 3 = candidate of class 3; 10 = Planck cluster confirmed by follow-up; 20 = known cluster.
  4. 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[edit]

The individual pipeline catalogues are contained in the FITS files

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 $\alpha$ parameter.
PP_BETA Real*4 GNFW pressure profile $\beta$ parameter.
PP_GAMMA Real*4 GNFW pressure profile $\gamma$ parameter.
PP_C500 Real*4 GNFW pressure profile $c_{500}$ parameter.
PP_Y2YFH Real*4 Conversion factor from $Y$ to $Y_{500}$.
Ext. 1: EXTNANE = PSZ_INDIVIDUAL (BINTABLE)
Column Name Data Type Units Description
INDEX Int*4 Index from union catalogue.
NAME String Source name - see Note1
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.
SNR_COMPAT Real*4 SNR 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_MAX Real*4 Maximum value of $\theta_\mathrm{s}$ 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

  1. Format PSZ1 Glll.ll±bb.bb where (l, b) are the Galactic coordinates truncated to 2 decimal places.
  2. 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.
  3. 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 × 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 $\theta_\mathrm{s}$ and the second dimension is $Y$.

Mask[edit]

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[edit]

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[2]). 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

  1. 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.
  2. 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.
  3. 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.
  4. Source for redshifts:
    -1 : No redshift available
     1 : MCXC updated compilation[3]
     2 : Databases NED and SIMBAD-CDS
     3 : SDSS cluster catalogue[4]
     4 : SDSS cluster catalogue[5]
     5 : SPT[6][7][8][9][10][11][12]
     6 : ACT[13][14][15][16]
     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[edit]

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.

Galactic Cold Core Catalogue[edit]

TBW - Montier

Catalogue of High-Redshift Sources[edit]

TBW - Montier

References[edit]

  1. ↑
  2. ↑ 2.02.12.2 Planck 2013 results. XXIX. The Planck Catalogue of Sunyaev-Zeldovich sources, Planck Collaboration, 2014, A&A, 571, A29.
  3. ↑ 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).
  4. ↑ 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).
  5. ↑ 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).
  6. ↑ 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).
  7. ↑ 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).
  8. ↑ 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).
  9. ↑ 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).
  10. ↑ 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).
  11. ↑ 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).
  12. ↑ 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).
  13. ↑ 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).
  14. ↑ 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).
  15. ↑ 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).
  16. ↑ 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).

Early Release Compact Source Catalog

(Planck) Low Frequency Instrument

(Planck) High Frequency Instrument

Flexible Image Transfer Specification

Data Processing Center

Full-Width-at-Half-Maximum

(Hierarchical Equal Area isoLatitude Pixelation of a sphere, <ref name="Template:Gorski2005">HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere, K. M. Górski, E. Hivon, A. J. Banday, B. D. Wandelt, F. K. Hansen, M. Reinecke, M. Bartelmann, ApJ, 622, 759-771, (2005).

Sunyaev-Zel'dovich

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