Difference between revisions of "Catalogues"

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==Planck Catalogue of Compact Sources==
+
==The Catalogue of Compact Sources==
−
The Planck Catalogue of Compact Sources (PCCS) is a sample of reliable sources, both Galactic and extragalactic, extracted directly from the Planck nominal maps. The first public version of the PCCS is derived from the data acquired by Planck between August 13 2009 and November 26 2010. The PCCS consists of nine lists of sources, extracted independently from each of Planck's nine frequency channels. It is fully described in <span style="color:red">[reference to the Planck Cosmology and Product Paper 05a]</span>.
 
  
−
The whole PCCS can be downloaded here [http://www.sciops.esa.int/index.php?project=planck&page=Planck_Legacy_Archive].
 
  
−
=== Detection procedure ===
+
===Product description===
−
The Mexican Hat Wavelet 2 (MHW2; Gonzalez-Nuevo et al., 2006) is the base algorithm used to produce the single channel catalogues of the PCCS. Although each DPC has is own implementation of this algorithm (IFCAMEX and HFI-MHW), the results are compatible at least at the statistical uncertainty level. Additional algorithms are also implemented, like the multi-frequency Matrix Multi-filters (MTXF; Herranz et al., 2009) and the Bayesian PowellSnake (Carvalho et al. 2009), but for the current version of the PCCS they are used just for the validation of the results obtained by the MHW2.
 
  
−
The full-sky maps are divided into a sufficient number of overlapping flat patches in such a way that 100% of the sky is covered. Each patch is then filtered by the MHW2 with a scale that is optimised to provide the maximum signal-to-noise ratio in the filtered maps. A sub-catalogue of objects is produced for each patch and then, at the end of the process, all the sub-catalogues are merged together, removing repetitions. For each channel, a parent sample is created containing all the sources detected with a signal-to-noise greater than 4. These 9 lists, that contain the positions, native flux densities and errors, are used as inputs in the validation step. The results of the validation process are finally used to decided the final thresholding or removal of spurious sources, defining the final PCCS.  
+
[[File:PCCS_skydist.png|400px|thumb|right|Sky distribution of the PCCS sources at three different channels: 30GHz (pink circles), 143GHz (magenta circles) and
 +
857GHz (green circles). The dimension of the circles is related to the brightness of the sources and the beam size of each channel.]]
  
−
=== Photometries ===
+
The PCCS is a set of nine single-frequencies lists of sources extracted from the Planck nominal mission data. By definition its reliability is > 80% and a special effort was made to use simple selection procedures in order to facilitate statistical analyses. With a common detection method for all the channels and the additional three photometries, spectral analysis can also be done safely. The deeper completeness levels and, as a consequence, the higher number of sources compared with its predecessor the ERCSC, will allow the extension of previous studies to more sources and to fainter flux densities. The PCCS is the natural evolution of the ERCSC, but both lack polarization and multi-frequency information. Future releases will take advantage of the full mission data and they will contain information on properties of sources not available in this release, such as polarization, multi-frequency and variability.
−
In addition of the native flux density estimation provided by the detection algorithm, three additional measurements are obtained for each of the source in the parent samples.
 
−
These additional flux density estimations are based on aperture photometry, PSF fitting and Gaussian fitting (see <span style="color:red">[reference to the Planck Cosmology and Product Paper 05a]</span> for a detailed description of these additional photometries). The native flux density estimation is the only one that is obtained directly from the filtered maps while for the others the flux density estimates has a local background subtracted. The flux density estimations have not been colour corrected. Colour corrections are available in <span style="color:red">[reference to the Color Correction description or Planck Cosmology and Product Paper 05a]</span>.
 
  
−
=== Validation process ===
 
−
The parent sample lists constitute only the starting point for the validation process. The results of the validation (both internal and external depending on the kind of information used) determine the final selection of sources to be included in the PCCS.
 
  
−
==== Internal validation ====
+
{| border="1" cellpadding="3" cellspacing="0" align="center" width=750px
−
The PCCS is validated through an internal Monte-Carlo quality assessment (MCQA) process that uses large numbers of source injection and detection loops on realistic simulated maps to constrain detection characteristics.
+
|+ '''Table 1: PCCS characteristics'''
 +
|- bgcolor="ffdead" 
 +
! Channel || 30 || 44 || 70 || 100 || 143 || 217 || 353 || 545 || 857
 +
|-
 +
| '''Frequency [GHz]''' || 28.4 || 44.1 || 70.4 || 100.0 || 143.0 || 217.0 || 353.0 || 545.0 || 857.0
 +
|-
 +
| '''Beam FWHM<span style="color:red"><sup>1</sup></span> [arcmin]''' || 32.38 || 27.10 || 13.30 || 9.88 || 7.18 || 4.87 || 4.65 || 4.72 || 4.39
 +
|-
 +
|'''SNR threshold''' || 4.0 || 4.0 || 4.0 || 4.6 || 4.7 || 4.8 || 4.9<span style="color:red"><sup>2</sup></span>/6.0<span style="color:red"><sup>3</sup></span> || 4.7/7.0 || 4.9/7.0
 +
|-
 +
| '''# of detections''' || 1256 || 731 || 939 || 3850 || 5675 || 16070 || 17689 || 26472 || 35719
 +
|-
 +
|| '''#  of detections for |b| > 30º)''' || 572 || 258 || 332 || 845 || 1051 || 1901 || 2035 || 4164 || 7851
 +
|-
 +
| '''Flux density uncertainty [mJy] || 109 || 198 || 149 || 61 || 38 || 35 || 74 || 132 || 189
 +
|-
 +
| '''Min flux density<span style="color:red"><sup>4</sup></span> [mJy]''' || 461 || 825 || 566 || 266 || 169 || 149 || 298 || 479 || 671
 +
|-
 +
| '''90% completeness [mJ]''' || 575 || 1047 || 776 || 300 || 190 || 180 || 330 || 570 || 680
 +
|-
 +
| '''Position uncertainty<span style="color:red"><sup>5</sup></span> [arcmin]''' || 1.8 || 2.1 || 1.4 || 1.0 || 0.7 || 0.7 || 0.8 || 0.5 || 0.4
 +
|-
 +
|}
  
−
Source injection consists on the introduction of fake sources in the real maps. The positions of the injected sources are chosen in order to avoid existing detections in the real maps and previously injected sources. By analysing the recovered injected sources we can determine several statistical properties of the detection process: completeness, photometry accuracy, variation of sensitivity along the sky, etc.
 
  
−
On the other hand, in order to study the number of false detections, also known as Purity, we need to perform realistic all-sky simulations. <span style="color:red">[Description or reference of the simulation used]</span>.  
+
'''Notes'''
 +
# The Planck beams are described in {{PlanckPapers|planck2013-p02d}} and {{PlanckPapers|planck2013-p03c}}. This table shows the values which were adopted for the PCCS (derived from the effective beams).
 +
# In the extragalactic zone (48% of the sky; see Fig. 2 in {{PlanckPapers|planck2013-p05}}).
 +
# In the Galactic zone (52% of the sky; see Fig. 2 in {{PlanckPapers|planck2013-p05}}).
 +
# Minimum flux density of the catalogue at |b| > 30º after excluding the 10% faintest sources.<br>
 +
# Positional uncertainty derived by comparison with PACO sample ({{BibCite|PATCABright}}{{BibCite|PATCAfaint}}{{BibCite|PATCASpec}}) up to 353 GHz and with Herschel samples (HRS, KINGFISH, HeViCS, H-ATLAS) in the other channels.
  
−
This statistical characterization of the detection process is used to choose the best signal-to-noise threshold for each channel in order to maximize the Completeness without penalizing the Purity.
+
Before using the PCCS, please read the Cautionary Notes in the PCCS general description [[Compact Source catalogues|section]]. For full details, see paper {{PlanckPapers|planck2013-p05}}.
  
−
==== External validation ====
+
===Production process===
  
 +
For a description of the production and validation processes of the PCCS see the corresponding [[Compact Source catalogues|section]].
  
−
=== Cautionary notes ===
+
===Inputs===
−
* Statistical Character : warnings about the statistical analysis of this catalogue... Completeness levels for statistical analysis as number counts, usage of sensitivity maps at fixed completeness level, etc
 
  
−
* Variability: At radio frequencies, many of the extragalactic sources are highly variable. A small fraction of them vary even on time scales of a few hours based on the brightness of the same source as it passes through the different Planck horns (refs?). Follow-up observations of these sources might show significant differences in flux density compared to the values in the data products. Although the maps used for the PCCS are based on ~2.5 sky coverages, the current version of the PCCS provides only a single average flux density estimate over all Planck data samples that were included in the all sky maps and does not contain any measure of the variability of the sources.  
+
The data obtained from the Planck nominal mission between (2009 August 12 and 2010 November 27) have been processed into full-sky maps by the HFI and LFI Data Processing Centres (DPCs). A description of the processing can be found in {{PlanckPapers|planck2013-p02}} and {{PlanckPapers|planck2013-p03}}. The data consist of two complete sky surveys and 60% of the third survey. This implies that the flux densities of sources obtained from the nominal mission maps are the average of at least two observations. The nine Planck frequency channel maps are used as input to the source detection pipelines. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Table 1.
  
−
* Contamination from CO: At infrared/submillimetre frequencies (100GHz and above), the Planck bandpasses straddle energetically significant CO lines (refs?). The effect is the most significant at 100GHz, where the line might contribute more than 50% of the measured flux density. Follow-up observations of these sources, especially those associated with Galactic star-forming regions, at a similar frequency but different bandpass, should correct for the potential contribution of line emission to the continuum flux density of the source. See Planck HFI Core Team (2011b) for details.
+
The input data used to generate this product are the following:
  
−
* Photometry: Each source has multiple measures of photometry APERFLUX, GAUFLUX, PSFFLUX and FLUXDET (or native) as defined above. The appropriate photometry to be used depends on the nature of the source. For sources which are unresolved at the spatial resolution of Planck, APERFLUX and FLUXDET are most appropriate. Even in this regime, PSF fits of faint sources fail and consequently these have a PSFFLUX value of NaN (Not a Number). For bright resolved sources, GAUSFLUX might be most appropriate although GAUSFLUX appears to overestimate the flux of sources close to the Galactic plane due to an inability to fit for the contribution of the Galactic background at the spatial resolution of the data.
+
* [[Frequency Maps | nominal survey, full channel sky maps]]
 +
* [[The RIMO | RIMO]]
 +
* [[Effective Beams | effective beams]]
  
−
* Cirrus/ISM: A significant fraction of the sources detected in the upper HFI bands could be associated with Galactic interstellar medium features or cirrus. The IRAS 100μm surface brightness in MJy sr1 for each of the sources, which is commonly used as a proxy for cirrus, is available through a search of the ERCSC with IRSA. Candidate ISM features can also be selected by choosing objects with EXTENDED=1 although nearby Galactic and extragalactic sources which are extended at Planck spatial resolution will meet this criterion. Alternately, the value of CIRRUS in the catalogue can be utilised to flag sources which might be clustered together and thereby associated with ISM structure.
+
===Related products===
  
−
==Planck SZ Cluster Catalogue==
+
Other products that are related and share some commonalities with the product being described here are the other catalogues:
−
The Planck SZ Cluster Catalogue is a nearly full-sky list of highly-reliable SZ clusters detected in the Planck data. It is fully described in <span style="color:red">[reference to the Planck Cosmology and Product Paper 05a]</span>. The catalogue is derived from the HFI frequency channel maps after masking and filling the bright point sources (SNR >= 10) from the general PCCS catalogue in those channels. Three detection methods were used to construct the catalogue: two implementations of the Matched Multi-Filter (MMF) algorithm and PowellSnakes (PwS), a Bayesian algorithm. A Galactic dust mask (leaving 85% of the sky) and a point source mask is applied a posteriori to remove detections in the portion of the sky where foregrounds are likely to cause spurious detections.
+
# [[Catalogues#The ERCSC | ERCSC]]
 +
# [[Catalogues#The SZ catalogues | SZ catalogue]]
 +
 
 +
===File names===
 +
 
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_030_R1.30.fits|link=COM_PCCS_030_R1.30.fits}}
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_044_R1.30.fits|link=COM_PCCS_044_R1.30.fits}}
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_070_R1.30.fits|link=COM_PCCS_070_R1.30.fits}}
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_100_R1.20.fits|link=COM_PCCS_100_R1.20.fits}}
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_143_R1.20.fits|link=COM_PCCS_143_R1.20.fits}}
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_217_R1.20.fits|link=COM_PCCS_217_R1.20.fits}}
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_353_R1.20.fits|link=COM_PCCS_353_R1.20.fits}}
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_545_R1.20.fits|link=COM_PCCS_545_R1.20.fits}}
 +
: {{PLASingleFile|fileType=cat|name=COM_PCCS_857_R1.20.fits|link=COM_PCCS_857_R1.20.fits}}
 +
 
 +
===Meta Data ===
 +
 
 +
The PCCS source list in each frequency is structured as a FITS binary table having one row for each detected source. The details of the FITS file structure are below
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" width=800px style="text-align:left"
 +
|+ '''FITS file structure'''
 +
|- bgcolor="ffdead" 
 +
!colspan="4" | Extension 0: Primary header, no data
 +
|- bgcolor="ffdead"
 +
! FITS Keyword || Data Type || Units || Description
 +
|-
 +
|INSTRUME || String || || LFI or HFI
 +
|-
 +
| VERSION || String || || Version of PCCS
 +
|-
 +
| DATE || String || || Date file created:yyyy-mm-dd
 +
|-
 +
| ORIGIN || String || || Name of organization responsible for the data (LFI-DPC – HFI-DPC)
 +
|-
 +
| TELESCOP || String || || PLANCK
 +
|-
 +
| CREATOR || String || || Pipeline Version
 +
|-
 +
| DATE-OBS || String || days || Start-up time of the survey: yyyy-mm-dd
 +
|-
 +
| DATE-END || String || days || Ending time of the survey: yyyy-mm-dd
 +
|- bgcolor="ffdead" 
 +
!colspan="4" | Extension 1:  (BINTABLE)
 +
|-bgcolor="ffdead"
 +
! Column Name || Data Type || Units || Description
 +
|-bgcolor="ffdead"
 +
!colspan="4"|Identification
 +
|-
 +
|NAME || String || || Source name (Note 1)
 +
|-bgcolor="ffdead"
 +
!colspan="4"|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)
 +
|-bgcolor="ffdead"
 +
!colspan="4"|Photometry
 +
|-
 +
|DETFLUX || Real*4 || mJy || Flux density of source as determined by detection method
 +
|-
 +
|DETFLUX_ERR || Real*4 || mJy || Uncertainty (1 sigma) in derived flux density from detection method
 +
|-
 +
|APERFLUX || Real*4 || mJy || Flux density of source as determined from 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
 +
|-bgcolor="ffdead"
 +
!colspan="4"|Flags and validation
 +
|-
 +
|EXTENDED || Integer*2 || || Extended source flag (Note 2)
 +
|-
 +
|CIRRUS_N || Integer*2 || || Number of sources detected at 857 GHz within 1 degree
 +
|-
 +
|EXT_VAL || Integer*2 || || External validation flag (Note 3)
 +
|-
 +
|ERCSC || String || || Name of the ERCSC counterpart if any
 +
|-bgcolor="ffdead"
 +
!colspan="4"|ONLY 857 GHz Catalogue
 +
|-
 +
|APERFLUX_217 || Real*4 || mJy || Estimated flux density at 217 GHz
 +
|-
 +
|APERFLUX_ERR_217 || Real*4 || mJy || Uncertainty in source flux density at 217 GHz
 +
|-
 +
|APERFLUX_353 || Real*4 || mJy || Estimated flux density at 353 GHz
 +
|-
 +
|APERFLUX_ERR_353 || Real*4 || mJy || Uncertainty in source flux density at 353 GHz
 +
|-
 +
|APERFLUX_545 || Real*4 || mJy || Estimated flux density at 545 GHz
 +
|-
 +
|APERFLUX_ERR_545 || Real*4 || mJy || Uncertainty in source flux density at 545 GHz
 +
|}
 +
 
 +
 
 +
'''Notes'''
 +
# Source names consist of a prefix and a position. The prefix used is PCCS1 fff for the catalogue at fff GHz. The position is in Galactic coordinates and specified as "Glll.ll±bb.bb" where the (l,b) values are truncated to two decimal places. For example, a source detected at (l,b) = (120.237, 4.231) in the 545 GHz Planck map would be labelled PCCS1 545 G120.23±04.23.
 +
# The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criteria for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
 +
# The EXT_VAL flag takes the value of 0, 1, or 2, based on the following conditions:
 +
#: = 2: The source has a clear counterpart in one of the catalogues considered as ancillary data.
 +
#: = 1: The source has no clear counterpart in one of the ancillary catalogues but it has been detected by the internal multi-frequency method (LFI channels) or match with neighbouring frequencies, above or below (HFI channels).
 +
#: = 0: The source has no clear counterpart in one of the ancillary catalogues and it has not been detected by the internal multi-frequency method or neighbouring frequencies.
 +
# The x-axis is defined for each source as parallel to the line of constant colatitude, with the same direction as the longitude. Therefore the position angles are measured anticlockwise from the y-axis.
 +
 
 +
== The SZ catalogues ==
 +
 
 +
 
 +
The Planck SZ catalogue is constructed as described in [[Compact_Source_catalogues#Planck_Sunyaev-Zeldovich_catalogue|SZ catalogue]] and in section 2 of {{PlanckPapers|planck2013-p05a}}.
 +
 
 +
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 {{PlanckPapers|planck2013-p05a}}.
 +
 
 +
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.
  
−
The master catalogue contains the merger of the catalogues from the three detection methods. The individual catalogues are also provided for the expert user in order to assess the consistency of the methods. The completeness and reliability of the catalogues have been assessed through internal and external validation. The catalogue has a reliability of 85% (TBC).
 
 
   
 
   
−
==Early Release Compact Source Catalogue==
+
====Union Catalogue====
−
The ERCSC is a list of high reliability (>90%) sources, both Galactic and extragalactic, derived from the data acquired by Planck between August 13 2009 and June 6 2010. The ERCSC consists of:
 
  
−
* nine lists of sources, extracted independently from each of Planck's nine frequency channels
+
The union catalogue is contained in  ''{{PLASingleFile|fileType=cat | name=COM_PCCS_SZ-union_R1.12.fits | link=COM_PCCS_SZ-union_R1.12.fits}}''.
  
−
* two lists extracted using multi-channel criteria: the Early Cold Cores catalogue (ECC), consisting of Galactic dense and cold cores, selected mainly on the basis of their temperature ; and the Early Sunyaev-Zeldovich catalogue (ESZ), consisting of galaxy clusters selected by the spectral signature of the Sunyaev-Zeldovich effect.
 
  
−
The whole ERCSC can be downloaded here [http://www.sciops.esa.int/index.php?project=PLANCK&page=Planck_Data_Products].
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|- bgcolor="ffdead" 
 +
!colspan="4" | Extension 0: Primary header, no data
 +
|- bgcolor="ffdead" 
 +
! FITS Keyword || Data Type || Units || Description
 +
|-
 +
|INSTRUME || String || || Instrument.
 +
|-
 +
| 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 $Y_{500}$.
 +
 
 +
|- bgcolor="ffdead" 
 +
!colspan="4" | Extension 1: data extension (BINTABLE)
 +
|- bgcolor="ffdead" 
 +
! 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|Caveats]] below.
 +
|-
 +
|SNR || Real*4 || || Signal-to-noise ratio of the detection.
 +
|-
 +
|PIPELINE || Int*4 || || Souce pipeline: 1= MMF1; 2 = MMF3; 3 = PwS.
 +
|-
 +
|PIPE_DET || Int*4 || || Pipelines which detect this object (note 2).
 +
|-
 +
|PCCS || Bool || || Indicates whether detection matches any PCCS source.
 +
|-
 +
|VALIDATION || Int*4 || || External validation status (Note 3)
 +
|-
 +
|ID_EXT || String|| || External identifier of cluster.
 +
|-
 +
|REDSHIFT || Real*4 || || Redshift of cluster.
 +
|-
 +
|COSMO || Bool || || Detection is in the cosmology sample.
 +
|-
 +
|COMMENT|| Bool || || Detection has a comment in the associated text file (Note 4).
 +
|}
 +
 
 +
'''Notes'''
 +
# format is ''PSZ1 Glll.ll+mn;bb.b'' where (l,b) are the Galactic and truncated to 2 decimal places.
 +
# The three least significant decimal digits are used to represent detection or non-detection by the pipelines. Order of the digits: hundreds = MMF1; tens = MMF3; units = PwS. If it is detected then the corresponding digit is set to 1, otherwise it is set to 0.
 +
# values are: 1 = candidate of class 1; 2 = candidate of class 2; 3 = candidate of class 3; 10 = Planck cluster confirmed by follow-up;  20 = known cluster.
 +
# The comments on the detections in the catalogue are contained in a text file called ''{{PLASingleFile|fileType=catdoc | name=COM_PCCS_SZ-union_comments_R1.11.txt | link=COM_PCCS_SZ-union_comments_R1.11.txt}}'', which contains one line for each detection in the union catalogue with COMMENT = T. The line starts with the INDEX and NAME of the detection to facilitate cross-referencing. The remainder of the line is the comment on that detection.
 +
 
 +
====Individual Catalogues====
 +
 
 +
The individual pipeline catalogues are contained in the FITS files
 +
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-MMF1_R1.11.fits  | link=COM_PCCS_SZ-MMF1_R1.11.fits }} (Matched Multi-Filter method #1)
 +
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-MMF3_R1.12.fits  | link=COM_PCCS_SZ-MMF3_R1.12.fits }} (Matched Multi-Filter method #3)
 +
* {{PLASingleFile | fileType=cat | name=COM_PCCS_SZ-PwS_R1.11.fits  | link=COM_PCCS_SZ-PwS_R1.11.fits }} (Powell Snakes method)
 +
Their structure is as follows:
 +
 
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|+ '''FITS file structure'''
 +
|- bgcolor="ffdead" 
 +
 
 +
! colspan="4" | Ext. 0: Primary header, no data
 +
|- bgcolor="ffdead" 
 +
! 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 $Y_{500}$.
 +
|- bgcolor="ffdead" 
 +
 
 +
 
 +
! colspan="4" | Ext. 1: EXTNANE = ''PSZ_INDIVIDUAL'' (BINTABLE)
 +
|- bgcolor="ffdead" 
 +
! 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|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).
 +
 
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data Type || Value || Description
 +
|-
 +
| PIPELINE || String || || Name of detection pipeline.
 +
|- bgcolor="ffdead" 
 +
 
 +
 
 +
! colspan="4" | Ext. 2: EXTNAME = ''PSZ_PROBABILITY'' (IMAGE) - Note 3
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data Type || Value || Description
 +
|-
 +
| NAXIS1 || Integer || 256 || Dim 1
 +
|-
 +
| NAXIS2 || Integer || 256 || Dim 2
 +
|-
 +
| NAXIS3 || Integer || Nsources || Dim 3 = Number of sources
 +
|- bgcolor="ffdead" 
 +
! Keyword || Data Type || Value || Description
 +
|-
 +
| PIPELINE || String || || Name of detection pipeline.
 +
|}
 +
 
 +
'''Notes'''
 +
# Format ''PSZ1 Glll.ll&plusmn;bb.bb'' where (l, b) are the Galactic coordinates truncated to 2 decimal places.
 +
# 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.
 +
# Ext. 2 contains a three-dimensional image with the two-dimensional probability distribution in $\theta_\mathrm{s}$ and $Y$ for each detection. The probability distributions are evaluated on a 256 &times; 256 linear grid between the limits specified in Ext. 1. The limits are determined independently for each detection. The dimension of the 3D image is 256 &times; 256 &times; n, where n is the number of detections.  The first dimension is $\theta_\mathrm{s}$ and the second dimension is $Y$.
 +
 
 +
====Mask====
 +
 
 +
The mask used to construct the catalogue is contained in a file
 +
: ''{{PLASingleFile|fileType=catdoc | name=COM_PCCS_SZ-unionMask_2048_R1.11.fits| link=COM_PCCS_SZ-unionMask_2048_R1.11.fits}}''. <span style="color:red">
 +
It is in GALACTIC coordinates, NESTED ordering, NSIDE=2048.
 +
 
 +
====Additional information====
 +
 
 +
A set of comments on the union catalogue is available in
 +
 
 +
: ''{{PLASingleFile|fileType=cat | name=COM_DocPCCS_SZ-union-comments_R1.11.txt | link=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
 +
 
 +
: ''{{PLASingleFile|fileType=cat | name=COM_PCCS_SZ-validation_R1.12.fits | link=COM_PCCS_SZ-validation_R1.12.fits}}''
 +
 
 +
(for more details see {{PlanckPapers|planck2013-p05a}}). This file contains a single ''BINTABLE'' extension.  The table contains 1 line per source, and the columns and their meaning are given below.
 +
 
 +
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
 +
|+ '''FITS file structure'''
 +
|- bgcolor="ffdead" 
 +
 
 +
! colspan="4" | Ext. 0:  (BINTABLE)
 +
|- bgcolor="ffdead" 
 +
! 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<sup>-4</sup> arcmin<sup>2</sup> || Compton parameter in R500 from SZ-proxy.
 +
|-
 +
|ERRP_YZ_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup>  || Error sup. in YZ_500
 +
|-
 +
|ERRM_YZ_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup>  || Error inf. in YZ_500
 +
|-
 +
|M_YZ_500 || Real*4 || 10<sup>14</sup> Msol|| Derived mass estimate (M_YZ_500) from SZ proxy.
 +
|-
 +
|ERRP_M_YZ_500 || Real*4 || 10<sup>14</sup> Msol || Error sup. on M_YZ_500.
 +
|-
 +
|ERRM_M_YZ_500 || Real*4 || 10<sup>14</sup> Msol || Error sup. on M_YZ_500.
 +
|-
 +
|S_X || Real*4 || erg/s/cm<sup>2</sup>  || Unabsorbed X-ray flux - see Note 1.
 +
|-
 +
|ERR_S_X || Real*4 || erg/s/cm<sup>2</sup>  || Error on unabsorbed X-ray flux.
 +
|-
 +
|Y_PSX_500 || Real*4 || 10<sup>-4</sup> arcmin<sup>2</sup> || SZ signal for PSZ clusters identified with MCXC clusters- see Note 2.
 +
|-
 +
|SN_PSX || Real*4 ||  || Signal to noise for PSZ clusters identified with MCXC clusters - see Note 3.
 +
|}
 +
 
 +
'''Notes'''
 +
# Unabsorbed X-ray flux measured in an aperture of 5 arcmin in the band [0.1-2.4] keV. The aperture is centered on the Planck position, except for candidates associated with a BSC source for which we adopt the X-ray position. For sources with <math>(S/N)_{RASS} < 1\sigma</math>, we only quote an upper limit.
 +
# SZ signal re-extracted fixing the size to the X-ray size provided in the MCXC catalogue at the X-ray position, for PSZ clusters identified with MCXC clusters.
 +
# Computed in the Planck data at the X-ray position fixing the size to the X-ray size provided in the MCXC catalogue, for PSZ clusters identified with MCXC clusters.
 +
# Source for redshifts:
 +
    -1 : No redshift available
 +
      1 : MCXC updated compilation{{BibCite|Piffaretti2011}}
 +
      2 : Databases NED and SIMBAD-CDS
 +
      3 : SDSS cluster catalogue{{BibCite|Wen2012}}
 +
      4 : SDSS cluster catalogue{{BibCite|Szabo2011}}
 +
      5 : SPT{{BibCite|Vanderlinde2010}}{{BibCite|Williamson2011}}{{BibCite|Andersson2011}}{{BibCite|Plagge2010}}{{BibCite|Reichardt2013}}{{BibCite|Story2011}}{{BibCite|Song2012}}
 +
      6 : ACT{{BibCite|Hasselfield2013}}{{BibCite|Marriage2011}}{{BibCite|Menanteau2010}}{{BibCite|Sifon2013}}
 +
      7 : Search in SDSS galaxy catalogue from Planck Collab.
 +
    20 : XMM-Newton confirmation from Planck Collab.
 +
    50 : ENO-imaging confirmation from Planck Collab.
 +
    60 : WFI-imaging confirmation from Planck Collab.
 +
    65 : NTT-spectroscopic confirmation from Planck Collab.
 +
    500 : RTT-spectroscopic confirmation from Planck Collab.
 +
    600 : NOT-spectroscopic confirmation from Planck Collab.
 +
    650 : GEMINI-spectroscopic confirmation from Planck Collab.
 +
    700 : ENO-spectroscopic confirmation from Planck Collab.
 +
 
 +
===Caveats===
 +
 
 +
The following issue was found in Feb. 2014 in R1.11 of the MMF3 catalogue: the POS_ERR field values are overestimated by a factor 3.125 on average.  This issue has been resolved in R1.12.  A corrected version of the union catalogue has also been produced (also R1.12)
 +
 
 +
The approximate 68% (1-sigma) confidence interval in the POS_ERR field is computed as half of the 95% (2-sigma) confidence interval. Previously this was erroneously described as a 95% confidence interval.
 +
 
 +
== The ERCSC ==
 +
 
 +
 
 +
The Plank Early Release Compact Source Catalogue was the first Planck product to be publicly released in Jan 2011. It was produced with a very rapid turnaround to facilitate follow-up observations with existing  cryogenic observatories such as Herschel. It contained a list of all high reliability sources, both Galactic and extragalactic, that were derived from the first all sky coverage by Planck. i.e., using observations obtained from 12 August 2009 to 6 June 2010. Thus the full sky was covered once, and ~60% of the sky was covered twice. The goals were to achieve a photometric accuracy of 30% and a positional accuracy  1/5 of the beam FWHM in the RMS sense.
 +
 
 +
The ERCSC consisted of nine source lists, one at each of the nine Planck frequency channels. The number of sources in the lists range from 705 at 30 GHz to 8988 at 857 GHz. No attempt was made to cross-match the sources from the different frequencies due to the wide range of spatial resolutions (33 arcmin at 30 GHz to 4.3 arcmin at 857 GHz) spanned by Planck. Furthermore, a list of ''Cold Cores'' of interstellar molecular clouds within the Galaxy and a list of galaxy clusters detected through the Sunyaev- Zel’dovich effect (SZ), were also provided. These consisted of candidate sources that were detected using multifrequency algorithms that use the distinct spectral signature of such sources. The Cold Cores catalogue contained 915 sources while the SZ cluster catalogue consisted of 189 sources
 +
 
 +
In order to generate the ERCSC,  four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is >90%. Reliability is defined as the fraction of sources in the catalog which have measured flux densities which are within 30% of their true flux density. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10σ photometric flux density limit of the catalogue at $|b| > 30$ deg is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion.  The sensitivity of the ERCSC is shown in the figure below. The ERCSC sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs.
 +
 
 +
The multifrequency information from Planck allows some basic classification of the sources to be undertaken. In the Galactic plane, at frequencies below 100 GHz, the majority of the sources are dominated by synchrotron or free-free emission. At the higher frequencies, the sources are almost exclusively dominated by thermal dust emission. At high Galactic latitudes however, the synchrotron sources  dominate the source counts to 217 GHz with dusty sources being the primary source population at 353 GHz and higher. Recent attempts to classify a subset of the Planck 857 GHz sources at high latitudes based on cross-correlations with sources in other catalogs such as WISE and SDSS, found that almost half of them are associated with stars and low-redshift galaxies while a significant fraction (44%) might be interstellar medium features{{BibCite|Johnson2013}}.
 +
 
 +
Full details on the construction, contents and usage of the ERCSC, ECC and ESZ catalogues can be found in {{PlanckPapers|planck2011-1-10}}, {{PlanckPapers|planck2011-5-1a}},  {{PlanckPapers|planck2011-7-7b}}.
 +
 
 +
 
 +
[[File:Ercscsensfig.png | 500px | center | thumb |'''Flux density limits ''']]
 +
 
 +
 
 +
The figure shows the ERCSC flux density limits, quanitfied as the faintest ERCSC source at |b|<10 deg (dashed black line) and at |b|>30 deg (solid black line), compared to those of other wide area surveys ({{PlanckPapers|planck2011-1-10}}). Also shown are spectra of known sources of foreground emission as red lines. The ERCSC sensitivity is worse in the Galactic plane due to the strong contribution of ISM emission, especially at submillimeter wavelengths. At face value, the WMAP and Planck flux density limits appear to be comparable at the lowest frequencies, but the Planck ERCSC is much more complete as discussed in {{PlanckPapers|planck2011-1-10}}.
 +
 
 +
==References==
 +
---------------
 +
 
 +
<References />
 +
 +
 
  
−
The ERCSC is also accessible via the NASA/IPAC Infrared Science Archive [http://irsa.ipac.caltech.edu/Missions/planck.html].
 
  
−
[[Category:Data processing]]
+
[[Category:Mission products|005]]

Latest revision as of 16:56, 23 July 2014

The Catalogue of Compact Sources[edit]

Product description[edit]

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

The PCCS is a set of nine single-frequencies lists of sources extracted from the Planck nominal mission data. By definition its reliability is > 80% and a special effort was made to use simple selection procedures in order to facilitate statistical analyses. With a common detection method for all the channels and the additional three photometries, spectral analysis can also be done safely. The deeper completeness levels and, as a consequence, the higher number of sources compared with its predecessor the ERCSC, will allow the extension of previous studies to more sources and to fainter flux densities. The PCCS is the natural evolution of the ERCSC, but both lack polarization and multi-frequency information. Future releases will take advantage of the full mission data and they will contain information on properties of sources not available in this release, such as polarization, multi-frequency and variability.


Table 1: PCCS characteristics
Channel 30 44 70 100 143 217 353 545 857
Frequency [GHz] 28.4 44.1 70.4 100.0 143.0 217.0 353.0 545.0 857.0
Beam FWHM1 [arcmin] 32.38 27.10 13.30 9.88 7.18 4.87 4.65 4.72 4.39
SNR threshold 4.0 4.0 4.0 4.6 4.7 4.8 4.92/6.03 4.7/7.0 4.9/7.0
# of detections 1256 731 939 3850 5675 16070 17689 26472 35719
# of detections for |b| > 30º) 572 258 332 845 1051 1901 2035 4164 7851
Flux density uncertainty [mJy] 109 198 149 61 38 35 74 132 189
Min flux density4 [mJy] 461 825 566 266 169 149 298 479 671
90% completeness [mJ] 575 1047 776 300 190 180 330 570 680
Position uncertainty5 [arcmin] 1.8 2.1 1.4 1.0 0.7 0.7 0.8 0.5 0.4


Notes

  1. The Planck beams are described in Planck-2013-IV[1] and Planck-2013-VII[2]. This table shows the values which were adopted for the PCCS (derived from the effective beams).
  2. In the extragalactic zone (48% of the sky; see Fig. 2 in Planck-2013-XXVIII[3]).
  3. In the Galactic zone (52% of the sky; see Fig. 2 in Planck-2013-XXVIII[3]).
  4. Minimum flux density of the catalogue at |b| > 30º after excluding the 10% faintest sources.
  5. Positional uncertainty derived by comparison with PACO sample ([4][5][6]) up to 353 GHz and with Herschel samples (HRS, KINGFISH, HeViCS, H-ATLAS) in the other channels.

Before using the PCCS, please read the Cautionary Notes in the PCCS general description section. For full details, see paper Planck-2013-XXVIII[3].

Production process[edit]

For a description of the production and validation processes of the PCCS see the corresponding section.

Inputs[edit]

The data obtained from the Planck nominal mission between (2009 August 12 and 2010 November 27) have been processed into full-sky maps by the HFI and LFI Data Processing Centres (DPCs). A description of the processing can be found in Planck-2013-II[7] and Planck-2013-VI[8]. The data consist of two complete sky surveys and 60% of the third survey. This implies that the flux densities of sources obtained from the nominal mission maps are the average of at least two observations. The nine Planck frequency channel maps are used as input to the source detection pipelines. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Table 1.

The input data used to generate this product are the following:

Related products[edit]

Other products that are related and share some commonalities with the product being described here are the other catalogues:

  1. ERCSC
  2. SZ catalogue

File names[edit]

COM_PCCS_030_R1.30.fits
COM_PCCS_044_R1.30.fits
COM_PCCS_070_R1.30.fits
COM_PCCS_100_R1.20.fits
COM_PCCS_143_R1.20.fits
COM_PCCS_217_R1.20.fits
COM_PCCS_353_R1.20.fits
COM_PCCS_545_R1.20.fits
COM_PCCS_857_R1.20.fits

Meta Data[edit]

The PCCS source list in each frequency is structured as a FITS binary table having one row for each detected source. The details of the FITS file structure are below

FITS file structure
Extension 0: Primary header, no data
FITS Keyword Data Type Units Description
INSTRUME String LFI or HFI
VERSION String Version of PCCS
DATE String Date file created:yyyy-mm-dd
ORIGIN String Name of organization responsible for the data (LFI-DPC – HFI-DPC)
TELESCOP String PLANCK
CREATOR String Pipeline Version
DATE-OBS String days Start-up time of the survey: yyyy-mm-dd
DATE-END String days Ending time of the survey: yyyy-mm-dd
Extension 1: (BINTABLE)
Column Name Data Type Units Description
Identification
NAME String Source name (Note 1)
Source Position
GLON Real*8 degrees Galactic longitude based on extraction algorithm
GLAT Real*8 degrees Galactic latitude based on extraction algorithm
RA Real*8 degrees Right ascension (J2000) transformed from (GLON,GLAT)
DEC Real*8 degrees Declination (J2000) transformed from (GLON,GLAT)
Photometry
DETFLUX Real*4 mJy Flux density of source as determined by detection method
DETFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from detection method
APERFLUX Real*4 mJy Flux density of source as determined from the aperture photometry
APERFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from the aperture photometry
PSFFLUX Real*4 mJy Flux density of source as determined from PSF fitting
PSFFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from PSF fitting
GAUFLUX Real*4 mJy Flux density of source as determined from 2-D Gaussian fitting
GAUFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from 2-D Gaussian fitting
GAU_SEMI1 Real*4 arcmin Gaussian fit along axis 1 (FWHM; see Note 4 for axis definition)
GAU_SEMI1_ERR Real*4 arcmin Uncertainty (1 sigma) in derived Gaussian fit along axis 1
GAU_SEMI2 Real*4 arcmin Gaussian fit along axis 2 (FWHM)
GAU_SEMI2_ERR Real*4 arcmin Uncertainty (1 sigma) in derived Gaussian fit along axis 2
GAU_THETA Real*4 deg Gaussian fit orientation angle (Note 4)
GAU_THETA_ERR Real*4 deg Uncertainty (1 sigma) in derived gaussian fit orientation angle
GAU_FWHM_EFF Real*4 arcmin Gaussian fit effective FWHM
Flags and validation
EXTENDED Integer*2 Extended source flag (Note 2)
CIRRUS_N Integer*2 Number of sources detected at 857 GHz within 1 degree
EXT_VAL Integer*2 External validation flag (Note 3)
ERCSC String Name of the ERCSC counterpart if any
ONLY 857 GHz Catalogue
APERFLUX_217 Real*4 mJy Estimated flux density at 217 GHz
APERFLUX_ERR_217 Real*4 mJy Uncertainty in source flux density at 217 GHz
APERFLUX_353 Real*4 mJy Estimated flux density at 353 GHz
APERFLUX_ERR_353 Real*4 mJy Uncertainty in source flux density at 353 GHz
APERFLUX_545 Real*4 mJy Estimated flux density at 545 GHz
APERFLUX_ERR_545 Real*4 mJy Uncertainty in source flux density at 545 GHz


Notes

  1. Source names consist of a prefix and a position. The prefix used is PCCS1 fff for the catalogue at fff GHz. The position is in Galactic coordinates and specified as "Glll.ll±bb.bb" where the (l,b) values are truncated to two decimal places. For example, a source detected at (l,b) = (120.237, 4.231) in the 545 GHz Planck map would be labelled PCCS1 545 G120.23±04.23.
  2. The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criteria for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
  3. The EXT_VAL flag takes the value of 0, 1, or 2, based on the following conditions:
    = 2: The source has a clear counterpart in one of the catalogues considered as ancillary data.
    = 1: The source has no clear counterpart in one of the ancillary catalogues but it has been detected by the internal multi-frequency method (LFI channels) or match with neighbouring frequencies, above or below (HFI channels).
    = 0: The source has no clear counterpart in one of the ancillary catalogues and it has not been detected by the internal multi-frequency method or neighbouring frequencies.
  4. The x-axis is defined for each source as parallel to the line of constant colatitude, with the same direction as the longitude. Therefore the position angles are measured anticlockwise from the y-axis.

The SZ catalogues[edit]

The Planck SZ catalogue is constructed as described in SZ catalogue and in section 2 of Planck-2013-XXIX[9].

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[9].

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[9]). 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[10]
     2 : Databases NED and SIMBAD-CDS
     3 : SDSS cluster catalogue[11]
     4 : SDSS cluster catalogue[12]
     5 : SPT[13][14][15][16][17][18][19]
     6 : ACT[20][21][22][23]
     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.

The ERCSC[edit]

The Plank Early Release Compact Source Catalogue was the first Planck product to be publicly released in Jan 2011. It was produced with a very rapid turnaround to facilitate follow-up observations with existing cryogenic observatories such as Herschel. It contained a list of all high reliability sources, both Galactic and extragalactic, that were derived from the first all sky coverage by Planck. i.e., using observations obtained from 12 August 2009 to 6 June 2010. Thus the full sky was covered once, and ~60% of the sky was covered twice. The goals were to achieve a photometric accuracy of 30% and a positional accuracy 1/5 of the beam FWHM in the RMS sense.

The ERCSC consisted of nine source lists, one at each of the nine Planck frequency channels. The number of sources in the lists range from 705 at 30 GHz to 8988 at 857 GHz. No attempt was made to cross-match the sources from the different frequencies due to the wide range of spatial resolutions (33 arcmin at 30 GHz to 4.3 arcmin at 857 GHz) spanned by Planck. Furthermore, a list of Cold Cores of interstellar molecular clouds within the Galaxy and a list of galaxy clusters detected through the Sunyaev- Zel’dovich effect (SZ), were also provided. These consisted of candidate sources that were detected using multifrequency algorithms that use the distinct spectral signature of such sources. The Cold Cores catalogue contained 915 sources while the SZ cluster catalogue consisted of 189 sources

In order to generate the ERCSC, four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is >90%. Reliability is defined as the fraction of sources in the catalog which have measured flux densities which are within 30% of their true flux density. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10σ photometric flux density limit of the catalogue at $|b| > 30$ deg is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The sensitivity of the ERCSC is shown in the figure below. The ERCSC sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs.

The multifrequency information from Planck allows some basic classification of the sources to be undertaken. In the Galactic plane, at frequencies below 100 GHz, the majority of the sources are dominated by synchrotron or free-free emission. At the higher frequencies, the sources are almost exclusively dominated by thermal dust emission. At high Galactic latitudes however, the synchrotron sources dominate the source counts to 217 GHz with dusty sources being the primary source population at 353 GHz and higher. Recent attempts to classify a subset of the Planck 857 GHz sources at high latitudes based on cross-correlations with sources in other catalogs such as WISE and SDSS, found that almost half of them are associated with stars and low-redshift galaxies while a significant fraction (44%) might be interstellar medium features[24].

Full details on the construction, contents and usage of the ERCSC, ECC and ESZ catalogues can be found in Planck-Early-VII[25], Planck-Early-VIII[26], Planck-Early-XXIII[27].


Flux density limits


The figure shows the ERCSC flux density limits, quanitfied as the faintest ERCSC source at |b|<10 deg (dashed black line) and at |b|>30 deg (solid black line), compared to those of other wide area surveys (Planck-Early-VII[25]). Also shown are spectra of known sources of foreground emission as red lines. The ERCSC sensitivity is worse in the Galactic plane due to the strong contribution of ISM emission, especially at submillimeter wavelengths. At face value, the WMAP and Planck flux density limits appear to be comparable at the lowest frequencies, but the Planck ERCSC is much more complete as discussed in Planck-Early-VII[25].

References[edit]

  1. ↑ Planck 2013 results: LFI Beams, Planck Collaboration 2013 IV, A&A, in press, (2014).
  2. ↑ Planck 2013 results: HFI time response and beams, Planck Collaboration 2013 VII, A&A, in press, (2014).
  3. ↑ 3.03.13.2 Planck 2013 results: The Planck Catalogue of Compact Sources, Planck Collaboration XXVIII, A&A, in press, (2014).
  4. ↑ The Planck-ATCA Co-eval Observations project: the brightsample, M. Massardi, A. Bonaldi, L. Bonavera, M. López-Caniego, G. de Zotti, R. D. Ekers, MNRAS, 415, 1597-1610, (2011).
  5. ↑ The Planck-ATCA Coeval Observations project: the faintsample, L. Bonavera, M. Massardi, A. Bonaldi, J. González-Nuevo, G. de Zotti, R. D. Ekers, MNRAS, 416, 559-566, (2011).
  6. ↑ The Planck-ATCA Co-eval Observations project: the spectrallyselected sample, A. Bonaldi, L. Bonavera, M. Massardi, G. De Zotti, MNRAS, 428, 1845-1854, (2013).
  7. ↑ Planck 2013 results: The Low Frequency Instrument data processing, Planck Collaboration 2013 II, A&A, in press, (2014).
  8. ↑ Planck 2013 results: High Frequency Instrument Data Processing, Planck Collaboration 2013 VI, A&A, in press, (2014).
  9. ↑ 9.09.19.2 Planck 2013 results: The Planck catalogue of Sunyaev-Zeldovich sources, Planck Collaboration XXIX, A&A, in press, (2014).
  10. ↑ 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).
  11. ↑ 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).
  12. ↑ 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).
  13. ↑ 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).
  14. ↑ 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).
  15. ↑ 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).
  16. ↑ 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).
  17. ↑ 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).
  18. ↑ 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).
  19. ↑ 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).
  20. ↑ 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).
  21. ↑ 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).
  22. ↑ 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).
  23. ↑ 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).
  24. ↑ Classification of Compact Submillimeter Sources in the Planck Archive, C. H. Johnson, C. Border, K. O'Connor, D. Rothrock, R. Chary, M. Bingham, M. Clark, M. Ernst, S. Gilbert, S. Koop, M. Maddaus, I. Miller, A. O'Bryan, T. Ravelomanantsoa, D. San Miguel, L. Schmidt, E. Searls, W. Tong, O. Torres, A. Zeidner, NITARP, in American Astronomical Society Meeting Abstracts American Astronomical Society Meeting Abstracts, 221, 352.18, (2013).
  25. ↑ 25.025.125.2 Planck early results. VII. The Early Release Compact Source Catalogue, Planck Collaboration VII, A&A, 536, A7, (2011).
  26. ↑ Planck early results. VIII. The all-sky early Sunyaev-Zeldovich cluster sample, Planck Collaboration VIII, A&A, 536, A8, (2011).
  27. ↑ Planck early results. XXIII. The Galactic cold core population revealed by the first all-sky survey, Planck Collaboration XXIII, A&A, 536, A23, (2011).

Early Release Compact Source Catalog

Full-Width-at-Half-Maximum

(Planck) High Frequency Instrument

(Planck) Low Frequency Instrument

Flexible Image Transfer Specification

Data Processing Center

Sunyaev-Zel'dovich

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