Catalogues

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Planck Catalogue of Compact Sources[edit]

The Planck Catalogue of Compact Sources is a set of single frequency lists of sources, both Galactic and extragalactic, extracted from the Planck maps.

The first public version of the PCCS was derived from the nominal mission data acquired by Planck between August 13 2009 and November 26 2010, as described in Planck-2013-XXVIII[1]. It consisted of nine lists of sources, one per channel between 30 and 857 GHz. The second public version of the catalogue (PCCS2) has been produced using the full mission data obtained between August 13 2009 and August 3 2013, as described in Planck-2015-A35[2], it consists of fifteen lists of sources, one list per channel at 30, 44 and 70 GHz, and two lists per channel at 100, 143, 217, 353, 545 and 857 GHz.

The maps used to produce these catalogues are the 2015 full mission frequency maps (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_SkyMap_???_2048_R2.00_full.fits).

The are three main differences between the PCCS and the PCCS2:

  1. The amount of data used to build the PCCS (Nominal Mission with 15.5 months) and PCCS2 (Full Mission with 48 months of LFI data and 29 months of HFI data).
  2. The inclusion of polarization information between 30 and 353 GHz, the seven Planck channels with polarization capabilities.
  3. The division of the catalogues into two sub-catalogues between 100-857 GHz, the PCCS2 and the PCCS2E, based on the location of the sources in the sky and on our ability to validate them.

Both the 2013 PCCS and the 2015 PCCS2 can be downloaded from the Planck Legacy Archive.

Detection procedure[edit]

The Mexican Hat Wavelet 2[3][4] is the base algorithm used to produce the single channel catalogues of the PCCS and the PCCS2. 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[5] (MTXF) and the Bayesian PowellSnakes [6]. Both of them have been used both in PCCS and PCCS2 for the validation of the results obtained by the MHW2 in total intensity.

In addition, two maximum likelihood methods have been used to do the analysis in polarization. Both of them can be used to blindly dectect sources in polarization maps. However, the PCCS2 analysis has been performed in a non-blind fashion, looking at the positions of the sources already detected in total intensity and providing an estimation of the polarized flux density. As for total intensity, each DPC has its own implementation of this code (IFCAPOL and PwSPOL). The IFCAPOL algorithm is based on the Filter Fusion technique [7] and has been applied to WMAP maps [8]. The PwSPOL algortihm is a modified version of PwS, the code used in the Early Release Compact Source catalogue Planck-Early-VII[9]. In practice, both of them are filtering methods based on matched filters, that filter the Q and U maps before attempting to estimate the flux density from each.

The detection of the compact sources is done locally on small flat patches to improve the efficiency of the process. The reason for this being that the filters can be optimized taking into accont the statistical properties of the background in the vicinity of the sources. In order to perform this local analysis, 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 optimized 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. Similarly, in polarization a flat patch centered at the position of the source detected in total intensity is obtained from the all-sky Q and U maps. Then a matched filter is computed taking into account the beam profile at each frequency and the power spectrum of each of the projected flat patches. In both cases, the filters are normalized in such a way that they preserve the amplitude of the sources after filtering, while removing the large scale diffuse emission and the small scale noise fluctuation.

The primary goal of the ERCSC was reliability greater than 90%. In order to increase completeness and explore possibly interesting new sources at fainter flux density levels, however, the initial overall reliability goal of the PCCS was reduced to 80%. The S/N thresholds applied to each frequency channel were determined, as far as possible, to meet this goal. The reliability of the PCCS catalogues has been assessed using the internal and external validation described below.

At 30, 44, and 70 GHz, the reliability goal alone would permit S/N thresholds below 4. A secondary goal of minimizing the upward bias on flux densities led to the imposition of an S/N threshold of 4.

At higher frequencies, where the confusion caused by the Galactic emission starts to become an issue, the sky was divided into two zones, one Galactic (52% of the sky) and one extragalactic (48% of the sky). At 100, 143, and 217 GHz, the S/N threshold needed to achieve the target reliability is determined in the extragalactic zone, but applied uniformly on sky. At 353, 545, and 857 GHz, the need to control confusion from Galactic cirrus emission led to the adoption of different S/N thresholds in the two zones. The extragalactic zone has a lower threshold than the Galactic zone.

In the PCCS2 we still have an 80% reliability goal, but a new approach has been followed. There was a demand for the possibility of producing an even higher reliability catalogue from Planck, and a new reliability flag has been added to the catalogues for this purpose.

In this version of the Planck catalogue of compact sources, between 100-857 GHz, we have split the catalogue into two, PCCS2 and PCCS2E, based on our ability to validate each of the sources.

For the lower frequencies, between 30 and 70 GHz, we still use a S/N threshold of 4. Moreover, as will be explained below, we use external catalogues and a multifrequency analysis to validate the sources. For the higher frequency channels, at 100 GHz and above, there is very little external information available to validate the catalogues and the validation has instead been done statistically and by applying Galactic masks and cirrus masks.

Photometry[edit]

In addition of the native flux density estimation provided by the detection algorithm, three additional measurements are obtained for each of the sources in the parent samples in total intensity. These additional flux density estimations are based on aperture photometry, PSF fitting and Gaussian fitting (see Planck-2013-XXVIII[1] for a detailed description of these additional photometries). The native flux density estimation is the only one that is obtained directly from the projected filtered maps while for the others the flux density estimates have a local background subtracted. The flux density estimations have not been color corrected because that would limit the usability of the catalogue. Color corrections are available in Section 7.4 of the LFI DPC paper Planck-2015-A03[10] and Section of the HFI DPC paper Planck-2015-A08[11], and can be applied by the user. In polarization we have used two methods to measure the flux densities in the Stokes Q and U maps. One is a maximum likelihood filtering method and the other is aperture photometry.

Validation process[edit]

The PCCS, its sources and the four different estimates of the flux density, have undergone an extensive internal and external validation process to ensure the quality of the catalogues. The validation of the non-thermal radio sources can be done with a large number of existing catalogues, whereas the validation of thermal sources is mostly done with simulations. These two approaches will be discussed below. Detections identified with known sources have been appropriately flagged in the catalogues.

Internal validation[edit]

The catalogues have been validated through an internal Monte-Carlo quality assessment process that uses large numbers of source injection and detection loops to characterize their properties, both in total intensity and polarization. For each channel, we calculate statistical quantities describing the quality of detection, photometry and astrometry of the detection code. The detection in total intensity is described by the completeness and reliability of the catalogue: completeness is a function of intrinsic flux, the selection threshold applied to detection (S/N) and location, while reliability is a function only of the detection S/N. The quality of photometry and astrometry is assessed through direct comparison of detected position and flux density parameters with the known inputs of matched sources. An input source is considered to be detected if a detection is made within one beam FWHM of the injected position. In polarization, we have also made Monte-Carlo quality assessments injecting polarized sources into the maps and attempting to detect and characterize their properties. In the three lowest frequencies, the sources have been injected in the real Q and U maps, while at 100 GHz and above, maps from the Full Focal Plane 8 simulations have been used.

External validation[edit]

At the three lowest frequencies of Planck, it is possible to validate the PCCS source identifications, completeness, reliability, positional accuracy and flux density accuracy using external data sets, particularly large-area radio surveys (NEWPS, AT20G, CRATES). Moreover, the external validation offers the opportunity for an absolute validation of the different photometries, directly related with the calibration and the knowledge of the beams. We have used several external catalogues to validate the data, but one additional excercise has been done. Simultaneous observations of a sample of 61 sources has been carried out in the Very Large Array, the Australia Compact Array and Planck at 30 and 44 GHz. Special Planck maps have been made covering just the observation period to avoid having more than one observation of the same source in the maps, minimizing the variability effects. As a result of this exercise, we have been able to validate our flux densities at the few percent level.

At higher frequencies, surveys as the South-Pole Telescope (SPT), the Atacama Cosmology Telescope (ACT) and H-ATLAS or HERMES from Herschel are very important, although only for limited regions of the sky. In particular, the Herschel synergy is crucial to study the possible contamination of the catalogues caused by the Galactic cirrus at high frequencies.

Cautionary notes[edit]

We list here some cautionary notes for users of the PCCS.

  • 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 Planck-2013-II[12]Planck-2013-VI[13]. 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 2.6 sky coverages, the PCCS provides only a single average flux density estimate over all Planck data samples that were included in the maps and does not contain any measure of the variability of the sources from survey to survey.
  • Contamination from CO: At infrared/submillimetre frequencies (100 GHz and above), the Planck bandpasses straddle energetically significant CO lines (see Planck-2013-XIII[14]). The effect is the most significant at 100 GHz, where the line might contribute more than 50% of the measured flux density of some sources. 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 measured continuum flux density of the source.
  • Bandpass corrections: For many sources in the three lowest Planck frequency channels, the bandpass correction of the Q and U flux densities is not negligible. Even though we have attempted to correct for this effect on a source by source basis and have propagated this uncertainty into the error bars on the polarized flux densities and polarization angles, there is still room for improvement. This can be seen in the residual leakage present at the position of Taurus A in the Stokes U maps. It is anticipated that there will be future updates to the LFI PCCS2 catalogues once the bandpass corrections and errors have been improved.
  • Photometry: Each source has multiple estimates of flux density, DETFLUX, APERFLUX, GAUFLUX and PSFFLUX, as defined above. The evaluation of APERFLUX makes the smallest number of assumptions about the data and hence is the most robust, especially in regions of high non-Gaussian background emission, but it may have larger uncertainties than the other methods. For bright resolved sources, GAUFLUX is recommended, with the caveat that it may not be robust for sources close to the Galactic plane due to the strong backgrounds. We have noticed that at the position of some of the brightest sources in polarization there is a small spurious signal related to the complex beams in polarization. This signal can have a small impact on the measurements of the flux densities in Q and/or U. In particular, this spurious signal can have an impact on the polarization position angle in those objects where most of the flux density of the source happens to be in one of the Q or U maps, like in the Crab nebula. In Planck-2015-A35[2] we have done an extensive analysis of the Crab nebula exploring different ways to remove this effect, but the polarization angles of the other sources in the catalogue have to be used with caution.
  • Cirrus/ISM: The upper bands of HFI could be contaminated with sources associated with Galactic interstellar medium features (ISM) or cirrus. The values of the parameters, CIRRUS N and SKY BRIGHTNESS in the catalogues may be used as indicators of contamination. CIRRUS N may be used to flag sources that might be clustered together and thereby associated with ISM structure. In order to provide some indications of the range of values of these parameters which could indicate contamination, we compared the properties of the IRAS-identified and non-IRAS-identified sources for both the PCCS2 and the PCCS2E, since outside the Galactic plane at Galactic latitudes |b| > 20◦, we can use the RIIFSCz [15] to provide a guide to the likely nature of sources. We cross match the PCCS2 857 GHz catalogue and the PCCS2E 857 GHz catalogue to the IRAS sources in the RIIFSCz using a 3 arcmin matching radius. Of the 4891 sources in the PCCS2 857 GHz catalogue 3094 have plausible IRAS counterparts while 1797 do not. Examination of histograms of the CIRRUS N and SKY BRIGHTNESS parameters in the PCCS2 show that these two classes of objects behave rather differently. The IRAS-identified sources have a peak sky brightness at about 1 MJy.sr−1. The non-IRAS-identified sources have a bimodal distribution with a slight peak at 1 MJy.sr−1 and a second peak at about 2.6 MJy.sr−1 . Both distributions have a long tail, but the non-IRAS-Identified tail is much longer. On this basis sources with SKY BRIGHTNESS > 4 MJy.sr−1 should be treated with caution. In contrast non-IRAS-identified sources with SKY BRIGHTNESS < 1.4 MJy.sr−1 are likely reliable. Examination of their sky distribution, for example, shows that many such sources lie in the IRAS coverage gaps. The CIRRUS N flag tells a rather similar story. Both IRAS-matched and IRAS non-matched sources have a peak CIRRUS N value of 2, but the non-matched sources have a far longer tail. Very few IRAS-matched sources have a value > 8 but many non- matched sources do. These should be treated with caution. The PCCS2E 857 GHz catalogue contains 10470 sources with |b| > 20◦ of which 1235 are matched to IRAS sources in the RIIFSCz and 9235 are not. As with the PCCS2 catalogue the distributions of CIRRUS N and SKY BRIGHTNESS are different, with the differences even more pronounced for these PCCS2E sources. Once again, few IRAS-matched sources have SKY BRIGHTNESS > 4 MJy.sr−1 , but the non-matched sources have brightnesses extending to >55MJy.sr−1. Similarly hardly any of the IRAS-matched sources have CIRRUS N > 8 but nearly half the unmatched sources do. The WHICH ZONE flag in the PCCS2E encodes the region in which the source sits, be it inside the filament mask (WHICH ZONE=1), the Galactic region (WHICH ZONE=2), or both (WHICH ZONE=3). Of the 9235 PCCS2E 857GHz sources that do not match an IRAS source and that lie in the region, |b| > 20◦, 1850 (20%) have WHICH ZONE=1, 2637 (29 %) have WHICH ZONE=2 and 4748 (51 %) have WHICH ZONE=3. The PCCS2E covers 30.36 % of the region |b| > 20◦ , where 2.47 % is in the filament mask, 23.15 % in the Galactic region and 4.74 % in both. If the 9235 unmatched detections were distributed uniformly over the region, |b| > 20◦, we can predict the number of non-matched sources in each zone and compare this to the values we have. We find that there are 2.5 and 3.3 times more sources than expected in zones 1 and 3, showing that the filament mask is indeed a useful criterion for regarding sources detected within it as suspicious. It should be noted that the EXTENDED flag could also be used to identify ISM features, but nearby Galactic and extra-galactic sources that are extended at Planck spatial resolution will also meet this criterion.



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

The second Planck Catalogue of Compact Sources (PCCS2) is a set of single-frequency source catalogues extracted from the Planck full-mission maps in intensity and polarization (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_SkyMap_???_2048_R2.00_full.fits). The catalogues have been constructed as described in PCCS and in section 2 of Planck-2015-A26[2]. The validation of the catalogues is described in section 3 of Planck-2015-A26[2].

The catalogue at 100 GHz and above has been divided into two sub-catalogues: the PCCS2, here the sources have been detected in regions of the sky where it is possible to estimate the reliability of the detections, either statistically or by using external catalogues; PCCS2, here the detected sources are located in regions of the sky where it is not possible to make an estimate of their reliability.

By definition, the reliability of the whole PCCS2 is ≥ 80%, and a flag is available that allows the user to select a subsample of sources with a higher level of reliability (e.g., 90% or 95%).

The nine Planck full-mission frequency channel maps are used as input to the source detection pipelines. They contain 48 months of data for LFI channels and 29 months of data for HFI channels. Therefore the flux densities of sources obtained from the full-mission maps are the average of at least 8 observations for LFI channels or at least 4 observations for HFI channels. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Tables 1 and 2.

Four different photometry methods have been used. For one of the methods, the native photometry from the Mexican hat wavelet detection algorithm, the analysis is performed on patches containing tangent plane projections of the map. For the other methods (aperture photometry, point spread function fitting, and Gaussian fitting), the analysis is performed directly on the full-sky maps.

PCCS2 in Intensity
Sky distribution of the PCCS2 intensity sources at three different channels: 30 GHz (red circles), 143 GHz (blue circles) and 857 GHz (green circles). The dimension of the circles is related to the brightness of the sources and the beam size of each channel.
PCCS2E in Intensity
Sky distribution of the PCCS2E intensity sources at three different channels: 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: 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 1560 934 1296 1742 2160 2135 1344 1694 4891
PCCS2E — — — 2487 4139 16842 22665 31068 43290
Union PCCS2+PCCS2E — — — 4229 6299 18977 24009 32762 48181
Number of sources in the extragalactic zonea.
PCCS2 745 367 504 1742 2160 2135 1344 1694 4891
PCCS2E — — — 0 0 26 289 839 2097
Union PCCS2+PCSS2E — — — 1742 2160 2161 1633 2533 6988
Flux densities [mJy] in the extragalactic zonea .
PCCS2
minimumb 376 603 444 232 147 127 242 535 720
90% completeness 426 676 489 269 177 152 304 555 791
uncertainty 87 134 101 55 35 29 55 105 168
PCCS2E
minimumb — — — — — 189 350 597 939
90% completeness — — — — — 144 311 557 927
uncertainty — — — — — 35 73 144 278

Table 1 Notes

a 30-70 GHz: the extragalactic zone is 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 122 30 34 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 — — — 43 111 325 666
Minimum polarized flux densitya [mJy] — — — 121 87 114 348
Polarized flux density uncertainty [mJy] — — — 52 44 55 178
Minimum polarized flux density completeness 90% [mJy] — — — 410 613 270 567
Minimum polarized flux density completeness 95% [mJy] — — — 599 893 464 590
Minimum polarized flux density completeness 100% [mJy] — — — 835 893 786 958

Table 2 Notes

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

Catalogues[edit]

The PCCS2 catalogues are contained in the FITS files:

COM_PCCS_030_R2.04.fits
COM_PCCS_044_R2.04.fits
COM_PCCS_070_R2.04.fits
COM_PCCS_100_R2.01.fits
COM_PCCS_143_R2.01.fits
COM_PCCS_217_R2.01.fits
COM_PCCS_353_R2.01.fits
COM_PCCS_545_R2.01.fits
COM_PCCS_857_R2.01.fits

and the PCCS2E catalogues are contained in the FITS files:

COM_PCCS_100-excluded_R2.01.fits
COM_PCCS_143-excluded_R2.01.fits
COM_PCCS_217-excluded_R2.01.fits
COM_PCCS_353-excluded_R2.01.fits
COM_PCCS_545-excluded_R2.01.fits
COM_PCCS_857-excluded_R2.01.fits

The structure of these files is as follows:

PCCS2/PCCS2E FITS file structure
Extension 0: Primary header, no data
FITS Keyword Data Type Units Description
INSTRUME String Instrument (LFI / HFI)
VERSION String Version of PCCS (PCCS2 / PCCS2_E)
DATE String Date file created: yyyy-mm-dd
ORIGIN String Name of organization responsible for the data (LFI-DPC / HFI-DPC)
TELESCOP String Telescope (PLANCK)
CREATOR String Pipeline Version
DATE-OBS String days Beginning of the survey: yyyy-mm-dd
DATE-END String days End of the survey: yyyy-mm-dd
FWHM Real*4 arcmin FWHM from an elliptical Gaussian fit to the effective beam
OMEGA_B Real*4 arcmin2 Area of the effective beam
FWHM_EFF Real*4 arcmin FWHM computed from OMEGA_B assuming beam is Gaussian
OMEGA_B1 Real*4 arcmin2 Beam area within a radius of 1 × FWHM_EFF
OMEGA_B2 Real*4 arcmin2 Beam area within a radius of 2 × FWHM_EFF
Extension 1: BINTABLE, EXTNAME = PCCS2_fff (where fff is the frequency channel)
Column Name Data Type Units Description
Identification
NAME String Source name (see note 1)
Source position
GLON Real*8 degrees Galactic longitude based on extraction algorithm
GLAT Real*8 degrees Galactic latitude based on extraction algorithm
RA Real*8 degrees Right ascension (J2000) transformed from (GLON,GLAT)
DEC Real*8 degrees Declination (J2000) transformed from (GLON,GLAT)
Photometry
DETFLUX Real*4 mJy Flux density of source as determined by detection method
DETFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from detection method
APERFLUX Real*4 mJy Flux density of source as determined from the aperture photometry
APERFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from the aperture photometry
PSFFLUX Real*4 mJy Flux density of source as determined from PSF fitting
PSFFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from PSF fitting
GAUFLUX Real*4 mJy Flux density of source as determined from 2-D Gaussian fitting
GAUFLUX_ERR Real*4 mJy Uncertainty (1 sigma) in derived flux density from 2-D Gaussian fitting
GAU_SEMI1 Real*4 arcmin Gaussian fit along axis 1 (FWHM; see note 2 for axis definition)
GAU_SEMI1_ERR Real*4 arcmin Uncertainty (1 sigma) in derived Gaussian fit along axis 1
GAU_SEMI2 Real*4 arcmin Gaussian fit along axis 2 (FWHM)
GAU_SEMI2_ERR Real*4 arcmin Uncertainty (1 sigma) in derived Gaussian fit along axis 2
GAU_THETA Real*4 deg Gaussian fit orientation angle (see note 2)
GAU_THETA_ERR Real*4 deg Uncertainty (1 sigma) in derived gaussian fit orientation angle
GAU_FWHM_EFF Real*4 arcmin Gaussian fit effective FWHM
Polarization measurements (30-353 GHz only)
P Real*4 mJy Polarization flux density of the sources as determined by a matched filter (see note 3)
P_ERR Real*4 mJy Uncertainty (1 sigma) in derived polarization flux density (see note 3)
ANGLE_P Real*4 degrees Orientation of polarization with respect to NGP (see notes 2 and 3)
ANGLE_P_ERR Real*4 degrees Uncertainty (1 sigma) in orientation of polarization (see note 3)
APER_P Real*4 mJy Polarization flux density of the sources as determined by aperture photometry (see note 3)
APER_P_ERR Real*4 mJy Uncertainty (1 sigma) in derived polarization flux density (see note 3)
APER_ANGLE_P Real*4 degrees Orientation of polarization with respect to NGP (see notes 2 and 3)
APER_ANGLE_P_ERR Real*4 degrees Uncertainty (1 sigma) in orientation of polarization (see note 3)
P_UPPER_LIMIT Real*4 mJy Polarization flux density 99.99% upper limit. This is provided only when P column is set to NULL; otherwise this column itself contains a NULL.
APER_P_UPPER_LIMIT Real*4 mJy Polarization flux density 99.99% upper limit. This is provided only when APER_P column is set to NULL; otherwise this column itself contains a NULL.
Marginal polarization measurements (100-353 GHz only) – see note 4
P_STAT Integer*2 Polarization detection status
PX Real*4 mJy Polarization flux density of the sources as determined by a matched filter using Bayesian polarization estimator.
PX_ERR_LOWER Real*4 mJy PX uncertainty; lower 95% error bar
PX_ERR_UPPER Real*4 mJy PX uncertainty; upper 95% error bar
ANGLE_PX Real*4 degrees Orientation of polarization with respect to NGP using Bayesian polarization estimator (see note 2)
ANGLE_PX_ERR_LOWER Real*4 degrees ANGLE_PX uncertainty; lower 95% error bar
ANGLE_PX_ERR_UPPER Real*4 degrees ANGLE_PX uncertainty; upper 95% error bar
Flags and validation
EXTENDED Integer*2 Extended source flag (see note 5)
EXT_VAL Integer*2 External validation flag (see note 6)
ERCSC String Name of the ERCSC counterpart, if any
PCCS String Name of the PCCS counterpart, if any
Flags and validation (PCCS2 only)
HIGHEST_RELIABILITY_CAT Integer*4 See note 7
Flags and validation (PCCS2E 100-857 GHz only)
WHICH_ZONE Integer*2 See note 8
Flags and validation (217-857 GHz only)
CIRRUS_N Integer*2 Number of sources (S/N > 5) detected at 857 GHz within a 1-degree radius.
SKY_BRIGHTNESS Real*4 MJy/sr The mean 857 GHz brightness within a 2-degree radius. This may be used as another indicator of cirrus contamination.
Flux densities at other frequencies (857 GHz only)
APERFLUX_217 Real*4 mJy Estimated flux density at 217 GHz
APERFLUX_ERR_217 Real*4 mJy Uncertainty in flux density at 217 GHz
APERFLUX_353 Real*4 mJy Estimated flux density at 353 GHz
APERFLUX_ERR_353 Real*4 mJy Uncertainty in flux density at 353 GHz
APERFLUX_545 Real*4 mJy Estimated flux density at 545 GHz
APERFLUX_ERR_545 Real*4 mJy Uncertainty in flux density at 545 GHz

Notes

  1. Format is PCCS2 fff Glll.ll±bb.bb for sources in the PCCS2 and PCCS2E fff Glll.ll±bb.bb for sources in the PCCS2E, where fff is the frequency channel and (l, b) is the position of the source in Galactic coordinates truncated to two decimal places.
  2. We follow the IAU/IEEE convention (Hamaker & Bregman 1996) for defining the angle of polarization of a source, and this convention is also used for the other angles in the catalogue. The angle is measured from the North Galactic Pole in a clockwise direction from -90 to 90 degrees.
  3. Provided when the significance of the polarization measurement is > 99.99% and set to NULL otherwise.
  4. The P_STAT flag gives the status of the marginal polarization detection, possible values are:
    3 – Bright: P field filled in; all PX fields set to NULL.
    2 – Significant: P field is set to NULL; 0 is outside the PX 95% HPD; all PX fields are filled.
    1 – Marginal: P field is set to NULL; 0 is inside the PX 95% HPD, but mode of PX posterior distribution is not 0; all PX fields are filled.
    0 – No detection: P field is set to NULL; mode of PX posterior distribution is 0; PX_ERRL, ANGLE_PX, ANGLE_PX_ERR_LOWER, and ANGLE_PX_ERR_UPPER are set to NULL.
  5. The EXTENDED flag has the value of 0 if the source is compact and the value of 1 is it extended. The source size is determined by the geometric mean of the Gaussian fit FWHMs, with the criterion for extension being sqrt(GAU_FWHMMAJ * GAU_FWHMIN) > 1.5 times the beam FWHM.
  6. The EXT_VAL flag gives the status of the external validation, possible values are:
    3 – The source has a clear counterpart in one of the catalogues used as ancillary data.
    2 – The source does not have a clear counterpart in one of the catalogues used as ancillary data but it has been detected by the internal multi-frequency method.
    1 – The source does not have a clear counterpart in one of the catalogues used as ancillary data and it has not been detected by the internal multi-frequency method, but it has been detected in a previous Planck source catalogue.
    0 – The source does not have a clear counterpart in one of the catalogues used as ancillary data and it has not been detected by the internal multi-frequency method.
  7. The HIGHEST_RELIABILTY_CAT column contains the highest reliability catalogue to which the source belongs. As the full catalogue reliability is ≥ 80%, this is the lowest possible value in this column. Where possible this is provided in steps of 1% otherwise it is in steps of 5%.
  8. The WHICH_ZONE column encodes the zone in which the source lies:
    1 – source lies inside filament mask.
    2 – source lies inside Galactic zone.
    3 – sources lies in both filament mask and Galactic zone.

Zone map[edit]

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

The files are called:

COM_PCCS_100-zoneMask_R2.01.fits
COM_PCCS_143-zoneMask_R2.01.fits
COM_PCCS_217-zoneMask_R2.01.fits
COM_PCCS_353-zoneMask_R2.01.fits
COM_PCCS_545-zoneMask_R2.01.fits
COM_PCCS_857-zoneMask_R2.01.fits

The structure of the files is as follows:

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

Notes

  1. This FITS extension contains an integer HEALPix map which encodes the information on which of 4 possible regions on the sky each pixel belongs to:
    0 – quantified-reliability zone (PCCS2).
    1 – filament mask.
    2 – Galactic zone.
    3 – filament mask and Galactic zone.

S/N threshold map[edit]

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

For the full catalogue (80% reliability in the quantified reliability zone) they are:

COM_PCCS_100-SN-threshold_R2.01.fits
COM_PCCS_143-SN-threshold_R2.01.fits
COM_PCCS_217-SN-threshold_R2.01.fits
COM_PCCS_353-SN-threshold_R2.01.fits
COM_PCCS_545-SN-threshold_R2.01.fits
COM_PCCS_857-SN-threshold_R2.01.fits

For 85% reliability they are:

COM_PCCS_100-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_143-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_217-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_353-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_545-SN-threshold-85pc-reliability_R2.01.fits
COM_PCCS_857-SN-threshold-85pc-reliability_R2.01.fits

For 90% reliability they are:

COM_PCCS_100-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_143-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_217-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_353-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_545-SN-threshold-90pc-reliability_R2.01.fits
COM_PCCS_857-SN-threshold-90pc-reliability_R2.01.fits

For 95% reliability they are:

COM_PCCS_100-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_143-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_217-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_353-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_545-SN-threshold-95pc-reliability_R2.01.fits
COM_PCCS_857-SN-threshold-95pc-reliability_R2.01.fits

The structure of the files is as follows:

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

Notes

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

Noise map[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:

COM_PCCS_100-noise-level_R2.01.fits
COM_PCCS_143-noise-level_R2.01.fits
COM_PCCS_217-noise-level_R2.01.fits
COM_PCCS_353-noise-level_R2.01.fits
COM_PCCS_545-noise-level_R2.01.fits
COM_PCCS_857-noise-level_R2.01.fits

The structure of the files is as follows:

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

Notes

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


Previous releases (PCCS and ERCSC)[edit]

Second Planck Release (2013): Description of the PCCS

The Catalogue of Compact Sources


Product description

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

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


Table 1: PCCS characteristics
Channel 30 44 70 100 143 217 353 545 857
Frequency [GHz] 28.4 44.1 70.4 100.0 143.0 217.0 353.0 545.0 857.0
Beam FWHM1 [arcmin] 32.38 27.10 13.30 9.88 7.18 4.87 4.65 4.72 4.39
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[16] and Planck-2013-VII[17]. 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[1]).
  3. In the Galactic zone (52% of the sky; see Fig. 2 in Planck-2013-XXVIII[1]).
  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 ([18][19][20]) 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[1].

Production process

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

Inputs

The data obtained from the Planck nominal mission between (2009 August 12 and 2010 November 27) have been processed into full-sky maps by the HFI and LFI Data Processing Centres (DPCs). A description of the processing can be found in Planck-2013-II[12] and Planck-2013-VI[13]. The data consist of two complete sky surveys and 60% of the third survey. This implies that the flux densities of sources obtained from the nominal mission maps are the average of at least two observations. The nine Planck frequency channel maps are used as input to the source detection pipelines. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Table 1.

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

Related products

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

  1. ERCSC
  2. SZ catalogue

File names

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

Meta Data

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

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


Notes

  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.

First Planck Release (2011): Description of the 2011 ERCSC (Early Compact Source, Cold Core and SZ Catalogues )

The ERCSC

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

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

In order to generate the ERCSC, four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is >90%. Reliability is defined as the fraction of sources in the catalog which have measured flux densities which are within 30% of their true flux density. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10σ photometric flux density limit of the catalogue at $|b| > 30$ 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[21].

Full details on the construction, contents and usage of the ERCSC, ECC and ESZ catalogues can be found in Planck-Early-VII[9], Planck-Early-VIII[22], Planck-Early-XXIII[23].


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[9]). 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[9].

(2015) Second SZ Catalogue[edit]

Planck Sunyaev-Zeldovich catalogue[edit]

The Planck SZ catalogue is a nearly full-sky list of SZ detections obtained from the Planck data. It is fully described in Planck-2013-XXIX[24], Planck-2015-A36[25]. The catalogue is derived from the HFI frequency channel maps after masking and filling the bright point sources (SNR >= 10) from the PCCS catalogues in those channels. Three detection pipelines were used to construct the catalogue, two implementations of the matched multi-filter (MMF) algorithm and PowellSnakes (PwS), a Bayesian algorithm. All three pipelines use a circularly symmetric pressure profile, the non-standard universal profile from [26], in the detection.

  • MMF1 and MMF3 are full-sky implementations of the MMF algorithm. The matched filter optimizes the cluster detection using a linear combination of maps, which requires an estimate of the statistics of the contamination. It uses spatial filtering to suppress both foregrounds and noise, making use of the prior knowledge of the cluster pressure profile and thermal SZ spectrum.
  • PwS differs from the MMF methods. It is a fast Bayesian multi-frequency detection algorithm designed to identify and characterize compact objects in a diffuse background. The detection process is based on a statistical model comparison test. Detections may be accepted or rejected based on a generalized likelihood ratio test or in full Bayesian mode. These two modes allow quantities measured by PwS to be consistently compared with those of the MMF algorithms.

A union catalogue is constructed from the detections by all three pipelines. A mask to remove Galactic dust, nearby galaxies and point sources (leaving 83.7% of the sky) is applied a posteriori to avoid detections in areas where foregrounds are likely to cause spurious detections. The completeness and reliability of the catalogues have been assessed through internal and external validation as described in section 4 of Planck-2015-A27[25].

The size of a detection is given in terms of the scale size, θs, and the flux is given in terms of the total integrated Comptonization parameter, Y = Y5R500. The parameters of the GNFW profile assumed by the detection pipelines are written in the headers of the catalogues. For the sake of convenience, the conversion factor from Y to Y500 is also provided in the header.

The union catalogue contains the coordinates of a detection, its signal-to-noise ratio, an estimate of Y and its uncertainty, together with a summary of the validation information, including external identification of a cluster and its redshift if they are available. The pipeline from which the information is taken is called the reference pipeline. If more than one pipeline makes the same detection, the information is taken from the the pipeline that makes the most significant detection. Where the redshift is known, we provide the SZ mass for the reference pipeline.

The individual catalogues contain the coordinates and the signal-to-noise ratio of the detections, and information on the size and flux of the detections. The entries are cross-referenced to the detections in the union catalogue. The full information on the degeneracy between θs and Y is included in the individual catalogues in the form of the two-dimensional probability distribution for each detection. It is computed on a well-sampled grid to produce a two-dimensional image for each detection. It is provided in this form so it can be combined with a model or external data to produce tighter constraints on the parameters. The individual catalogues also contain Planck measurements of the SZ mass observable, MSZ, as calculated using a Y-M scaling relation and an assumed redshift to break the Y-θs degeneracy. These are provided for each detection as functions of assumed redshift, in the range 0.01 < z < 1, along with the upper and lower 68% confidence limits.

The selection function of the union catalogue, the intersection catalogue and the individual catalogues are provided in additional files. The selection function files contains the probability of detection for clusters of given intrinsic parameters θ500 and Y500. The file includes the definition of the survey area in the form of a HEALPix mask, and is evaluated for a range of signal-to-noise thresholds between 4.5 and 10.

Union catalogue[edit]

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

Extension 0: Primary header, no data
FITS Keyword Data Type Units Description
INSTRUME String Instrument (HFI)
VERSION String Version of catalogue
DATE String Date file created: yyyy-mm-dd
ORIGIN String Name of organization responsible for the data (HFI-DPC)
TELESCOP String Telescope (PLANCK)
CREATOR String Pipeline version
DATE-OBS String Start date of the survey: yyyy-mm-dd
DATE-END String End date of the survey: yyyy-mm-dd
PROCVER String Data version
PP_ALPHA Real*4 GNFW pressure profile α parameter
PP_BETA Real*4 GNFW pressure profile β parameter
PP_GAMMA Real*4 GNFW pressure profile γ parameter
PP_C500 Real*4 GNFW pressure profile c500 parameter
PP_Y2YFH Real*4 Conversion factor from Y to Y500
Extension 1: BINTABLE, EXTNAME = PSZ2_UNION
Column Name Data Type Units Description
INDEX Int*4 Index used to cross-reference with individual catalogues
NAME String Source name (see note 1)
GLON Real*8 degrees Galactic longitude
GLAT Real*8 degrees Galactic latitude
RA Real*8 degrees Right ascension (J2000) transformed from (GLON,GLAT)
DEC Real*8 degrees Declination (J2000) transformed from (GLON,GLAT)
POS_ERR Real*4 arcmin Position uncertainty (95% confidence interval)
SNR Real*4 Signal-to-noise ratio of the detection
PIPELINE Int*4 Pipeline from which information is taken (reference pipeline): 1= MMF1; 2 = MMF3; 3 = PwS
PIPE_DET Int*4 Pipelines which detect this object (see note 2)
PCCS2 Bool Indicates whether detection matches with any in PCCS2 catalogues
PSZ Int*4 Index of matching detection in PSZ1, or -1 if new detection
IR_FLAG Int*1 Flag denoting heavy infrared contamination
Q_NEURAL Real*4 Neural network quality flag (see note 3)
Y5R500 Real*4 10-3 arcmin2 Mean marginal Y5R500 as determined by reference pipeline
Y5R500_ERR Real*4 10-3 arcmin2 Uncertainty on Y5R500 as determined by reference pipeline
VALIDATION Int*4 External validation status (see note 4)
REDSHIFT_ID String External identifier of cluster associated with redshift measurement (see note 5)
REDSHIFT Real*4 Redshift of cluster (see note 5)
MSZ Real*4 1014 Msol SZ mass proxy (see note 6)
MSZ_ERR_UP Real*4 1014 Msol Upper bound of 68% SZ mass proxy confidence interval (see note 6)
MSZ_ERR_LOW Real*4 1014 Msol Lower bound of 68% SZ mass proxy confidence interval (see note 6)
MCXC String Identifier of X-ray counterpart in the MCXC, if one is present
REDMAPPER String Identifier of optical counterpart in the RedMAPPer catalogue, if one is present
ACT String Identifier of SZ counterpart in the ACT catalogues, if one is present
SPT String Identifier of SZ counterpart in the SPT catalogues, if one is present
WISE_FLAG Int*4 Confirmation flag of WISE overdensity (see note 7)
AMI_EVIDENCE Real*4 Bayesian evidence for AMI counterpart detection (see note 8)
COSMO Bool Indicates whether detection is in the cosmology sample
COMMENT String Comments on this detection

Notes

  1. Format is PSZ2 Glll.ll±bb.b where (l,b) are the Galactic coordinates truncated to 2 decimal places.
  2. The three least significant decimal digits are used to represent detection or non-detection by the pipelines. Order of the digits: hundreds = MMF1; tens = MMF3; units = PwS. If it is detected then the corresponding digit is set to 1, otherwise it is set to 0.
  3. Neural network quality flag is 1-Qbad, following the definitions in Aghanim et al. 2014.
  4. Summary of the external validation, encoding the most robust external identification: 10 = ENO follow-up; 11 = RTT follow-up; 12 = PanSTARRs; 13 = RedMAPPer non-blind; 14 = SDSS high-z; 15 = AMI; 16 = WISE; 20 = legacy identification from the PSZ1; 21 = MCXC; 22 = SPT; 23 = ACT; 24 = RedMAPPer; 25 = legacy identification from PSZ1 with externally updated redshift; 30 = NED; -1 = no known external counterpart.
  5. Redshift source is the most robust external identification listed in the VALIDATION field.
  6. MSZ is the hydrostatic mass assuming the best-fit Y-M scaling relation of Arnaud 2010 as a prior. The uncertainties are statistical and based on the Planck measurement uncertainties only. Not included in the uncertainties are the statistical errors on the scaling relation, the intrinsic scatter in the relation, or systematic errors in data selection for the scaling relation fit.
  7. Assigned by visual inspection: 0 = no significant galaxy overdensity; 1 = possible galaxy overdensity; 2 = probable galaxy overdensity; 3 = significant galaxy overdensity detected; -1 = possible galaxy overdensity (affected by bright star artefacts); -2 = no significant galaxy overdensity (affected by bright star artefacts); -3 = no assessment possible (affected by bright star artefacts); -10 = not analysed.
  8. Defined in the paper.

Individual catalogues[edit]

The individual pipeline catalogues are contained in the FITS files

Their structure is as follows:

FITS file structure
Extension 0: Primary header, no data
FITS Keyword Data Type Units Description
INSTRUME String Instrument (HFI)
VERSION String Version of catalogue
DATE String Date file created: yyyy-mm-dd
ORIGIN String Name of organization responsible for the data (HFI-DPC)
TELESCOP String Telescope (PLANCK)
CREATOR String Pipeline version
DATE-OBS String Start time of the survey: yyyy-mm-dd
DATE-END String End time of the survey: yyyy-mm-dd
PROCVER String Data version
PP_ALPHA Real*4 GNFW pressure profile α parameter
PP_BETA Real*4 GNFW pressure profile β parameter
PP_GAMMA Real*4 GNFW pressure profile γ parameter
PP_C500 Real*4 GNFW pressure profile c500 parameter
PP_Y2YFH Real*4 Conversion factor from Y to Y500
Extension 1: BINTABLE, EXTNAME = PSZ2_INDIVIDUAL
Column Name Data Type Units Description
INDEX Int*4 Index from union catalogue
NAME String Source name (see note 1)
GLON Real*8 degrees Galactic longitude
GLAT Real*8 degrees Galactic latitude
RA Real*8 degrees Right ascension (J2000) transformed from (GLON, GLAT)
DEC Real*8 degrees Declination (J2000) transformed from (GLON, GLAT)
POS_ERR Real*4 arcmin Position uncertainty (95% confidence interval)
SNR Real*4 Signal-to-noise ratio of detection
TS_MIN Real*4 Minimum value of θs in grid in second extension HDU (see note 2)
TS_MAX Real*4 Maximum value of θs in grid in second extension HDU (see note 2)
Y_MIN Real*4 Minimum value of Y in grid in second extension HDU (see note 2)
Y_MAX Real*4 Maximum value of Y in grid in second extension HDU (see note 2)
Keyword Data Type Value Description
PIPELINE String Name of detection pipeline
Extension 2: IMAGE, EXTNAME = PSZ2_PROBABILITY (see note 2)
Keyword Data Type Value Description
NAXIS1 Integer 256 Dimension 1
NAXIS2 Integer 256 Dimension 2
NAXIS3 Integer Ndet Dimension 3 = Number of detections
Keyword Data Type Value Description
PIPELINE String Name of detection pipeline
Extension 3: IMAGE, EXTNAME = PSZ2_MSZ_ARRAY (see note 3)
Keyword Data Type Value Description
NAXIS1 Integer 100 Dimension 1
NAXIS2 Integer 4 Dimension 2
NAXIS3 Integer Ndet Dimension 3 = Number of detections
Keyword Data Type Value Description
PIPELINE String Name of detection pipeline


Notes

  1. Format PSZ2 Glll.ll±bb.bb where (l, b) are the Galactic coordinates truncated to 2 decimal places.
  2. Extension 2 contains a three-dimensional image with the two-dimensional probability distribution in θs and Y for each detection. The probability distributions are evaluated on a 256 × 256 linear grid between the limits specified in extension 1. The limits are determined independently for each detection. The dimension of the 3D image is 256 × 256 × Ndet, where Ndet is the number of detections. The first dimension is θs and the second dimension is Y.
  3. Extension 3 contains a three-dimensional image with the information on the MSZ observable per cluster as a function of assumed redshift. The image dimensions are 100 × 4 × Ndet, where Ndet is the number of detections. The first dimension is the assumed redshift. The second dimension has size 4: the first element is the assumed redshift value corresponding to the MSZ values. The second element is the MSZ lower 68% confidence bound, the third element is the MSZ estimate and the fourth element is the MSZ upper 68% confidence bound, all in units of 1014 Msol. These uncertainties are based on the Planck measurement uncertainties only. Not included in the error estimates are the statistical errors on the scaling relation, the intrinsic scatter in the relation, or systematic errors in data selection for the scaling relation fit.

Selection function[edit]

The selection function for the union, intersection and individual pipeline catalogues are contained in the FITS files:

Their structure is as follows:

FITS file structure
Extension 0: Primary header, no data
FITS Keyword Data Type Units Description
INSTRUME String Instrument (HFI)
VERSION String Version of catalogue
DATE String Date file created: yyyy-mm-dd
ORIGIN String Name of organization responsible for the data (HFI-DPC)
TELESCOP String Telescope (PLANCK)
CREATOR String Pipeline version
DATE-OBS String Start time of the survey: yyyy-mm-dd
DATE-END String End time of the survey: yyyy-mm-dd
PROCVER String Data version
JOIN String Join type (UNION, INTERSEC, MMF1, MMF3, PwS)
MASK String Mask name (SURVEY, COSMOLOG)
Extension 1: BINTABLE, HEALPix map (see note 1)
FITS keyword Data Type Value Description
PIXTYPE String HEALPIX HEALPix pixelation
ORDERING String RING Pixel ordering
NSIDE Int*4 2048 HEALPix resolution parameter
NPIX Int*4 50331648 Number of pixels
COORDSYS String G Coordinate system
Extension 2: IMAGE, EXTNAME = SELFUNC (see note 2)
Keyword Data Type Value Description
NAXIS1 Integer 30 Dimension 1
NAXIS2 Integer 32 Dimension 2
NAXIS3 Integer 12 Dimension 3
Keyword Data Type Value Description
AXIS1 String CY500 Name of axis 1
AXIS2 String T500 Name of axis 2
AXIS3 String SNRCUT Name of axis 3
UNITS String PERCENT Units of selection function
COMPTYPE String DIFF Type of selection function (differential)
Extension 3: IMAGE, EXTNAME = YGRID (see note 3)
Keyword Data Type Value Description
NAXIS1 Integer 30 Dimension 1
Keyword Data Type Value Description
COL1 String CY500 Grid values of Y500
Extension 4: IMAGE, EXTNAME = TGRID (see note 4)
Keyword Data Type Value Description
NAXIS1 Integer 32 Dimension 1
Keyword Data Type Value Description
COL1 String T500 Grid values of θ500
Extension 5: IMAGE, EXTNAME = SNR_THRESH (see note 5)
Keyword Data Type Value Description
NAXIS1 Integer 12 Dimension 1
Keyword Data Type Value Description
COL1 String S/N Grid values of S/N threshold

Notes

  1. Extension 1 contains a mask defining the survey region, given by an Nside = 2048 ring-ordered HEALPix map in GALACTIC coordinates. Pixels in the survey region have the value 1.0 while pixels outside of the survey region have value 0.0.
  2. Extension 2 contains a three-dimensional image containing the survey completeness probability distribution for various S/N thresholds. The information is stored in an image of size 30 × 32 × 12. The first dimension is Y500, the second dimension is θ500 and the third dimension is the signal-to-noise threshold. The units are percent and lie in the range 0-100 and denote the detection probability of a cluster in the given (Y500, θ500) bin.
  3. Extension 3 contains the Y500 grid values for the completeness data cube in the second extension. It has length 30 and spans the range from 1.12480 × 10-4 arcmin2 to 7.20325 × 10-2 arcmin2 in logarithmic steps.
  4. Extension 4 contains the θ500 grid values for the completeness data cube in the second extension. It has length 32 and spans the range from 0.9416 arcmin to 35.31 arcmin in logarithmic steps.
  5. Extension 5 contains the signal-to-noise threshold grid values for the completeness data cube in the second extension. It has length 12 and contains thresholds from 4.5 to 10.0 in steps of 0.5.

Previous releases (PSZ1)[edit]

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

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

Three pipelines are used to detect SZ clusters: two independent implementations of the Matched Multi-Filter (MMF1 and MMF3), and PowellSnakes (PwS). The main catalogue is constructed as the union of the catalogues from the three detection methods. The individual catalogues are provided for the expert user in order to assess the consistency of the pipelines. The completeness and reliability of the catalogues have been assessed through internal and external validation as described in sections 3-6 of Planck-2013-XXIX[24].

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

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

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

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

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

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

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


Additional information

A set of comments on the union catalogue is available in

COM_DocPCCS_SZ-union-comments_R1.11.txt

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

COM_PCCS_SZ-validation_R1.12.fits

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

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

Notes

  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[27]
     2 : Databases NED and SIMBAD-CDS
     3 : SDSS cluster catalogue[28]
     4 : SDSS cluster catalogue[29]
     5 : SPT[30][31][32][33][34][35][36]
     6 : ACT[37][38][39][40]
     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.



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

Catalogue of Planck Galactic Cold Clumps[edit]

The catalogue of Planck Galactic Cold Clumps (PGCC) is a list of 13188 Galactic sources and 54 sources located in the Small and Large Magellanic Clouds, identified as cold sources in Planck data, as described in Planck-2015-A37[41]. The sources are extracted with the CoCoCoDeT algorithm (Montier, 2010), using Planck-HFI 857, 545, and 353 GHz maps and the 3 THz IRIS map (Miville 2005), an upgraded version of the IRAS data at 5 arcmin resolution. This is the first all-sky catalogue of Galactic cold sources obtained with homogeneous methods and data.

The CoCoCoDeT detection algorithm uses the 3 THz map as a spatial template of a warm background component. Local estimates of the average colour of the background are derived at 30 arcmin resolution around each pixel of the maps at 857, 545, and 353 GHz. Together these describe a local warm component that is subtracted, leaving 857, 545, and 353 GHz maps of the cold residual component map over the full sky. A point source detection algorithm is applied to these three maps. A detection requires S/N > 4 in pixels in all Planck bands and a minimum angular distance of 5 arcmin to other detections.

A 2D Gaussian fit provides an estimate of the position angle and FWHM size along the major and minor axes. The ellipse defined by the FWHM values is used in aperture photometry to derive the flux density estimates in all four bands. Based on the quality of the flux density estimates in all four bands, PGCC sources are divided into three categories of FLUX_QUALITY:

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

We also raise a flag on the blending between sources which can be used to quantify the reliability of the aperture photometry processing.

To estimate possible contamination by extragalactic sources we (1) cross-correlated the positions with catalogues of extragalactic sources, (2) rejected detections with SED [in colour-colour plots] consistent with radio sources, and (3) rejected detections with clear association to extragalactic sources visible in DSS images. Compared to the original number of sources, these only resulted in a small number of rejections.

Distance estimates, combining seven different methods, have been obtained for 5574 sources with estimates ranging from hundreds of pc in local molecular clouds up to 10.5 kpc along the Galactic plane. The methods include cross-correlation with kinematic distances previously listed for infrared dark clouds (IRDCs), optical and near-infrared extinction using SDSS and 2MASS data, respectively, association with molecular clouds with known distances, and finally referencing parallel work done on a small sample of sources followed up with Herschel. Most PGCC sources appear to be located in the solar neighbourhood.

The derived physical properties of the PGCC sources are: temperature, column density, physical size, mass, density and luminosity. PGCC sources exhibit an average temperature of about 14K, and ranging from 5.8 to 20K. They span a large range of physical properties (such as column density, mass and density) covering a large varety of objects, from dense cold cores to large molecular clouds.

The validation of this catalogue has been performed with a Monte Carlo Quality Assessment analysis wich allowed us to quantify the statistical reliability of the flux densities and of the source position and geometry estimates. The position accuracy is better than 0.2' and 0.8' for 68% and 95% of the sources, respectively, while the ellipticity of the sources is recovered with an accuracy better than 10% at 1[math]\sigma[/math]. This kind of analysis is also very powerful to characterize the selection function of the CoCoCoDeT algorithm applied to Planck data. The completeness of the detection has been studied as a function of the temperature of the injected sources. It has been shown that sources with FLUX_QUALITY=2 are effectively sources with low temperatures and have a high completeness level for temperatures below 10K.

We computed the cross-correlation between the PGCC catalogue and the other internal Planck catalogues: PCCS2, PCCS2E, PSZ and PHz. The PGCC catalogue contains about 45% new sources, not simultaneously detected in the 857, 545, and 353 GHz bands of the PCCS2 and PCCS2E. A few sources (65) are also detected in the PSZ2 and PGCC catalogues, suggesting a dusty nature of these candidates. Finally there are only 15 sources in common between the PGCC and PHz (which is focused on extragalactic sources at high redshift), that require further analysis to elucidate.

The PGCC catalogue contains also 54 sources located in the Small and Large Magellanic Clouds (SMC and LMC), two nearby galaxies which are so close that we can identify individual clumps in them.

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

All-sky distribution of the PGCC sources.

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

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

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

All-sky distribution of the PGCC sources with FLUX_QUALITY=1.
All-sky distribution of the PGCC sources with FLUX_QUALITY=2.
All-sky distribution of the PGCC sources with FLUX_QUALITY=3.

Distance estimates have been obtained on 5574 PGCC sources using seven different methods/technics, as described in Planck-2015-A28[41]. A flag is raised to quantify the quality of the distance estimates, defined as follows:

  • DIST_QUALITY=0 : No distance estimate ;
  • DIST_QUALITY=1 : Single distance estimate ;
  • DIST_QUALITY=2 : Multiple distance estimates which are consistent within 1[math]\sigma[/math] ;
  • DIST_QUALITY=3 : Multiple distance estimates which are not consistent within 1[math]\sigma[/math] ;
  • DIST_QUALITY=4 : Single upper limits.

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

All-sky distribution of the 4655 PGCC sources for which a distance estimate with a DIST_QUALITY flag equal to 1 or 2 is available. The various types of distance estimates are defined as follows : kinematic (purple), optical extinction (blue), near-infrared extinction (green), molecular complex association (orange), and Herschel HKP-GCC (red). We also show the distribution of the 664 sources with an upper-limit estimate (DIST_QUALITY=4) provided by the near-infrared extinction method (light green). Molecular complexes are outlined with black contours.

The catalogue is contained in the FITS file HFI_PCCS_GCC_R2.02.fits. It structure is as follows:

FITS file structure
Identification
FITS Keyword Data Type Units Description
NAME String Source Name
SNR real*8 Maximum S/N over the 857, 545, and 353 GHz Planck cold residual maps
SNR_857 real*8 S/N of the cold residual detection at 857 GHz
SNR_545 real*8 S/N of the cold residual detection at 545 GHz
SNR_353 real*8 S/N of the cold residual detection at 353 GHz
Source position
FITS Keyword Data Type Units Description
GLON real*8 deg Galactic longitude based on morphology fitting
GLAT real*8 deg Galactic latitude based on morphology fitting
RA real*8 deg Right ascension (J2000) in degrees transformed from (GLON, GLAT)
DEC real*8 deg Declination (J2000) in degrees transformed from (GLON, GLAT)
Morphology
FITS Keyword Data Type Units Description
GAU_MAJOR_AXIS real*8 arcmin FWHM along the major axis of the elliptical Gaussian
GAU_MAJOR_AXIS_SIG real*8 arcmin 1[math]\sigma[/math] uncertainty on the FWHM along the major axis
GAU_MINOR_AXIS real*8 arcmin FWHM along the minor axis of the elliptical Gaussian
GAU_MINOR_AXIS_SIG real*8 arcmin 1[math]\sigma[/math] uncertainty on the FWHM along the minor axis
GAU_POSITION_ANGLE real*8 rad Position angle of the elliptical gaussian (see note 1)
GAU_POSITION_ANGLE_SIG real*8 rad 1[math]\sigma[/math] uncertainty on the position angle
Photometry
FITS Keyword Data Type Units Description
FLUX_3000_CLUMP real*8 Jy Flux density of the clump at 3 THz
FLUX_3000_CLUMP_SIG real*8 Jy 1[math]\sigma[/math] uncertainty on the flux density of the clump at 3 THz
FLUX_857_CLUMP real*8 Jy Flux density of the clump at 857 GHz
FLUX_857_CLUMP_SIG real*8 Jy 1[math]\sigma[/math] uncertainty on the flux density of the clump at 857 GHz
FLUX_545_CLUMP real*8 Jy Flux density of the clump at 545 GHz
FLUX_545_CLUMP_SIG real*8 Jy 1[math]\sigma[/math] uncertainty on the flux density of the clump at 545 GHz
FLUX_353_CLUMP real*8 Jy Flux density of the clump at 353 GHz
FLUX_353_CLUMP_SIG real*8 Jy 1[math]\sigma[/math] uncertainty on the flux density of the clump at 353 GHz
FLUX_3000_WBKG real*8 Jy Flux density of the warm background at 3 THz (see note 2)
FLUX_3000_WBKG_SIG real*8 Jy 1[math]\sigma[/math] uncertainty on the flux density of warm background at 3 THz
FLUX_857_WBKG real*8 Jy Flux density of the warm background at 857 GHz
FLUX_857_WBKG_SIG real*8 Jy 1[math]\sigma[/math] uncertainty on the flux density of the warm background at 857 GHz
FLUX_545_WBKG real*8 Jy Flux density of the warm background at 545 GHz
FLUX_545_WBKG_SIG real*8 Jy 1[math]\sigma[/math] uncertainty on the flux density of the warm background at 545 GHz
FLUX_353_WBKG real*8 Jy Flux density of the warm background at 353 GHz
FLUX_353_WBKG_SIG real*8 Jy 1[math]\sigma[/math] uncertainty on the flux density of the warm background at 353 GHz
FLUX_QUALITY int*4 1-3 Category of flux density reliability (see note 3)
FLUX_BLENDING int*4 0/1 1 if blending issue with flux density estimate (see note 4)
FLUX_BLENDING_IDX int*8 Catalogue index of the closest source responsible for blending
FLUX_BLENDING_ANG_DIST real*8 arcmin Angular distance to the closest source responsible for blending
FLUX_BLENDING_BIAS_3000 real*8 % Relative bias of the flux density at 3000 GHz due to blending
FLUX_BLENDING_BIAS_857 real*8 % Relative bias of the flux density at 857 GHz due to blending
FLUX_BLENDING_BIAS_545 real*8 % Relative bias of the flux density at 545 GHz due to blending
FLUX_BLENDING_BIAS_353 real*8 % Relative bias of the flux density at 353 GHz due to blending
Distance
FITS Keyword Data Type Units Description
DIST_KINEMATIC real*8 kpc Distance estimate [1] using kinematics
DIST_KINEMATIC_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [1] using kinematics
DIST_OPT_EXT_DR7 real*8 kpc Distance estimate [2] using optical extinction on SDSS DR7
DIST_OPT_EXT_DR7_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [2] using optical extinction on SDSS DR7
DIST_OPT_EXT_DR9 real*8 kpc Distance estimate [3] using optical extinction on SDSS DR9
DIST_OPT_EXT_DR9_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [3] using optical extinction on SDSS DR9
DIST_NIR_EXT_IRDC real*8 kpc Distance estimate [4] using near-infrared extinction towards IRDCs
DIST_NIR_EXT_IRDC_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [4] using near-infrared extinction towards IRDCs
DIST_NIR_EXT real*8 kpc Distance estimate [5] using near-infrared extinction
DIST_NIR_EXT_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [5] using near-infrared extinction
DIST_MOLECULAR_COMPLEX real*8 kpc Distance estimate [6] using molecular complex association
DIST_MOLECULAR_COMPLEX_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [6] using molecular complex association
DIST_HKP_GCC real*8 kpc Distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
DIST_HKP_GCC_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
DIST_OPTION int*4 0-7 Option of the best distance estimate used in other physical properties
DIST_QUALITY int*4 0-4 Quality Flag of the consistency between distance estimates (see note 5)
DIST real*8 kpc Best distance estimate used for further physical properties
DIST_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the best distance estimate
Temperature
FITS Keyword Data Type Units Description
TEMP_CLUMP real*8 K Temperature of the clump with [math]\beta[/math] as a free parameter
TEMP_CLUMP_SIG real*8 K 1[math]\sigma[/math] uncertainty on the clump temperature with [math]\beta[/math] free
TEMP_CLUMP_LOW1 real*8 K Lower 68% confidence limit of the clump temperature with [math]\beta[/math] free
TEMP_CLUMP_UP1 real*8 K Upper 68% confidence limit of the clump temperature with [math]\beta[/math] free
BETA_CLUMP real*8 Spectral index [math]\beta[/math] of the clump
BETA_CLUMP_SIG real*8 1[math]\sigma[/math] uncertainty (from MCMC) on the emissivity spectral index [math]\beta[/math] of the clump
BETA_CLUMP_LOW1 real*8 Lower 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the clump
BETA_CLUMP_UP1 real*8 Upper 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the clump
TEMP_BETA2_CLUMP real*8 K Temperature of the clump with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_SIG real*8 K 1[math]\sigma[/math] uncertainty on the temperature of the clump with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_LOW1 real*8 K Lower 68% confidence limit of the clump temperature with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_UP1 real*8 K Upper 68% confidence limit of the clump temperature with [math]\beta[/math] = 2
TEMP_WBKG real*8 K Temperature of the warm background with [math]\beta[/math] as a free parameter (see note 6)
TEMP_WBKG_SIG real*8 K 1[math]\sigma[/math] dispersion of the warm background temperature with [math]\beta[/math] free
TEMP_WBKG_LOW1 real*8 K Lower 68% confidence limit of the warm background temperature with [math]\beta[/math] free
TEMP_WBKG_UP1 real*8 K Upper 68% confidence limit of the warm background temperature with [math]\beta[/math] free
BETA_WBKG real*8 Spectral index [math]\beta[/math] of the warm background (see note 6)
BETA_WBKG_SIG real*8 1[math]\sigma[/math] uncertainty (from MCMC) of the emissivity spectral index [math]\beta[/math] of the warm background
BETA_WBKG_LOW1 real*8 Lower 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the warm background
BETA_WBKG_UP1 real*8 Upper 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the warm background
TEMP_BETA2_WBKG real*8 K Temperature of the warm background with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_SIG real*8 K 1[math]\sigma[/math] uncertainty on the temperature of the warm background with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_LOW1 real*8 K Lower 68% confidence limit of the warm background temperature with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_UP1 real*8 K Upper 68% confidence limit of the warm background temperature with [math]\beta[/math] = 2
Physical properties
FITS Keyword Data Type Units Description
NH2 real*8 cm-2 Column density [math]N_{H_2}[/math] of the clump
NH2_SIG real*8 cm-2 1[math]\sigma[/math] uncertainty on the column density
NH2_LOW[1,2,3] real*8 cm-2 Lower 68%, 95% and 99% confidence limit of the column density
NH2_UP[1,2,3] real*8 cm-2 Upper 68%, 95% and 99% confidence limit of the column density
MASS real*8 [math]M_{o}[/math] Mass estimate of the clump
MASS_SIG real*8 [math]M_{o}[/math] 1[math]\sigma[/math] uncertainty on the mass estimate of the clump
MASS_LOW[1,2,3] real*8 [math]M_{o}[/math] Lower 68%, 95% and 99% confidence limit of the mass estimate
MASS_UP[1,2,3] real*8 [math]M_{0}[/math] Upper 68%, 95% and 99% confidence limit of the mass estimate
DENSITY real*8 cm-3 Mean density of the clump
DENSITY_SIG real*8 cm-3 1[math]\sigma[/math] uncertainty on the mean density estimate of the clump
DENSITY_LOW[1,2,3] real*8 cm-3 Lower 68%, 95% and 99% confidence limit of the mean density estimate
DENSITY_UP[1,2,3] real*8 cm-3 Upper 68%, 95% and 99% confidence limit of the mean density estimate
SIZE real*8 pc Physical size of the clump
SIZE_SIG real*8 pc 1[math]\sigma[/math] uncertainty on the physical size estimate of the clump
SIZE_LOW[1,2,3] real*8 pc Lower 68%, 95% and 99% confidence limit of the physical size estimate
SIZE_UP[1,2,3] real*8 pc Upper 68%, 95% and 99% confidence limit of the physical size estimate
LUMINOSITY real*8 Lo Luminosity of the clump
LUMINOSITY_SIG real*8 Lo 1[math]\sigma[/math] uncertainty on the luminosity estimate of the clump
LUMINOSITY_LOW[1,2,3] real*8 Lo Lower 68%, 95% and 99% confidence limit of the luminosity estimate
LUMINOSITY_UP[1,2,3] real*8 Lo Upper 68%, 95% and 99% confidence limit of the luminosity estimate
Flags
FITS Keyword Data Type Units Description
XFLAG_LMC int*4 0/1 1 if part of the LMC
XFLAG_SMC int*4 0/1 1 if part of the SMC
XFLAG_ECC int*4 0/1 1 if present in the ECC
XFLAG_PCCS_857 int*4 0/1 1 if present in the PCCS 857 GHz band
XFLAG_PCCS_545 int*4 0/1 1 if present in the PCCS 545 GHz band
XFLAG_PCCS_353 int*4 0/1 1 if present in the PCCS 353 GHz band
XFLAG_PCCS_217 int*4 0/1 1 if present in the PCCS 217 GHz band
XFLAG_PCCS_143 int*4 0/1 1 if present in the PCCS 143 GHz band
XFLAG_PCCS_100 int*4 0/1 1 if present in the PCCS 100 GHz band
XFLAG_PCCS_70 int*4 0/1 1 if present in the PCCS 70 GHz band
XFLAG_PCCS_44 int*4 0/1 1 if present in the PCCS 44 GHz band
XFLAG_PCCS_30 int*4 0/1 1 if present in the PCCS 30 GHz band
XFLAG_PSZ int*4 0/1 1 if present in the PCCS PSZ
XFLAG_PHZ int*4 0/1 1 if present in the PCCS HZ
XFLAG_HKP_GCC int*4 0/1 1 if present in the Herschel HKP-GCC


Notes:

  • 1: The position angle of the 2D ellipse is defined as the angle between the axis parallele to the Galactic plane and the major axis, counted clockwise.
  • 2: The warm bakcground flux densities are computed using the same solid angle as for the clumps flux densities, but on the warm conponent map.
  • 3: See text above for a full description of the FLUX_QUALITY flag, for which 1 is best.
  • 4: This relative bias due to blending provides a rough estimate of the factor that should be applied on the clumpds flux densities to get a corrected estimate. It has been obtained on a very simple modelling of clumps morphology and the local environment. It has therefore to be taken very carefully.
  • 5: See text above for a full description of the DIST_QUALITY flag.
  • 6: Temperature and spectral index of the warm background are based on the warm background flux density estimates obtained on the same solid angle used for clumps


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

The Planck list of high-redshift source candidates (PHZ) is a list of 2151 sources located in the cleanest 26% of the sky and identified as point sources exhibiting an excess in the submillimeter compared to their environment. It has been built using the 48 months Planck data at 857, 545, 353 and 217 GHz combined with the 3 THz IRAS data, as it is described in [42]. These sources are considered as high-z source candidates (z>1.5-2), given the very low contamination by Galactic cirrus.


FITS file structure
Identification
FITS Keyword Data Type Units Description
NAME String Source Name
SNR_X545 real*8 S/N in the 545 GHz excess map
SNR_D857 real*8 S/N in the 857 GHz cleaned map
SNR_D545 real*8 S/N in the 545 GHz cleaned map
SNR_D353 real*8 S/N in the 353 GHz cleaned map
Source position
FITS Keyword Data Type Units Description
GLON real*8 deg Galactic longitude based on morphology fitting
GLAT real*8 deg Galactic latitude based on morphology fitting
RA real*8 deg Right ascension (J2000) in degrees transformed from (GLON, GLAT)
DEC real*8 deg Declination (J2000) in degrees transformed from (GLON, GLAT)
Morphology
FITS Keyword Data Type Units Description
GAU_MAJOR_AXIS real*8 arcmin FWHM along the major axis of the elliptical Gaussian
GAU_MAJOR_AXIS_SIG real*8 arcmin 1[math]\sigma[/math] uncertainty on the FWHM along the major axis
GAU_MINOR_AXIS real*8 arcmin FWHM along the minor axis of the elliptical Gaussian
GAU_MINOR_AXIS_SIG real*8 arcmin 1[math]\sigma[/math] uncertainty on the FWHM along the minor axis
GAU_POSITION_ANGLE real*8 rad Position angle of the elliptical gaussian (see note 1)
GAU_POSITION_ANGLE_SIG real*8 rad 1[math]\sigma[/math] uncertainty on the position angle
Photometry
FITS Keyword Data Type Units Description
FLUX_CLEAN_857 real*8 Jy Flux density of the clump at 857 GHz
FLUX_CLEAN_857_SIG_SKY real*8 Jy 1[math]\sigma[/math] uncertainty at 857 GHz due to sky confusion
FLUX_CLEAN_857_SIG_DATA real*8 Jy 1[math]\sigma[/math] uncertainty at 857 GHz due to measurement error
FLUX_CLEAN_857_SIG_GEOM real*8 Jy 1[math]\sigma[/math] uncertainty at 857 GHz due to elliptical Gaussian fit accuracy
FLUX_CLEAN_545 real*8 Jy Flux density of the clump at 545 GHz
FLUX_CLEAN_545_SIG_SKY real*8 Jy 1[math]\sigma[/math] uncertainty at 545 GHz due to sky confusion
FLUX_CLEAN_545_SIG_DATA real*8 Jy 1[math]\sigma[/math] uncertainty at 545 GHz due to measurement error
FLUX_CLEAN_545_SIG_GEOM real*8 Jy 1[math]\sigma[/math] uncertainty at 545 GHz due to elliptical Gaussian fit accuracy
FLUX_CLEAN_353 real*8 Jy Flux density of the clump at 353 GHz
FLUX_CLEAN_353_SIG_SKY real*8 Jy 1[math]\sigma[/math] uncertainty at 353 GHz due to sky confusion
FLUX_CLEAN_353_SIG_DATA real*8 Jy 1[math]\sigma[/math] uncertainty at 353 GHz due to measurement error
FLUX_CLEAN_353_SIG_GEOM real*8 Jy 1[math]\sigma[/math] uncertainty at 353 GHz due to elliptical Gaussian fit accuracy
FLUX_CLEAN_217 real*8 Jy Flux density of the clump at 217 GHz
FLUX_CLEAN_217_SIG_SKY real*8 Jy 1[math]\sigma[/math] uncertainty at 217 GHz due to sky confusion
FLUX_CLEAN_217_SIG_DATA real*8 Jy 1[math]\sigma[/math] uncertainty at 217 GHz due to measurement error
FLUX_CLEAN_217_SIG_GEOM real*8 Jy 1[math]\sigma[/math] uncertainty at 217 GHz due to elliptical Gaussian fit accuracy
Distance
FITS Keyword Data Type Units Description
DIST_KINEMATIC real*8 kpc Distance estimate [1] using kinematics
DIST_KINEMATIC_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [1] using kinematics
DIST_OPT_EXT_DR7 real*8 kpc Distance estimate [2] using optical extinction on SDSS DR7
DIST_OPT_EXT_DR7_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [2] using optical extinction on SDSS DR7
DIST_OPT_EXT_DR9 real*8 kpc Distance estimate [3] using optical extinction on SDSS DR9
DIST_OPT_EXT_DR9_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [3] using optical extinction on SDSS DR9
DIST_NIR_EXT_IRDC real*8 kpc Distance estimate [4] using near-infrared extinction towards IRDCs
DIST_NIR_EXT_IRDC_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [4] using near-infrared extinction towards IRDCs
DIST_NIR_EXT real*8 kpc Distance estimate [5] using near-infrared extinction
DIST_NIR_EXT_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [5] using near-infrared extinction
DIST_MOLECULAR_COMPLEX real*8 kpc Distance estimate [6] using molecular complex association
DIST_MOLECULAR_COMPLEX_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [6] using molecular complex association
DIST_HKP_GCC real*8 kpc Distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
DIST_HKP_GCC_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the distance estimate [7] from the Herschel Key-Programme Galactic Cold Cores
DIST_OPTION int*4 0-7 Option of the best distance estimate used in other physical properties
DIST_QUALITY int*4 0-4 Quality Flag of the consistency between distance estimates (see note 5)
DIST real*8 kpc Best distance estimate used for further physical properties
DIST_SIG real*8 kpc 1[math]\sigma[/math] uncertainty on the best distance estimate
Temperature
FITS Keyword Data Type Units Description
TEMP_CLUMP real*8 K Temperature of the clump with [math]\beta[/math] as a free parameter
TEMP_CLUMP_SIG real*8 K 1[math]\sigma[/math] uncertainty on the clump temperature with [math]\beta[/math] free
TEMP_CLUMP_LOW1 real*8 K Lower 68% confidence limit of the clump temperature with [math]\beta[/math] free
TEMP_CLUMP_UP1 real*8 K Upper 68% confidence limit of the clump temperature with [math]\beta[/math] free
BETA_CLUMP real*8 Spectral index [math]\beta[/math] of the clump
BETA_CLUMP_SIG real*8 1[math]\sigma[/math] uncertainty (from MCMC) on the emissivity spectral index [math]\beta[/math] of the clump
BETA_CLUMP_LOW1 real*8 Lower 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the clump
BETA_CLUMP_UP1 real*8 Upper 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the clump
TEMP_BETA2_CLUMP real*8 K Temperature of the clump with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_SIG real*8 K 1[math]\sigma[/math] uncertainty on the temperature of the clump with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_LOW1 real*8 K Lower 68% confidence limit of the clump temperature with [math]\beta[/math] = 2
TEMP_BETA2_CLUMP_UP1 real*8 K Upper 68% confidence limit of the clump temperature with [math]\beta[/math] = 2
TEMP_WBKG real*8 K Temperature of the warm background with [math]\beta[/math] as a free parameter (see note 6)
TEMP_WBKG_SIG real*8 K 1[math]\sigma[/math] dispersion of the warm background temperature with [math]\beta[/math] free
TEMP_WBKG_LOW1 real*8 K Lower 68% confidence limit of the warm background temperature with [math]\beta[/math] free
TEMP_WBKG_UP1 real*8 K Upper 68% confidence limit of the warm background temperature with [math]\beta[/math] free
BETA_WBKG real*8 Spectral index [math]\beta[/math] of the warm background (see note 6)
BETA_WBKG_SIG real*8 1[math]\sigma[/math] uncertainty (from MCMC) of the emissivity spectral index [math]\beta[/math] of the warm background
BETA_WBKG_LOW1 real*8 Lower 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the warm background
BETA_WBKG_UP1 real*8 Upper 68% confidence limit of the emissivity spectral index [math]\beta[/math] of the warm background
TEMP_BETA2_WBKG real*8 K Temperature of the warm background with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_SIG real*8 K 1[math]\sigma[/math] uncertainty on the temperature of the warm background with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_LOW1 real*8 K Lower 68% confidence limit of the warm background temperature with [math]\beta[/math] = 2
TEMP_BETA2_WBKG_UP1 real*8 K Upper 68% confidence limit of the warm background temperature with [math]\beta[/math] = 2
Physical properties
FITS Keyword Data Type Units Description
NH2 real*8 cm-2 Column density [math]N_{H_2}[/math] of the clump
NH2_SIG real*8 cm-2 1[math]\sigma[/math] uncertainty on the column density
NH2_LOW[1,2,3] real*8 cm-2 Lower 68%, 95% and 99% confidence limit of the column density
NH2_UP[1,2,3] real*8 cm-2 Upper 68%, 95% and 99% confidence limit of the column density
MASS real*8 [math]M_{o}[/math] Mass estimate of the clump
MASS_SIG real*8 [math]M_{o}[/math] 1[math]\sigma[/math] uncertainty on the mass estimate of the clump
MASS_LOW[1,2,3] real*8 [math]M_{o}[/math] Lower 68%, 95% and 99% confidence limit of the mass estimate
MASS_UP[1,2,3] real*8 [math]M_{0}[/math] Upper 68%, 95% and 99% confidence limit of the mass estimate
DENSITY real*8 cm-3 Mean density of the clump
DENSITY_SIG real*8 cm-3 1[math]\sigma[/math] uncertainty on the mean density estimate of the clump
DENSITY_LOW[1,2,3] real*8 cm-3 Lower 68%, 95% and 99% confidence limit of the mean density estimate
DENSITY_UP[1,2,3] real*8 cm-3 Upper 68%, 95% and 99% confidence limit of the mean density estimate
SIZE real*8 pc Physical size of the clump
SIZE_SIG real*8 pc 1[math]\sigma[/math] uncertainty on the physical size estimate of the clump
SIZE_LOW[1,2,3] real*8 pc Lower 68%, 95% and 99% confidence limit of the physical size estimate
SIZE_UP[1,2,3] real*8 pc Upper 68%, 95% and 99% confidence limit of the physical size estimate
LUMINOSITY real*8 Lo Luminosity of the clump
LUMINOSITY_SIG real*8 Lo 1[math]\sigma[/math] uncertainty on the luminosity estimate of the clump
LUMINOSITY_LOW[1,2,3] real*8 Lo Lower 68%, 95% and 99% confidence limit of the luminosity estimate
LUMINOSITY_UP[1,2,3] real*8 Lo Upper 68%, 95% and 99% confidence limit of the luminosity estimate
Flags
FITS Keyword Data Type Units Description
XFLAG_LMC int*4 0/1 1 if part of the LMC
XFLAG_SMC int*4 0/1 1 if part of the SMC
XFLAG_ECC int*4 0/1 1 if present in the ECC
XFLAG_PCCS_857 int*4 0/1 1 if present in the PCCS 857 GHz band
XFLAG_PCCS_545 int*4 0/1 1 if present in the PCCS 545 GHz band
XFLAG_PCCS_353 int*4 0/1 1 if present in the PCCS 353 GHz band
XFLAG_PCCS_217 int*4 0/1 1 if present in the PCCS 217 GHz band
XFLAG_PCCS_143 int*4 0/1 1 if present in the PCCS 143 GHz band
XFLAG_PCCS_100 int*4 0/1 1 if present in the PCCS 100 GHz band
XFLAG_PCCS_70 int*4 0/1 1 if present in the PCCS 70 GHz band
XFLAG_PCCS_44 int*4 0/1 1 if present in the PCCS 44 GHz band
XFLAG_PCCS_30 int*4 0/1 1 if present in the PCCS 30 GHz band
XFLAG_PSZ int*4 0/1 1 if present in the PCCS PSZ
XFLAG_PHZ int*4 0/1 1 if present in the PCCS HZ
XFLAG_HKP_GCC int*4 0/1 1 if present in the Herschel HKP-GCC


References[edit]

  1. ↑ 1.01.11.21.31.4 Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources, Planck Collaboration, 2014, A&A, 571, A28.
  2. ↑ 2.02.12.22.3 Planck 2015 results. XXVI. The second Planck catalogue of compact sources, Planck Collaboration, 2016, A&A, 594, A26.
  3. ↑ The Mexican hat wavelet family: application to point-source detection in cosmic microwave background maps, J. González-Nuevo, F. L. Argüeso, M. López-Caniego, MNRAS, 369, 1603-1610, (2009).
  4. ↑ Comparison of filters for the detection of point sources in Planck simulations, M. López-Caniego,D. Herranz, J. González-Nuevo, J. L. Sanz, R. B. Barreiro, P. Vielva, F. Argüeso, L. Toffolatti, MNRAS, 370, 2047-2063, (2006).
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  6. ↑ A fast Bayesian approach to discrete object detection in astronomical data sets - PowellSnakes I, P. Carvalho, G. Rocha, M. P. Hobson, MNRAS, 393, 681-702, (2009).
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  13. ↑ 13.013.113.2 Planck 2013 results. VI. High Frequency Instrument Data Processing, Planck Collaboration, 2014, A&A, 571, A6.
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  17. ↑ Planck 2013 results. VII. HFI time response and beams, Planck Collaboration, 2014, A&A, 571, A7.
  18. ↑ 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).
  19. ↑ 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).
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  25. ↑ 25.025.1 Planck 2015 results. XXVII. The second Planck catalogue of Sunyaev-Zeldovich sources, Planck Collaboration, 2016, A&A, 594, A27.
  26. ↑ The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and the Y_SZ - M_500 relation, M. Arnaud, G. W. Pratt, R. Piffaretti, H. Böhringer, J. H. Croston, E. Pointecouteau, ApJ, 517, A92, (2010).
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  29. ↑ 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).
  30. ↑ 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).
  31. ↑ 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).
  32. ↑ 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).
  33. ↑ 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).
  34. ↑ 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).
  35. ↑ 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).
  36. ↑ 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).
  37. ↑ 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).
  38. ↑ 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).
  39. ↑ 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).
  40. ↑ 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).
  41. ↑ 41.041.1 Planck 2015 results. XXVIII. The Planck catalogue of Galactic cold clumps, Planck Collaboration, 2016, A&A, 594, A28.
  42. ↑

(Planck) Low Frequency Instrument

(Planck) High Frequency Instrument

Data Processing Center

Early Release Compact Source Catalog

Full-Width-at-Half-Maximum

Flexible Image Transfer Specification

(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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