PLANCKGCC - Planck Catalog of Galactic Cold Clumps (PGCC)

Overview

The authors present the Planck Catalog of Galactic Cold Clumps (PGCC), an all-sky catalog of Galactic cold clump candidates detected by Planck. This catalog is the full version of the Early Cold Core (ECC) catalog, which was made available in 2011 with the Early Release Compact Source Catalog (ERCSC) and which contained 915 high signal-to-noise sources. It is based on the Planck 48-month mission data that are currently being released to the astronomical community. The PGCC catalog is an observational catalog consisting exclusively of Galactic cold sources. The three highest Planck bands (857, 454, and 353GHz) have been combined with IRAS data at 3THz to perform a multi-frequency detection of sources colder than their local environment. After rejection of possible extragalactic contaminants, the PGCC catalog contains 13188 Galactic sources spread across the whole sky, i.e., from the Galactic plane to high latitudes, following the spatial distribution of the main molecular cloud complexes. The median temperature of PGCC sources lies between 13 and 14.5K, depending on the quality of the flux density measurements, with a temperature ranging from 5.8 to 20K after removing the sources with the top 1% highest temperature estimates. Using seven independent methods, reliable distance estimates have been obtained for 5574 sources, which allows the authors to derive their physical properties such as their mass, physical size, mean density, and luminosity. The PGCC sources are located mainly in the solar neighborhood, but also up to a distance of 10.5kpc in the direction of the Galactic center, and range from low-mass cores to large molecular clouds. Because of this diversity and because the PGCC catalog contains sources in very different environments, the catalog is useful for investigating the evolution from molecular clouds to cores. Finally, it also includes 54 additional sources located in the Small and Large Magellanic Clouds.

This catalog is based on three highest Planck frequency channels (i.e., 857, 545, 353 GHz), which are designed to cover the Galactic cold dust emission peak. The 217 GHz band is not included for two reasons: first, the band is contaminated by the CO J=2->1 emission line, which is expected to be significant towards dense regions; second, the contamination by the cosmic microwave background may become problematic at high latitude.

The Planck data are combined with the IRIS all-sky data (Miville-Deschenes & Lagache 2005). The IRIS 3THz (100{mu}m) data were chosen to complement the Planck data because it is a good tracer of Galactic warm (~20 K) dust, among other reasons provided in the paper.

Catalog Bibcode

2016A&A...594A..28P

References

Planck 2015 results. XXVIII. The Planck Catalogue of Galactic cold clumps.
    Planck collaboration
    Ade P.A.R., Aghanim N., Arnaud M., Ashdown M., Aumont J., Baccigalupi C.,
    Banday A.J., Barreiro R.B., Bartolo N., Battaner E., Benabed K., Benoit A.,
    Benoit-Levy A., Bernard J.-P., Bersanelli M., Bielewicz P., Bonaldi A.,
    Bonavera L., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M.,
    Burigana C., Butler R.C., Calabrese E., Catalano A., Chamballu A.,
    Chiang H.C., Christensen P.R., Clements D.L., Colombi S., Colombo L.P.L.,
    Combet C., Couchot F., Coulais A., Crill B.P., Curto A., Cuttaia F.,
    Danese L., Davies R.D., Davis R.J., de Bernardis P., de Rosa A.,
    de Zotti G., Delabrouille J., Desert F.-X., Dickinson C., Diego J.M.,
    Dole H., Donzelli S., Dore O., Douspis M., Ducout A., Dupac X.,
    Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Falgarone E.,
    Fergusson J., Fergusson J., Finelli F., Forni O., Frailis M., Fraisse A.A.,
    Franceschi E., Frejsel A., Galeotta S., Galli S., Ganga K., Giard M.,
    Giraud-Heraud Y., Gjerlow E., Gonzalez-Nuevo J., Gorski K.M., Gratton S.,
    Gregorio A., Gruppuso A., Gudmundsson J.E., Hansen F.K., Hanson D.,
    Harrison D.L., Helou G., Henrot-Versille S., Hernandez-Monteagudo C.,
    Herranz D., Hildebrandt S.R., Hivon E., Hobson M., Holmes W.A.,
    Hornstrup A., Hovest W., Huffenberger K.M., Hurier G., Jaffe A.H.,
    Jaffe T.R., Jones W.C., Juvela M., Keihanen E., Keskitalo R., Kisner T.S.,
    Knoche J., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A.,
    Lattanzi M., Lawrence C.R., Leonardi R., Lesgourgues J., Levrier F.,
    Liguori M., Lilje P.B., Linden-Vornle M., Lopez-Caniego M., Lubin P.M.,
    Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A.,
    Marshall D.J., Martin P.G., Martinez-Gonzalez E., Masi S., Matarrese S.,
    Mazzotta P., McGehee P., Melchiorri A., Mendes L., Mennella A.,
    Migliaccio M., Mitra S., Miville-Deschenes M.-A., Moneti A., Montier L.,
    Morgante G., Mortlock D., Moss A., Munshi D., Murphy J.A., Naselsky P.,
    Nati F., Natoli P., Netterfield C.B., Norgaard-Nielsen H.U., Noviello F.,
    Novikov D., Novikov I., Oxborrow C.A., Paci F., Pagano L., Pajot F.,
    Paladini R., Paoletti D., Pasian F., Patanchon G., Pearson T.J.,
    Pelkonen V.-M., Perdereau O., Perotto L., Perrotta F., Pettorino V.,
    Piacentini F., Piat M., Pierpaoli E., Pietrobon D., Plaszczynski S.,
    Pointecouteau E., Polenta G., Pratt G.W., Prezeau G., Prunet S.,
    Puget J.-L., Rachen J.P., Reach W.T., Rebolo R., Reinecke M.,
    Remazeilles M., Renault C., Renzi A., Ristorcelli I., Rocha G., Rosset C.,
    Rossetti M., Roudier G., Rubino-Martin J.A., Rusholme B., Sandri M.,
    Santos D., Savelainen M., Savini G., Scott D., Seiffert M.D.,
    Shellard E.P.S., Spencer L.D., Stolyarov V., Sudiwala R., Sunyaev R.,
    Sutton D., Suur-Uski A.-S., Sygnet J.-F., Tauber J.A., Terenzi L.,
    Toffolatti L., Tomasi M., Tristram M., Tucci M., Tuovinen J., Umana G.,
    Valenziano L., Valiviita J., Van Tent B., Vielva P., Villa F., Wade L.A.,
    Wandelt B.D., Wehus I.K., Yvon D., Zacchei A., Zonca A.
   <Astron. Astrophys. 594, A28 (2016)>
   =2016A&A...594A..28P    (SIMBAD/NED BibCode)

Provenance

This table was created by the HEASARC in March 2019 based upon the CDS Catalog J/A+A/594/A28 file pgcc.dat.

Parameters

Name
The source designation.

RA
The Right Ascension of the GCC source in the selected equinox. The position was based on morphology fitting.

Dec
The Declination of the GCC source in the selected equinox. The position was based on morphology fitting.

LII
The Galactic longitude of the GCC source in the selected equinox. The position was based on morphology fitting.

BII
The Galactic latitude of the GCC source in the selected equinox. The position was based on morphology fitting.

SNR
The maximum signal-to-noise ratio over 857, 545, 353 GHz Planck cold residual maps. The cold residual maps are built by subtracting a warm component from each frequency map and described in detail in the paper and related Planck Collaboration XXIII (2011) paper. In these maps, cold sources show a positive signal, having a lower temperature than the local background. In some cases, the sources are not cold but are located in a region with warmer backgrounds (or foregrounds), such as along the line-of-sight with an active star forming region.

SNR_857_GHz
The signal-to-noise ratio based on the 857 GHz Planck cold residual map. The cold residual map is built by subtracting a warm component from this frequency map and described in detail in the paper and related Planck Collaboration XXIII (2011) paper. In the map, cold sources show a positive signal, having a lower temperature than the local background. In some cases, the sources are not cold but are located in a region with warmer backgrounds (or foregrounds), such as along the line-of-sight with an active star forming region.

SNR_545_GHz
The signal-to-noise ratio based on the 545 GHz Planck cold residual map. The cold residual map is built by subtracting a warm component from this frequency map and described in detail in the paper and related Planck Collaboration XXIII (2011) paper. In the map, cold sources show a positive signal, having a lower temperature than the local background. In some cases, the sources are not cold but are located in a region with warmer backgrounds (or foregrounds), such as along the line-of-sight with an active star forming region.

SNR_353_GHz
The signal-to-noise ratio based on the 353 GHz Planck cold residual map. The cold residual map is built by subtracting a warm component from this frequency map and described in detail in the paper and related Planck Collaboration XXIII (2011) paper. In the map, cold sources show a positive signal, having a lower temperature than the local background. In some cases, the sources are not cold but are located in a region with warmer backgrounds (or foregrounds), such as along the line-of-sight with an active star forming region.

Major_Axis
The major axis based on the FWHM of the elliptical Gaussian fit of the 857 GHz over the 3 THz color ratio map at the location where the snr_857_ghz is the highest .

Major_Axis_Error
The 1-sigma uncertainty on major_axis, which is based on the elliptical Gaussian fit of the 857 GHz over the 3 THz color ratio map at the location where the snr_857_ghz is the highest.

Minor_Axis
The minor axis based on the FWHM of the elliptical Gaussian fit of the 857 GHz over the 3 THz color ratio map at the location where the snr_857_ghz is the highest.

Minor_Axis_Error
The 1-sigma uncertainty on minor_axis, which is based on the elliptical Gaussian fit of the 857 GHz over the 3 THz color ratio map at the location where the snr_857_ghz is the highest.

Position_Angle
The position angle of the elliptical Gaussian, defined as the clockwise angle between the Galactic plane orientation and the orientation of the major axis (converted by the HEASARC to degrees from the radian units used in the original table).

Position_Angle_Error
The 1-sigma uncertainty on position_angle (converted by the HEASARC to degrees from the radian units used in the original table).

Flux_3000_GHz
The flux density of the clump at 3 THz (converted by the HEASARC to mJy from Jy units in the original table). This is the flux density measured within the elliptical Gaussian fit (given by major_axis, minor_axis and position_angle).

Flux_3000_GHz_Error
The 1-sigma uncertainty on the flux density of the clump at 3 THz (converted by the HEASARC to mJy from Jy units in the original table).

Flux_857_GHz
The flux density of the clump at 857 GHz (converted by the HEASARC to mJy from Jy units in the original table). The flux density is based on the cold residual maps and therefore obtained after subtracting the warm component, using the aperture based on the elliptical Gaussian fit (given by major_axis, minor_axis and position_angle) .

Flux_857_GHz_Error
The 1-sigma uncertainty on the flux density of the clump at 857 GHz (converted by the HEASARC to mJy from Jy units in the original table). These are based on the FWHM of flux density distributions measured from artificial sources generated with Monte Carlo simulations.

Flux_545_GHz
The flux density of the clump at 545 GHz (converted by the HEASARC to mJy from Jy units in the original table). The flux density is based on the cold residual maps and therefore obtained after subtracting the warm component, using the aperture based on the elliptical Gaussian fit (given by major_axis, minor_axis and position_angle) .

Flux_545_GHz_Error
The 1-sigma uncertainty on the flux density of the clump at 545 GHz (converted by the HEASARC to mJy from Jy units in the original table). These are based on the FWHM of flux density distributions measured from artificial sources generated with Monte Carlo simulations.

Flux_353_GHz
The flux density of the clump at 353 GHz (converted by the HEASARC to mJy from Jy units in the original table). The flux density is based on the cold residual maps and therefore obtained after subtracting the warm component, using the aperture based on the elliptical Gaussian fit (given by major_axis, minor_axis and position_angle).

Flux_353_GHz_Error
The 1-sigma uncertainty on the Flux Density of the Clump at 353 GHz (converted by the HEASARC to mJy from Jy units in the original table). These are based on the FWHM of flux density distributions measured from artificial sources generated with Monte Carlo simulations.

Flux_3000_GHz_Bkg
The flux density of the warm background at 3THz (converted by the HEASARC to mJy from Jy units in the original table), measured using a polynomial fit of the background surface at 3 THz, subtracting any significant component arising from within the elliptical Gaussian aperture for the cold clump.

Flux_3000_GHz_Bkg_Error
The 1-sigma uncertainty on the flux density of the warm background at 3THz.

Flux_857_GHz_Bkg
The flux density of the warm background at 857 GHz (converted by the HEASARC to mJy from Jy units in the original table). This background component is extrapolated from the 3 THz map of the warm component and integrated over a solid angle with the same size as the cold clump.

Flux_857_GHz_Bkg_Error
The 1-sigma uncertainty on the flux density of the warm background at 857 GHz.

Flux_545_GHz_Bkg
The flux density of the warm background at 545 GHz (converted by the HEASARC to mJy from Jy units in the original table). This background component is extrapolated from the 3 THz map of the warm component and integrated over a solid angle with the same size as the cold clump.

Flux_545_GHz_Bkg_Error
The 1-sigma uncertainty on the flux density of the warm background at 545 GHz.

Flux_353_GHz_Bkg
The flux density of the warm background at 353 GHz (converted by the HEASARC to mJy from Jy units in the original table). This background component is extrapolated from the 3 THz map of the warm component and integrated over a solid angle with the same size as the cold clump.

Flux_353_GHz_Bkg_Error
The 1-sigma uncertainty on the flux density of the warm background at 353 GHz.

Flux_Flag
This flag indicates the category of the flux density quality, as follows:

    1 = "reliable flux densities" which have S/N > 1 in both Planck (857, 545,
        and 353 GHz) and IRIS 3 THz bands, allowing full characterization of
        their color ratio and their temperature.

    2 = "Missing 3 THz flux density" which have flux densities with S/N in all
        the Planck bands but not the 3THz IRIS band, where only an upper limit
        is available. These are sources with low flux densities and extremely
        cold temperatures with no detectable counterparts in the infrared.

    3 = "Detection only" where the quality of the elliptical Gaussian fit is
        poor and thus no reliable flux density can be obtained. These sources
        are likely extended or embedded in a complex environment.

Blend_Flag
This Boolean flag indicates a blending issue with the flux density estimate due to the presence of a nearby and partly overlapping source.

Blend_Catalog_Index
The catalog index for the closest source responsible for blending.

Blend_Offset
The angular distance in arcmin to the closest source responsible for blending.

Blend_Bias_3000_GHz
The relative bias of the flux density at 3 THz due to blending is approximately estimated as the level of contamination due to a nearby source. This bias is only indicative and cannot be used to correct the flux density estimate.

Blend_Bias_857_GHz
The relative bias of the flux density at 857 GHz due to blending is approximately estimated as the level of contamination due to a nearby source. This bias is only indicative and cannot be used to correct the flux density estimate.

Blend_Bias_545_GHz
The relative bias of the flux density at 545 GHz due to blending is approximately estimated as the level of contamination due to a nearby source. This bias is only indicative and cannot be used to correct the flux density estimate.

Blend_Bias_353_GHz
The relative bias of the flux density at 353 GHz due to blending is approximately estimated as the level of contamination due to a nearby source. This bias is only indicative and cannot be used to correct the flux density estimate.

Temperature
The temperature of the clump in K, allowing the emissivity spectral index to be a free parameter. The temperatures were measured from fitting a modified blackbody to the spectral energy distribution given by the cold source flux densities values for the IRIS 3THz and Planck 857, 545, and 353 GHz channels and assuming that the observed emission is optically thin at frequencies <= 3THz, that the emissivity spectral index is constant within the fitted wavelength range, and that the source is isothermal. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature, spectral_index, and amplitude of the blackbody fit. The temperature is the mean in the MCMC sample distribution.

Temperature_Error
The 1-sigma uncertainty on the clump temperature, in K, where the emissivity spectral index was free. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature, spectral_index, and amplitude of the blackbody fit. The temperature_error is the standard deviation in the MCMC sample distribution.

Temperature_Lower
The marginalized lower 68% confidence interval of the clump temperature where the emissivity spectral index was a free parameter, calculated from the MCMC samples.

Temperature_Upper
The marginalized upper 68% confidence interval of the clump temperature where the emissivity spectral index was a free parameter, calculated from the MCMC samples.

Spectral_Index
The emissivity spectral index of the clump, based on fitting a modified blackbody to the spectral energy distribution given by the IRIS 3THz and Planck 857, 545, and 353 GHz channels and assuming that the observed emission is optically thin at frequencies <= 3THz, that spectral_index is constant within the fitted wavelength range, and that the source is isothermal. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature, spectral_index, and amplitude of the blackbody fit. The spectral_index is the mean in the MCMC sample distribution.

Spectral_Index_Error
The 1-sigma uncertainty on the spectral_index. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature, spectral_index, and amplitude of the blackbody fit. The temperature_error is the standard deviation in the MCMC sample distribution.

Spectral_Index_Lower
The marginalized lower 68% confidence interval of the spectral_index, calculated from the MCMC samples.

Spectral_Index_Upper
The marginalized upper 68% confidence interval of the spectral_index, calculated from the MCMC samples.

Temperature_Alt
The temperature of the clump in K, fixing the emissivity spectral index to 2.0. The temperatures were measured from fitting a modified blackbody to the spectral energy distribution given by the IRIS 3THz and Planck 857, 545, and 353 GHz channels and assuming that the observed emission is optically thin at frequencies <= 3THz, that the emissivity spectral index is constant within the fitted wavelength range, and that the source is isothermal. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature and amplitude of the blackbody fit. The temperature_alt is the mean in the MCMC sample distribution.

Temperature_Alt_Error
The 1-sigma uncertainty on the clump temperature, in K, where the emissivity spectral index was set to 2.0. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature and amplitude of the blackbody fit. The temperature_alt_error is the standard deviation in the MCMC sample distribution.

Temperature_Alt_Lower
The marginalized lower 68% confidence interval of the clump temperature where the emissivity spectral index was set to 2.0, calculated from the MCMC samples.

Temperature_Alt_Upper
The marginalized upper 68% confidence interval of the clump temperature where the emissivity spectral index was set to 2.0, calculated from the MCMC samples.

Temp_Bkg
The temperature of the warm background in K, allowing the emissivity spectral index to be a free parameter. The temperatures were measured from fitting a modified blackbody to the spectral energy distribution given by the warm background flux densities in the IRIS 3THz and Planck 857, 545, and 353 GHz channels and assuming that the observed emission is optically thin at frequencies <= 3THz, that the emissivity spectral index is constant within the fitted wavelength range, and that the source is isothermal. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature, spectral index, and amplitude of the blackbody fit. The temperature_alt is the mean in the MCMC sample distribution.

Temp_Bkg_Error
The 1-sigma uncertainty on the warm background temperature, in K, where the emissivity spectral index was free. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature, spectral_index, and amplitude of the blackbody fit. The temperature_error is the standard deviation in the MCMC sample distribution.

Temp_Bkg_Lower
The marginalized lower 68% confidence interval of the warm background temperature where the emissivity spectral index was a free parameter, calculated from the MCMC samples.

Temp_Bkg_Upper
The marginalized upper 68% confidence interval of the warm background temperature where the emissivity spectral index was a free parameter, calculated from the MCMC samples.

Spectral_Index_Bkg
The emissivity spectral index of the warm background, based on fitting a modified blackbody to the spectral energy distribution given by the warm background flux density values for IRIS 3THz and Planck 857, 545, and 353 GHz channels and assuming that the observed emission is optically thin at frequencies <= 3THz, that spectral_index is constant within the fitted wavelength range, and that the source is isothermal. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature, spectral_index, and amplitude of the blackbody fit. The spectral_index is the mean in the MCMC sample distribution.

Spectral_Index_Bkg_Error
The 1-sigma uncertainty on the warm background spectral_index_bkg. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature, spectral_index, and amplitude of the blackbody fit. The temperature_error is the standard deviation in the MCMC sample distribution.

Spectral_Index_Bkg_Lower
The marginalized lower 68% confidence interval of the spectral_index_bkg, calculated from the MCMC samples.

Spectral_Index_Bkg_Upper
The marginalized upper 68% confidence interval of the spectral_index_bkg, calculated from the MCMC samples.

Temp_Bkg_Alt
The temperature of the warm background in K, fixing the emissivity spectral index to 2.0. The temperatures were measured from fitting a modified blackbody to the spectral energy distribution given by the warm background flux densities in the IRIS 3THz and Planck 857, 545, and 353 GHz channels and assuming that the observed emission is optically thin at frequencies <= 3THz, that the emissivity spectral index is constant within the fitted wavelength range, and that the source is isothermal. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature and amplitude of the blackbody fit. The temperature_alt is the mean in the MCMC sample distribution.

Temp_Bkg_Alt_Error
The 1-sigma uncertainty on the warm background temperature, in K, where the emissivity spectral index was set to 2.0. The authors use a Bayesian approach to estimating the temperatures, with flat priors for the temperature and amplitude of the blackbody fit. The temperature_alt_error is the standard deviation in the MCMC sample distribution.

Temp_Bkg_Alt_Upper
The marginalized lower 68% confidence interval of the warm background temperature where the emissivity spectral index was set to 2.0, calculated from the MCMC samples.

Temp_Bkg_Alt_Lower
The marginalized lower 68% confidence interval of the warm background temperature where the emissivity spectral index was set to 2.0, calculated from the MCMC samples.

Distance_Alt1
The kinematic distance estimate, in kpc. This is obtained by combining the gas observed radial velocity with a Galactic rotation curve, assuming gas circular motion.

Distance_Alt1_Error
The 1-sigma uncertainty in the kinematic distance estimate, in kpc.

Distance_Alt2
The distance in kpc estimated using optical extinction measures from SDSS DR7.

Distance_Alt2_Error
1-sigma uncertainty in The distance in kpc estimated using optical extinction measures from SDSS DR7.

Distance_Alt3
The distance in kpc estimated using optical extinction measures from SDSS DR9.

Distance_Alt3_Error
1-sigma uncertainty in The distance in kpc estimated using optical extinction measures from SDSS DR9.

Distance_Alt4
The distance in kpc estimated using near-Infrared extinction towards infrared dark clouds.

Distance_Alt4_Error
1-sigma uncertainty in the distance in kpc estimated using near-Infrared extinction towards infrared dark clouds.

Distance_Alt5
The distance in kpc estimated using near-Infrared extinction with 2MASS data.

Distance_Alt5_Error
1-sigma uncertainty in the distance in kpc estimated using near-Infrared extinction with 2MASS data.

Distance_Alt6
The distance in kpc estimated using molecular complex association and the quoted distances from the literature.

Distance_Alt6_Error
1-sigma uncertainty on the distance in kpc estimated using molecular complex association and the quoted distances from the literature.

Distance_Alt7
The distance estimated from the Herschel key-program Galactic Cold Cores, with distances taken from the literature.

Distance_Alt7_Error
1-sigma uncertainty on the distance in kpc estimated from the Herschel key-program Galactic Cold Cores.

Distance_Flag
The flag denoting the best distance estimate that was used in the calculation of other physical properties. The flag N means that the best distance is given by distance_altN.

Distance_Quality_Flag
The quality flag marking the consistency between distance estimates, as denoted by:

    0 = No distance estimate
    1 = Single distance estimate
    2 = Multiple distance estimates which are consistent within 1{sigma}
    3 = Multiple distance estimates which are not consistent within 1{sigma}
    4 = Single upper limits

Distance
The best distance estimate in kpc that was used in the calculation of other physical properties. The distance_flag provides the information that links the method to which this distance corresponds.

Distance_Error
The 1-sigma uncertainty for the best distance estimate in kpc that was used in the calculation of other physical properties. The distance_flag provides the information that links the method to which this distance corresponds.

Mass
The mass estimate of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the mean of the mass distribution.

Mass_Error
The 1-sigma uncertainty on the mass estimate of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the standard dispersion of the mass distribution.

Mass_Lower
The lower 68% confidence limit of the mass estimate of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the lower 68% confidence limit of the mass distribution.

Mass_Lower_2sig
The lower 95% confidence limit of the mass estimate of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the lower 95% confidence limit of the mass distribution.

Mass_Lower_3sig
The lower 99% confidence limit of the mass estimate of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the lower 99% confidence limit of the mass distribution.

Mass_Upper
The upper 68% confidence limit of the mass estimate of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the upper 68% confidence limit of the mass distribution.

Mass_Upper_2sig
The upper 95% confidence limit of the mass estimate of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the upper 95% confidence limit of the mass distribution.

Mass_Upper_3sig
The upper 99% confidence limit of the mass estimate of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the upper 99% confidence limit of the mass distribution.

Size
The physical size of the clump, in pc, based on the geometric mean of the major and minor FWHM: sqrt(major_axis * minor_axis), and converted to a physical size using the best distance, given by the distance parameter in this table. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the mean of the size distribution.

Size_Error
The 1-sigma uncertainty on the physical size of the clump, in pc, based on the geometric mean of the major and minor FWHM: sqrt(major_axis * minor_axis), and converted to a physical size using the best distance, given by the distance parameter in this table. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the standard dispersion of the size distribution.

Size_Lower
The lower 68% confidence limit of the physical size of the clump, in pc, based on the geometric mean of the major and minor FWHM: sqrt(major_axis * minor_axis), and converted to a physical size using the best distance, given by the distance parameter in this table. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the 68% lower limit of the size distribution.

Size_Lower_2sig
The lower 95% confidence limit of the physical size of the clump, in pc, based on the geometric mean of the major and minor FWHM: sqrt(major_axis * minor_axis), and converted to a physical size using the best distance, given by the distance parameter in this table. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the 95% lower limit of the size distribution.

Size_Lower_3sig
The lower 99% confidence limit of the physical size of the clump, in pc, based on the geometric mean of the major and minor FWHM: sqrt(major_axis * minor_axis), and converted to a physical size using the best distance, given by the distance parameter in this table. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the 99% lower limit of the size distribution.

Size_Upper
The upper 68% confidence limit of the physical size of the clump, in pc, based on the geometric mean of the major and minor FWHM: sqrt(major_axis * minor_axis), and converted to a physical size using the best distance, given by the distance parameter in this table. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the 68% upper limit of the size distribution.

Size_Upper_2sig
The upper 95% confidence limit of the physical size of the clump, in pc, based on the geometric mean of the major and minor FWHM: sqrt(major_axis * minor_axis), and converted to a physical size using the best distance, given by the distance parameter in this table. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the 95% upper limit of the size distribution.

Size_Upper_3sig
The upper 99% confidence limit of the physical size of the clump, in pc, based on the geometric mean of the major and minor FWHM: sqrt(major_axis * minor_axis), and converted to a physical size using the best distance, given by the distance parameter in this table. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the 99% upper limit of the size distribution.

Density
The mean density of the clump, measured from the mass/volume, assuming a sphere with diameter given by the size parameter. The physical parameters, mass and size, are obtained from 10⁶ Monte Carlo simulations, and this value is based on the mean of the density distribution.

Density_Error
The 1-sigma uncertainty of the mean density of the clump, measured from the mass/volume, assuming a sphere with diameter given by the size parameter. The physical parameters, mass and size, are obtained from 10⁶ Monte Carlo simulations, and this value is based on the standard dispersions of the density distribution.

Density_Lower
The lower 68% confidence limit of the mean density of the clump, measured from the mass/volume, assuming a sphere with diameter given by the size parameter. The physical parameters, mass and size, are obtained from 10⁶ Monte Carlo simulations, and this value is based on the lower 68% confidence limits of the density distribution.

Density_Lower_2sig
The lower 95% confidence limit of the mean density of the clump, measured from the mass/volume, assuming a sphere with diameter given by the size parameter. The physical parameters, mass and size, are obtained from 10⁶ Monte Carlo simulations, and this value is based on the lower 95% confidence limits of the density distribution.

Density_Lower_3sig
The lower 99% confidence limit of the mean density of the clump, measured from the mass/volume, assuming a sphere with diameter given by the size parameter. The physical parameters, mass and size, are obtained from 10⁶ Monte Carlo simulations, and this value is based on the lower 99% confidence limits of the density distribution.

Density_Upper
The upper 68% confidence limit of the mean density of the clump, measured from the mass/volume, assuming a sphere with diameter given by the size parameter. The physical parameters, mass and size, are obtained from 10⁶ Monte Carlo simulations, and this value is based on the upper 68% confidence limits of the density distribution.

Density_Upper_2sig
The upper 95% confidence limit of the mean density of the clump, measured from the mass/volume, assuming a sphere with diameter given by the size parameter. The physical parameters, mass and size, are obtained from 10⁶ Monte Carlo simulations, and this value is based on the upper 95% confidence limits of the density distribution.

Density_Upper_3sig
The upper 99% confidence limit of the mean density of the clump, measured from the mass/volume, assuming a sphere with diameter given by the size parameter. The physical parameters, mass and size, are obtained from 10⁶ Monte Carlo simulations, and this value is based on the upper 99% confidence limits of the density distribution.

L_Bol
The luminosity of the clump (converted by HEASARC to erg/s units from the original solar luminosity units), based on the integral of the modeled black body function with temperature and emissivity spectral_index and calculated over the 300 GHz - 10THz frequency range. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the mean of the luminosity distribution.

NH2
The H₂ column density of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the mean of the H₂ column density distribution.

NH2_Error
The 1-sigma uncertainty on the H₂ column density of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value is the standard dispersion of the H₂ column density distribution.

NH2_Lower
The lower 68% confidence limit of the H₂ column density of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value corresponds to the lower 68% confidence limit of the H₂ column density distribution.

NH2_Lower_2sig
The lower 95% confidence limit of the H₂ column density of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value corresponds to the lower 95% confidence limit of the H₂ column density distribution.

NH2_Lower_3sig
The lower 99% confidence limit of the H₂ column density of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value corresponds to the lower 99% confidence limit of the H₂ column density distribution.

NH2_Upper
The upper 68% confidence limit of the H₂ column density of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value corresponds to the upper 68% confidence limit of the H₂ column density distribution.

NH2_Upper_2sig
The upper 95% confidence limit of the H₂ column density of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value corresponds to the upper 95% confidence limit of the H₂ column density distribution.

NH2_Upper_3sig
The upper 99% confidence limit of the H₂ column density of the clump. The physical parameters are obtained from 10⁶ Monte Carlo simulations, and this value corresponds to the upper 99% confidence limit of the H₂ column density distribution.

Offset_Hot_Source
The angular distance between the cold clump and the closest hot source, in arcmin. The authors rejected sources with offset_hot_source < 5 arcmin, because the presence of hot sources within this distance can lead to an overestimate of the background temperature, given as temp_bkg in this table, and thus lead to spurious detections.

LMC_Flag
Boolean flag indicating whether the source is located within the LMC (lmc_flag=1) or not (lmc_flag=0)

SMC_Flag
Boolean flag indicating whether the source is located within the SMC (smc_flag=1) or not (smc_flag=0)

ECC_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Early Cold Cores catalog (ecc_flag=1) or not (eec_flag=0)

PCCS_857_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 857 GHz (pccs_857_ghz_flag=1) or not (pccs_857_ghz_flag=0)

PCCS_545_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 545 GHz (pccs_545_ghz_flag=1) or not (pccs_545_ghz_flag=0)

PCCS_353_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 353 GHz (pccs_353_ghz_flag=1) or not (pccs_353_ghz_flag=0)

PCCS_217_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 217 GHz (pccs_217_ghz_flag=1) or not (pccs_217_ghz_flag=0)

PCCS_143_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 143 GHz (pccs_143_ghz_flag=1) or not (pccs_143_ghz_flag=0)

PCCS_100_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 100 GHz (pccs_100_ghz_flag=1) or not (pccs_100_ghz_flag=0)

PCCS_70_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 70 GHz (pccs_70_ghz_flag=1) or not (pccs_70_ghz_flag=0)

PCCS_44_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 44 GHz (pccs_44_ghz_flag=1) or not (pccs_44_ghz_flag=0)

PCCS_30_GHz_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Compact Sources at 30 GHz (pccs_30_ghz_flag=1) or not (pccs_30_ghz_flag=0)

PSZ_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of Sunyaev-Zel'dovich sources (psz_flag=1) or not (psz_flag=0)

PHZ_Flag
Boolean flag indicating whether the source is located within the Planck internal catalog, the Planck Catalog of High-redshift sources candidates (phz_flag=1) or not (phz_flag=0)

HKPGCC_Flag
Boolean flag indicating whether the source is further investigated int eh Herschel open time key program Galactic Cold Cores (hkpgcc_flag=1) or not (hkpgcc_flag=0)

Contact Person

Questions regarding the PLANCKGCC database table can be addressed to the HEASARC Help Desk.

Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:33:01 EDT