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## PLANCKGCC - Planck Catalog of Galactic Cold Clumps (PGCC) |
HEASARC Archive |

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.

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)

**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
10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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
10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6} 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 10^{6}
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 10^{6}
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 10^{6}
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 10^{6}
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 10^{6}
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 10^{6}
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 10^{6} Monte Carlo simulations, and this value is the mean of
the luminosity distribution.

**NH2**

The H_{2} column density of the clump. The physical parameters are obtained
from 10^{6} Monte Carlo simulations, and this value is the mean of the H_{2}
column density distribution.

**NH2_Error**

The 1-sigma uncertainty on the H_{2} column density of the clump. The physical
parameters are obtained from 10^{6} Monte Carlo simulations, and this value is
the standard dispersion of the H_{2} column density distribution.

**NH2_Lower**

The lower 68% confidence limit of the H_{2} column density of the clump. The
physical parameters are obtained from 10^{6} Monte Carlo simulations, and this
value corresponds to the lower 68% confidence limit of the H_{2} column
density distribution.

**NH2_Lower_2sig**

The lower 95% confidence limit of the H_{2} column density of the clump. The
physical parameters are obtained from 10^{6} Monte Carlo simulations, and this
value corresponds to the lower 95% confidence limit of the H_{2} column
density distribution.

**NH2_Lower_3sig**

The lower 99% confidence limit of the H_{2} column density of the clump. The
physical parameters are obtained from 10^{6} Monte Carlo simulations, and this
value corresponds to the lower 99% confidence limit of the H_{2} column
density distribution.

**NH2_Upper**

The upper 68% confidence limit of the H_{2} column density of the clump. The
physical parameters are obtained from 10^{6} Monte Carlo simulations, and this
value corresponds to the upper 68% confidence limit of the H_{2} column
density distribution.

**NH2_Upper_2sig**

The upper 95% confidence limit of the H_{2} column density of the clump. The
physical parameters are obtained from 10^{6} Monte Carlo simulations, and this
value corresponds to the upper 95% confidence limit of the H_{2} column
density distribution.

**NH2_Upper_3sig**

The upper 99% confidence limit of the H_{2} column density of the clump. The
physical parameters are obtained from 10^{6} Monte Carlo simulations, and this
value corresponds to the upper 99% confidence limit of the H_{2} 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)