J/MNRAS/473/1059 Complete sample of Galactic clump properties (Urquhart+, 2018)
ATLASGAL - properties of a complete sample of Galactic clumps.
Urquhart J.S., Koenig C., Giannetti A., Leurini S., Moore T.J.T.,
Eden D.J., Pillai T., Thompson M.A., Braiding C., Burton M.G., Csengeri T.,
Dempsey J.T., Figura C., Froebrich D., Menten K.M., Schuller F.,
Smith M.D., Wyrowski F.
<Mon. Not. R. Astron. Soc. 473, 1059 (2018)>
=2018MNRAS.473.1059U 2018MNRAS.473.1059U (SIMBAD/NED BibCode)
ADC_Keywords: Galactic plane ; Associations, stellar ; Molecular clouds
Keywords: stars: formation - stars: massive - ISM: clouds -
Galaxy: kinematics and dynamics - Galaxy: structure
Abstract:
The APEX Telescope Large Area Survey of the Galaxy (ATLASGAL) is an
unbiased 870um submillimetre survey of the inner Galactic plane
(|l|<60° with |b|<1.5°). It is the largest and most sensitive
ground-based submillimetre wavelength Galactic survey to date and has
provided a large and systematic inventory of all massive, dense clumps
in the Galaxy (≥1000M☉ at a heliocentric distance of 20kpc) and
includes representative samples of all of the earliest embedded stages
of high-mass star formation. Here, we present the first detailed
census of the properties (velocities, distances, luminosities and
masses) and spatial distribution of a complete sample of ∼8000 dense
clumps located in the Galactic disc (5°<|l|<60°). We derive
highly reliable velocities and distances to ∼97 per cent of the
sample and use mid- and far-infrared survey data to develop an
evolutionary classification scheme that we apply to the whole sample.
Comparing the evolutionary subsamples reveals trends for increasing
dust temperatures, luminosities and linewidths as a function of
evolution indicating that the feedback from the embedded protoclusters
is having a significant impact on the structure and dynamics of their
natal clumps. We find that the vast majority of the detected clumps
are capable of forming a massive star and 88 per cent are already
associated with star formation at some level. We find the clump mass
to be independent of evolution suggesting that the clumps form with
the majority of their mass in situ. We estimate the statistical
lifetime of the quiescent stage to be ∼5x104yr for clump masses
>1000M☉ decreasing to ∼1x104yr for clump masses
>10000M☉. We find a strong correlation between the fraction of
clumps associated with massive stars and peak column density. The
fraction is initially small at low column densities, but reaching
100 per cent for column densities above 1023cmx2; there are no
clumps with column densities above this value that are not already
associated with massive star formation. All of the evidence is
consistent with a dynamic view of star formation wherein the clumps
form rapidly and are initially very unstable so that star formation
quickly ensues.
Description:
Derived clump parameters for ATLASGAL clumps located in the Galactic
longitudes 300<l<355 and 5<l<60.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 115 8002 Derived distance measurements to all ATLASGAL
clumps in the study
table5.dat 112 8002 Derived physical properties for all ATLASGAL
clumps in the study (updated)
table8.dat 149 776 Derive positions and properties for all clump
associations (clusters)
tablea2.dat 106 3160 Gaussian components for detected emission
components
refs.dat 82 54 References
fig6/* . 7861 SED in png
fig8/* . 411 Images in fits, eps and png
figa1/* . 2330 13CO spectra in png and eps
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See also:
J/A+A/540/A113 : Starless clumps in ATLASGAL (Tackenberg+, 2012)
J/A+A/544/A146 : ATLASGAL cold high-mass clumps with NH3 (Wienen+, 2012)
J/A+A/549/A45 : ATLASGAL Compact Source Catalog: 330<l<21 (Contreras+, 2013)
J/MNRAS/431/1752 : ATLASGAL 6.7GHz methanol masers (Urquhart+, 2013)
J/MNRAS/435/400 : ATLASGAL Properties of compact HII regions (Urquhart+, 2013)
J/A+A/565/A75 : ATLASGAL Dust condensations in Galactic plane
(Csengeri+, 2014)
J/A+A/568/A41 : ATLASGAL Compact Source Catalog: 280<l<60 (Urquhart+, 2014)
J/A+A/570/A65 : ATLASGAL massive clumps CO depletion (Giannetti+, 2014)
J/MNRAS/443/1555 : ATLASGAL massive star forming clumps sample (Urquhart+ 2014)
J/A+A/579/A91 : ATLASGAL inner Galaxy massive cold dust clumps
(Wienen+, 2015)
J/A+A/581/A74 : Molecular clouds as viewed by ATLASGAL (Abreu-Vicente+ 2015)
J/A+A/586/A149 : SiO in ATLASGAL-selected massive clumps (Csengeri+, 2016)
J/A+A/591/A5 : ATLASGAL dense filamentary structures (Li+, 2016)
J/ApJ/824/29 : ATLASGAL clumps with IRAS flux & MALT90 data
(Stephens+, 2016)
J/ApJS/231/11 : High-mass starless clump candidates from ATLASGAL
(Yuan+, 2017)
J/A+A/599/A139 : ATLASGAL massive clumps dust characterization (Koenig+ 2017)
J/A+A/600/L10 : Massive cluster progenitors from ATLASGAL (Csengeri+, 2017)
J/A+A/601/A60 : ATLASGAL massive cluster progenitors sample (Csengeri+ 2017)
J/A+A/602/A37 : ATLASGAL-selected massive clumps millimeter RRL (Kim+, 2017)
J/A+A/603/A33 : Temperature evolution in massive clumps (Giannetti+, 2017)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Clump ATLASGAL catalogue name, AGALLLL.lll+BB.bbb
(Clump_name)
20- 25 F6.1 km/s VLSR ?=- Radial Velocity (VLSR)
27- 28 I2 --- r_VLSR ?=- Reference for the VLSR in refs.dat file
(VLSR_ref)
30- 33 F4.1 kpc DistReid ?=- Distance determined from the Reid et al.
(2016ApJ...823...77R 2016ApJ...823...77R) Bayesian model
(Reid_dist)
35- 38 F4.1 kpc DistNear ?=- Near distance (Near_dist)
40- 43 F4.1 kpc DistFar ?=- Far distance (Far_dist)
45- 48 F4.1 kpc Dist ?=- Adopted kinematic distance (Distance)
50- 55 A6 --- SolFlag Flag indicating how the kinematic distance was
assigned (Solution_flag) (1)
57- 67 A11 --- r_Dist ?=- Reference used to determine the kinematic
distance in refs.dat file (Distance_ref)
69- 83 A15 --- Cluster Name of cluster source is associated with
GLLL.lll+BB.bbb or Bania Clump 1
(Cluster_name)
85- 88 F4.1 kpc DistCl ?=- Cluster distance this is used for the
clump (Cluster_dist)
90-115 A26 --- SED Name of the image with SED in subdirectory
fig6
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Note (1): Flags as follows:
(i) = Parallax/Spectroscopic
(ii) = Outer Galaxy
(iii) = Tangent
(iv) = Z distance
(v) = HI EA
(vi) = HI SA Near (?)
(vi) = HI SA Far (?)
(vii) = IRDC associations
(viii) = Literature
(ix) = Ambiguous (Solar circle)
(x) = No vlsr available
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Clump ATLASGAL catalogue name (Clump_name)
20- 31 A12 --- EvolType Star formation evolutionary stage
(Evolution_type)
33- 37 F5.2 Jy/beam Fpeak 870 micron peak flux density (Peak_flux)
39- 44 F6.2 Jy/beam Fint 870 micron integrated flux density (Int_flux)
46- 51 F6.1 km/s VLSR ?=- Radial Velocity (VLSR)
53- 57 F5.2 kpc Dist ?=- Assigned distance (cluster distance is
avaiable else adpoted kinematic distance)
(Distance)
59- 63 F5.2 kpc RGC ?=- Galactocentric distance (RGC)
65- 69 F5.3 pc Rad ?=- Clump effective radius (Radius)
71- 74 F4.1 K Tdust ?=- Dust temperature determined from SED fit
(Dust_temp)
76- 81 F6.3 [Lsun] logLbol ?=- Log of the bolomeric luminosity (Bol_lum)
83- 88 F6.3 [Msun] logMclump ?=- Log of the clump mass (Clump_mass)
90- 95 F6.3 [cm-2] logNH2 ?=- Log of the H2 column density (Col_den)
97- 99 F3.1 km/s NH3LW ?=- Ammonia (1,1) deconvolved linewidth
(NH3_linewidth)
101-105 F5.3 Msun Mvirial ?=- Virial mass estimated from the NH3
linewidth (Virial_mass)
107-112 F6.3 --- alpha ?=- Virial parameter (alpha)
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Cluster Cluster name, GLLL.lll+BB.bbb or Bania Clump 1
(Cluster_name)
16- 43 A28 --- OName Literature name (Other_name)
45- 47 I3 --- Nclump Number of clumps associated with cluster
(Number_clump)
49- 55 F7.3 deg GLON Longitude of cluster (Gal_long)
57- 61 F5.3 deg e_GLON Longitude size of cluster (standard deviation)
(Gallongsize)
63- 68 F6.3 deg GLAT Latitude of cluster (Gal_lat)
70- 74 F5.3 deg e_GLAT Latitude size of cluster (standard deviation)
(Gallatsize)
76- 81 F6.1 km/s Mean radial velocity of cluster (Mean_vlsr)
83- 87 F5.2 km/s s_ Standard deviation of velocity components
(Stdev_vlsr)
89- 92 F4.1 kpc Dist ?=- Cluster distance (Distance)
94- 97 F4.1 K <Temp> ?=- Mean clump temperature (Mean_temp)
99-102 F4.1 K s_<Temp> ?=- Standard deviation of clump temperatures
(Stdev_temp)
104-109 F6.3 [Lsun] logLbol ?=- Log of the total bolomeric luminosity of
all associate clumps (cluster_lum)
111-115 F5.3 [Msun] logMclump ?=- Log of the total clump mass (cluster_mass)
117-121 F5.1 Sun L/M ?=- Luminosity to mass ratio (L/M_ratio)
123-149 A27 --- FileName Name of the image in subdirectory fig8 (1)
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Note (1): Images are available in fits, eps and png, i.e.
FileName.fits, FileName.eps and FileName.png, respectively.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Clump ATLASGAL catalogue name (Clump_name)
19 A1 --- n_Clump [*] * indicates the velocity assigned to the
source
21- 24 I4 mK rms ? Spectral noise (rms)
26- 31 F6.1 km/s VLSR13CO ?=- 13CO Component radial velocity (VLSR)
33- 36 F4.1 K Peak13CO ?=- 13CO Peak emission (13CO(2-1)Peak)
38- 41 F4.2 km/s W13CO ?=- 13CO Line width (13CO(2-1)sigmaV)
43- 47 F5.1 K.km/s Int13CO ?=- 13CO Integrated line intensity
(13CO(2-1)Intensity)
49- 54 F6.1 km/s VLSRC18O ?=- C^18O Component radial velocity
(C18O(2-1)VLSRC)
56- 58 F3.1 K PeakC18O ?=- C18O Peak emission (C18O(2-1)Peak)
60- 63 F4.2 km/s WC18O ?=- C18O Line width (C18O(2-1)sigmaV)
65- 68 F4.1 K.km/s IntC18O ?=- C18O Integrated line intensity
(C18O(2-1)Intensity)
70- 73 F4.2 --- Depth ?=- Optical depth (Optical_depth)
75-106 A32 --- sp Name of the file with 13CO spectrum image
in subdirectory figa1
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode Bibcode
24- 44 A21 --- Aut Author's name
46- 82 A37 --- Com Comments
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Acknowledgements:
James Urquhart, j.s.urquhart(at)gmail.com
History:
* 15-Jan-2018: on-line version
* 23-Jul-2019: table5 updated
(End) James Urquhart [University of Kent], Patricia Vannier [CDS] 15-Jan-2018