J/MNRAS/484/4444 ATLASGAL dense clumps Molecular parameters (Urquhart+, 2019)
ATLASGAL - molecular fingerprints of a sample of massive star-forming clumps.
Urquhart J.S., Figura C., Wyrowski F., Giannetti A., Kim W.-J., Wienen M.,
Leurini S., Pillai T., Csengeri T., Gibson S.J., Menten K.M., Moore T.J.T.,
Thompson M.A.
<Mon. Not. R. Astron. Soc., 484, 4444-4470 (2019)>
=2019MNRAS.484.4444U 2019MNRAS.484.4444U (SIMBAD/NED BibCode)
ADC_Keywords: H II regions ; Star Forming Region ; Molecular data
Keywords: stars: early-type - stars: formation - ISM: clouds -
(ISM:) abundances - submillimetre: ISM - ISM: molecules
Abstract:
We have conducted a 3-mm molecular-line survey towards 570 high-mass
star-forming clumps, using the Mopra telescope. The sample is selected
from the 10000 clumps identified by the ATLASGAL (APEX Telescope
Large Area Survey of the Galaxy) survey and includes all of the most
important embedded evolutionary stages associated with massive star
formation, classified into five distinct categories (quiescent,
protostellar, young stellar objects, HII regions, and
photon-dominated regions). The observations were performed in
broad-band mode with frequency coverage of 85.2-93.4GHz and a
velocity resolution of ∼0.9km/s, detecting emission from 26
different transitions. We find significant evolutionary trends in the
detection rates, integrated line intensities, and abundances of many
of the transitions and also identify a couple of molecules that appear
to be invariant to changes in the dust temperature and evolutionary
stage [N2H+ (1-0) and HN13C (1-0)]. We use the K-ladders for
CH3C2H (5-4) and CH3CH (5-4) to calculate the rotation
temperatures and find around one-third of the quiescent clumps have
rotation temperatures that suggest the presence of an internal heating
source. These sources may constitute a population of very young
protostellar objects that are still dark at 70um and suggest that
the fraction of truly quiescent clumps may only be a few per cent. We
also identify a number of line ratios that show a strong correlation
with the evolutionary stage of the embedded objects and discuss their
utility as diagnostic probes of evolution.
Description:
Molecular line parameters for ∼600 dense clumps identified by the
ATLASGAL survey.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 93 570 ATLASGAL sources
table5.dat 81 6611 Molecular line detections towards ATLASGAL
sources
table10.dat 97 16429 Parameters and noise values for all lines
covered in the survey
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Clump ATLASGAL catalogue name
20- 31 A12 --- Class Evolutionary classification
33- 40 F8.4 deg GLON Galactic Longitude
42- 48 F7.4 deg GLAT Galactic Latitude
50- 54 F5.2 arcsec Offset Offset between the peak submm and
pointing centre of the observations
56- 60 F5.2 kpc Dist ?=- Heliocentric distance
62- 65 F4.2 kpc e_Dist ?=- Distance uncertainty
67- 71 F5.2 K Tdust ?=- Dust Temperature
73- 77 F5.2 K e_Tdust ?=- Dust Temperature Uncertainty
79- 83 F5.2 [cm+2] logN(H2) ?=- H2 column density
85- 88 F4.2 [Msun] logMass ?=- Clump mass
90- 93 F4.2 [Lsun] logBolLum ?=- Bolometric luminosity
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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
20- 34 A15 --- Trans Molecular Transition
36- 38 I3 mK rms 1 sigma noise value
40- 46 F7.2 km/s VLSR Line VLSR
48- 51 F4.2 km/s e_VLSR Line VLSR uncertainty
53- 57 F5.2 K TA* Line intensity
59- 62 F4.2 K e_TA* Line intensity uncertainty
64- 69 F6.2 km/s dVLSR Line width (sigma)
71- 74 F4.2 km/s e_dVLSR Line width (sigma) uncertainty
76- 81 F6.2 K.km/s Int Integrated intensity
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Byte-by-byte Description of file: table10.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Clump ATLASGAL catalogue name
20- 34 A15 --- Trans Molecular Transition
36- 40 I5 mK rms 1 sigma noise value
42- 48 F7.2 km/s VLSR ?=- Line VLSR
50- 59 F10.2 km/s e_VLSR ?=- Line VLSR uncertainty
61- 65 F5.2 K TA* ?=- Line intensity
67- 73 F7.2 K e_TA* ?=- Line intensity uncertainty
75- 80 F6.2 km/s dVLSR ?=- Line width (sigma)
82- 90 F9.2 km/s e_dVLSR ?=- Line width (sigma) uncertainty
92- 97 F6.2 K.km/s Int ?=- Integrated intensity
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Acknowledgements:
James Urquhart, J.S.Urquhart(at)kent.ac.uk
(End) James Urquhart [University of Kent], Patricia Vannier [CDS] 08-Dec-2021