Please use this identifier to cite or link to this item: https://hdl.handle.net/2440/82889
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Type: Journal article
Title: The carbon inventory in a quiescent, filamentary molecular cloud in G328
Author: Burton, M.
Ashley, M.
Braiding, C.
Storey, J.
Kulesa, C.
Hollenbach, D.
Wolfire, M.
Gluck, C.
Rowell, G.
Citation: The Astrophysical Journal: an international review of astronomy and astronomical physics, 2014; 782(2):1-8
Publisher: Institute of Physics
Issue Date: 2014
ISSN: 0004-637X
1538-4357
Organisation: Institute for Photonics & Advanced Sensing (IPAS)
Statement of
Responsibility: 
Michael G. Burton, Michael C. B. Ashley, Catherine Braiding, John W. V. Storey, Craig Kulesa, David J. Hollenbach, Mark Wolfire, Christian Glück and Gavin Rowell
Abstract: We present spectral line images of [C I] 809 GHz, CO J = 1-0 115 GHz and H I 1.4 GHz line emission, and calculate the corresponding C, CO and H column densities, for a sinuous, quiescent giant molecular cloud about 5 kpc distant along the l = 328° sightline (hereafter G328) in our Galaxy. The [C I] data comes from the High Elevation Antarctic Terahertz telescope, a new facility on the summit of the Antarctic plateau where the precipitable water vapor falls to the lowest values found on the surface of the Earth. The CO and H I data sets come from the Mopra and Parkes/ATCA telescopes, respectively. We identify a filamentary molecular cloud, ~75 × 5 pc long with mass ~4 × 104 M ☉ and a narrow velocity emission range of just 4 km s–1. The morphology and kinematics of this filament are similar in CO, [C I], and H I, though in the latter appears as self-absorption. We calculate line fluxes and column densities for the three emitting species, which are broadly consistent with a photodissociation region model for a GMC exposed to the average interstellar radiation field. The [C/CO] abundance ratio averaged through the filament is found to be approximately unity. The G328 filament is constrained to be cold (T Dust < 20 K) by the lack of far-IR emission, to show no clear signs of star formation, and to only be mildly turbulent from the narrow line width. We suggest that it may represent a GMC shortly after formation, or perhaps still in the process of formation.
Keywords: ISM: abundances
ISM: clouds
ISM: molecules
ISM: structure
radio lines: ISM
telescopes
Description: Extent: 8 p.
Rights: © 2014.The American Astronomical Society. All rights reserved.
DOI: 10.1088/0004-637X/782/2/72
Grant ID: http://purl.org/au-research/grants/arc/DP120101585
Appears in Collections:Aurora harvest 4
IPAS publications

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