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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 |
Published version: | http://dx.doi.org/10.1088/0004-637x/782/2/72 |
Appears in Collections: | Aurora harvest 4 IPAS publications |
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