The Carbon Inventory in a Quiescent, Filamentary Molecular Cloud in G328
We present spectral line images of [CI] 809 GHz, CO J=1-0 115 GHz and HI 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 [CI] data co...
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ftdatacite:10.48550/arxiv.1401.0421 2023-05-15T13:34:52+02:00 The Carbon Inventory in a Quiescent, Filamentary Molecular Cloud in G328 Burton, Michael Ashley, Michael Braiding, Catherine Storey, John Kulesa, Craig Hollenbach, David Wolfire, Mark Glueck, Christian Rowell, Gavin 2014 https://dx.doi.org/10.48550/arxiv.1401.0421 https://arxiv.org/abs/1401.0421 unknown arXiv https://dx.doi.org/10.1088/0004-637x/782/2/72 arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ Astrophysics of Galaxies astro-ph.GA FOS Physical sciences article-journal Article ScholarlyArticle Text 2014 ftdatacite https://doi.org/10.48550/arxiv.1401.0421 https://doi.org/10.1088/0004-637x/782/2/72 2022-04-01T13:00:11Z We present spectral line images of [CI] 809 GHz, CO J=1-0 115 GHz and HI 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 [CI] data comes from the High Elevation Antarctic Terahertz (HEAT) 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 HI datasets come from the Mopra and Parkes/ATCA telescopes, respectively. We identify a filamentary molecular cloud, ~75 x 5 pc long with mass ~4 x 10E4 Msun and a narrow velocity emission range of just 4 km/s. The morphology and kinematics of this filament are similar in CO, [CI] and HI, 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 PDR 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 (Tdust < 20K) 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 be in the process of formation. : 29 pages, 5 figures. Accepted for publication in The Astrophysical Journal (2014) Text Antarc* Antarctic DataCite Metadata Store (German National Library of Science and Technology) Antarctic The Antarctic |
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DataCite Metadata Store (German National Library of Science and Technology) |
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Astrophysics of Galaxies astro-ph.GA FOS Physical sciences |
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Astrophysics of Galaxies astro-ph.GA FOS Physical sciences Burton, Michael Ashley, Michael Braiding, Catherine Storey, John Kulesa, Craig Hollenbach, David Wolfire, Mark Glueck, Christian Rowell, Gavin The Carbon Inventory in a Quiescent, Filamentary Molecular Cloud in G328 |
topic_facet |
Astrophysics of Galaxies astro-ph.GA FOS Physical sciences |
description |
We present spectral line images of [CI] 809 GHz, CO J=1-0 115 GHz and HI 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 [CI] data comes from the High Elevation Antarctic Terahertz (HEAT) 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 HI datasets come from the Mopra and Parkes/ATCA telescopes, respectively. We identify a filamentary molecular cloud, ~75 x 5 pc long with mass ~4 x 10E4 Msun and a narrow velocity emission range of just 4 km/s. The morphology and kinematics of this filament are similar in CO, [CI] and HI, 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 PDR 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 (Tdust < 20K) 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 be in the process of formation. : 29 pages, 5 figures. Accepted for publication in The Astrophysical Journal (2014) |
format |
Text |
author |
Burton, Michael Ashley, Michael Braiding, Catherine Storey, John Kulesa, Craig Hollenbach, David Wolfire, Mark Glueck, Christian Rowell, Gavin |
author_facet |
Burton, Michael Ashley, Michael Braiding, Catherine Storey, John Kulesa, Craig Hollenbach, David Wolfire, Mark Glueck, Christian Rowell, Gavin |
author_sort |
Burton, Michael |
title |
The Carbon Inventory in a Quiescent, Filamentary Molecular Cloud in G328 |
title_short |
The Carbon Inventory in a Quiescent, Filamentary Molecular Cloud in G328 |
title_full |
The Carbon Inventory in a Quiescent, Filamentary Molecular Cloud in G328 |
title_fullStr |
The Carbon Inventory in a Quiescent, Filamentary Molecular Cloud in G328 |
title_full_unstemmed |
The Carbon Inventory in a Quiescent, Filamentary Molecular Cloud in G328 |
title_sort |
carbon inventory in a quiescent, filamentary molecular cloud in g328 |
publisher |
arXiv |
publishDate |
2014 |
url |
https://dx.doi.org/10.48550/arxiv.1401.0421 https://arxiv.org/abs/1401.0421 |
geographic |
Antarctic The Antarctic |
geographic_facet |
Antarctic The Antarctic |
genre |
Antarc* Antarctic |
genre_facet |
Antarc* Antarctic |
op_relation |
https://dx.doi.org/10.1088/0004-637x/782/2/72 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1401.0421 https://doi.org/10.1088/0004-637x/782/2/72 |
_version_ |
1766058638220197888 |