Tracing H2 column density with atomic carbon C i and co isotopologsReport as inadecuate

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We present the first results of neutral carbon Ci 3P1–3P0 at 492 GHz and carbon monoxide 13CO, J = 1–0mapping in the Vela Molecular Ridge cloud C VMR-C and the G333 giant molecular cloud complexes with theNANTEN2 and Mopra telescopes. For the four regions mapped in this work, we find that Ci has very similarspectral emission profiles to 13CO, with comparable line widths. We find that C i has an opacity of 0.1–1.3 acrossthe mapped region while the Ci-13CO peak brightness temperature ratio is between 0.2 and 0.8. The C i columndensity is an order of magnitude lower than that of 13CO. The H2 column density derived from Ci is comparableto values obtained from 12CO. Our maps show that Ci is preferentially detected in gas with low temperatures below20 K, which possibly explains the comparable H2 column density calculated from both tracers both Ci and 12COunderestimate column density, as a significant amount of the C i in the warmer gas is likely in the higher energystate transition C i 3P2–3P1 at 810 GHz, and thus it is likely that observations of both the above C i transitionsare needed in order to recover the total H2 column density.Nota general

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Author: Bronfman Aguiló, Leonardo; - Lo, Nadia; - Cunningham, M. R.; - Jones, P. A.; - Cortes, P. C.; - Simon, R.; - Lowe, V.; - Fissel,



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