The relationship between the dust and gas-phase co across the california molecular cloud

S. Kong, C. J. Lada, E. A. Lada, C. Román-Zúñiga, John H Bieging, M. Lombardi, J. Forbrich, J. F. Alves

Research output: Contribution to journalArticle

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Abstract

We present results of an extinction-CO line survey of the southeastern part of the California molecular cloud (CMC). Deep, wide-field, near-infrared images were used to construct a sensitive, relatively high resolution (∼0.5 arcmin) (NICEST) extinction map of the region. The same region was also surveyed in the <sup>12</sup>CO(2-1), <sup>13</sup>CO(2-1), and C<sup>18</sup>O(2-1) emission lines at the same angular resolution. These data were used to investigate the relation between the molecular gas, traced by CO emission lines, and the dust column density, traced by extinction, on spatial scales of 0.04 pc across the cloud. We found strong spatial variations in the abundances of <sup>13</sup>CO and C<sup>18</sup>O that were correlated with variations in gas temperature, consistent with temperature-dependent CO depletion/desorption on dust grains. The <sup>13</sup>CO-to-C<sup>18</sup>O abundance ratio was found to increase with decreasing extinction, suggesting selective photodissociation of C<sup>18</sup>O by the ambient UV radiation field. The effect is particularly pronounced in the vicinity of an embedded cluster where the UV radiation appears to have penetrated deeply (i.e., ≲ 15 mag) into the cloud. We derived the cloud-averaged X-factor to be X = 2.53 × 10<sup>20</sup> , a value somewhat higher than the Milky Way average. On sub-parsec scales we find there is no single empirical value of the <sup>12</sup>CO X-factor that can characterize the molecular gas in cold (T ≲ 15 K) cloud regions, with X ∝ for 3 mag. However, in regions containing relatively hot (T 25 K) molecular gas we find a clear correlation between W(<sup>12</sup>CO) and over a large (3 ≲ ≲ 25 mag) range of extinction. This results in a constant X = 1.5 × 10<sup>20</sup> for the hot gas, a lower value than either the average for the CMC or the Milky Way. Overall we find an (inverse) correlation between X and T in the cloud with X ∝ T. This correlation suggests that the global X-factor of a giant molecular cloud may depend on the relative amounts of hot gas contained within the cloud.

Original languageEnglish (US)
Article number58
JournalAstrophysical Journal
Volume805
Issue number1
DOIs
StatePublished - May 20 2015

Fingerprint

molecular clouds
dust
vapor phases
extinction
molecular gases
gas
high temperature gases
gas temperature
angular resolution
photodissociation
radiation distribution
desorption
near fields
near infrared
depletion
spatial variation
temperature
high resolution
radiation

Keywords

  • dust extinction
  • ISM: abundances
  • ISM: clouds
  • stars: formation

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Kong, S., Lada, C. J., Lada, E. A., Román-Zúñiga, C., Bieging, J. H., Lombardi, M., ... Alves, J. F. (2015). The relationship between the dust and gas-phase co across the california molecular cloud. Astrophysical Journal, 805(1), [58]. https://doi.org/10.1088/0004-637X/805/1/58

The relationship between the dust and gas-phase co across the california molecular cloud. / Kong, S.; Lada, C. J.; Lada, E. A.; Román-Zúñiga, C.; Bieging, John H; Lombardi, M.; Forbrich, J.; Alves, J. F.

In: Astrophysical Journal, Vol. 805, No. 1, 58, 20.05.2015.

Research output: Contribution to journalArticle

Kong, S, Lada, CJ, Lada, EA, Román-Zúñiga, C, Bieging, JH, Lombardi, M, Forbrich, J & Alves, JF 2015, 'The relationship between the dust and gas-phase co across the california molecular cloud', Astrophysical Journal, vol. 805, no. 1, 58. https://doi.org/10.1088/0004-637X/805/1/58
Kong, S. ; Lada, C. J. ; Lada, E. A. ; Román-Zúñiga, C. ; Bieging, John H ; Lombardi, M. ; Forbrich, J. ; Alves, J. F. / The relationship between the dust and gas-phase co across the california molecular cloud. In: Astrophysical Journal. 2015 ; Vol. 805, No. 1.
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