A reanalysis of the carbon abundance in the translucent cloud toward HD 245341

Ulysses J. Sofia*, Edward L. Fitzpatrick, David M. Meyer

*Corresponding author for this work

Research output: Contribution to journalArticle

29 Scopus citations

Abstract

We have reanalyzed the Goddard High Resolution Spectrograph data set presented by Snow et al., which contains the interstellar intersystem C n] X2325 line through the translucent cloud toward HD 24534 (X Persei). In contrast to the results of Snow et al., we clearly detect the C II] feature at the 3 a confidence level and measure a C+ column density of 2.7 ± 0.8 × 1017 cm-2. Accounting for the C I column density along the line of sight, we find 106 C/H = 106 ± 38 in the interstellar gas toward this star. This gas-phase carbon-to-hydrogen ratio suggests that slightly more carbon depletion may be occurring in translucent as compared to diffuse clouds. The average diffuse-cloud C/H, however, is within the 1 a uncertainty of the measurement toward HD 24534. We therefore cannot rule out the possibility that the two cloud types have comparable gas-phase C/H and therefore comparable depletions of carbon. Subject headings: dust, extinction - ISM: abundances - ultraviolet: ISM

Original languageEnglish (US)
Pages (from-to)L47-L49
JournalAstrophysical Journal
Volume504
Issue number1 PART II
DOIs
StatePublished - 1998

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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