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20 April 2024

» arxiv » 1005.1671

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Strong absorption by interstellar hydrogen fluoride: Herschel/HIFI observations of the sight-line to G10.6-0.4 (W31C)
D. A. Neufeld ; P. Sonnentrucker ; T. G. Phillips ; D. C. Lis ; M. De Luca ; J. R. Goicoechea ; J. H. Black ; M. Gerin ; T. Bell ; F. Boulanger ; J. Cernicharo ; A. Coutens ; E. Dartois ; M. Kazmierczak ; P. Encrenaz ; E. Falgarone ; T. R. Geballe ; T. Giesen ; B. Godard ; P. F. Goldsmith ; C. Gry ; H. Gupta ; P. Hennebelle ; E.Herbst ; P. Hily-Blant ; C. Joblin ; R. Kolos ; J. Krelowski ; J. Martin-Pintado ; K. M. Menten ; R. Monje ; B. Mookerjea ; J. Pearson ; M. Perault ; C. Persson ; R. Plume ; M. Salez ; S. Schlemmer ; M. Schmidt ; J. Stutzki ; D. Teyssier ; C. Vastel ; S. Yu ; P. Cais ; E. Caux ; R. Liseau ; P. Morris ; P. Planesas ;
Date:	10 May 2010
Abstract:	We report the detection of strong absorption by interstellar hydrogen fluoride along the sight-line to the submillimeter continuum source G10.6-0.4 (W31C). We have used Herschel’s HIFI instrument, in dual beam switch mode, to observe the 1232.4763 GHz J=1-0 HF transition in the upper sideband of the Band 5a receiver. The resultant spectrum shows weak HF emission from G10.6-0.4 at LSR velocities in the range -10 to -3 km/s, accompanied by strong absorption by foreground material at LSR velocities in the range 15 to 50 km/s. The spectrum is similar to that of the 1113.3430 GHz 1(11)-0(00) transition of para-water, although at some frequencies the HF (hydrogen fluoride) optical depth clearly exceeds that of para-H2O. The optically-thick HF absorption that we have observed places a conservative lower limit of 1.6E+14 cm-2 on the HF column density along the sight-line to G10.6-0.4. Our lower limit on the HF abundance, 6E-6 relative to hydrogen nuclei, implies that hydrogen fluoride accounts for between ~ 30 and 100% of the fluorine nuclei in the gas phase along this sight-line. This observation corroborates theoretical predictions that - because the unique thermochemistry of fluorine permits the exothermic reaction of F atoms with molecular hydrogen - HF will be the dominant reservoir of interstellar fluorine under a wide range of conditions.
Source:	arXiv, 1005.1671
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