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Widespread Galactic CF+ absorption: detection toward W49 with the Plateau de Bure Interferometer

hal.structure.identifierNational Radio Astronomy Observatory [NRAO]
dc.contributor.authorLISZT, H. S.,
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorGUZMAN, V. V.,
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorPETY, J.,
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorGERIN, M.,
hal.structure.identifierJohns Hopkins University [JHU]
dc.contributor.authorNEUFELD, D. A.,
hal.structure.identifierAMOR 2015
dc.contributor.authorGRATIER, P.
dc.date.issued2015-05
dc.identifier.issn0004-6361
dc.description.abstractEnTo study the usefulness of \CFP\ as a tracer of the regions where C\p\ and \HH\ coexist in the interstellar medium. We used the Plateau de Bure Interferometer to synthesize \CFP\ J=1-0 absorption at 102.6 GHz toward the core of the distant HII region W49N at l = 43.2\degr, b=0.0\degr, and we modeled the fluorine chemistry in diffuse/translucent molecular gas. We detected \CFP\ absorption over a broad range of velocity showing that \CFP\ is widespread in the \HH-bearing Galactic disk gas. Originally detected in dense gas in the Orion Bar and Horsehead PDR, \CFP\ was subsequently detected in absorption from diffuse and translucent clouds seen toward \bll\ and 3C111. Here we showed that \CFP\ is distributed throughout the diffuse and translucent molecular disk gas with N(\CFP)/N(\HH) $= 1.5-2.0\times10^{-10}$, increasing to N(\CFP)/N(\HH) $= 3.5\times10^{-10}$ in one cloud at 39 \kms\ having higher N(\HH) $\approx 3\times10^{21}\pcc$. Models of the fluorine chemistry reproduce the observed column densities and relative abundance of HF, from which \CFP\ forms, but generally overpredict the the column density of \CFP\ by factors of 1.4-4. We show that a free space photodissociation rate $\Gamma \ga 10^{-9}\ps$, comparable to that of CH, might account for much of the discrepancy but a recent calculation finds a value about ten times smaller. In the heavily blended and kinematically complex spectra seen toward W49, \CFP\ absorption primarily traces the peaks of the \HH\ distribution.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enWidespread Galactic CF+ absorption: detection toward W49 with the Plateau de Bure Interferometer
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201526232
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1505.07927
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A12
bordeaux.volume579
bordeaux.peerReviewedoui
hal.identifierhal-01158892
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01158892v1
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