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Depletion of chlorine into HCl ice in a protostellar core

hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorKAMA, M.,
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorCAUX, E.,
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorLOPEZ-SEPULCRE, A.,
hal.structure.identifierAMOR 2015
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierAstronomical Institute Anton Pannekoek [AI PANNEKOEK]
dc.contributor.authorDOMINIK, C.,
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorCECCARELLI, C.,
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorLANZA, M.,
hal.structure.identifierLaboratoire Ondes et Milieux Complexes [LOMC]
dc.contributor.authorLIQUE, F.,
dc.contributor.authorOCHSENDORF, B. B.,
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorLIS, D. C.,
dc.contributor.authorCABALLERO, R. N.,
hal.structure.identifierSRON Netherlands Institute for Space Research [SRON]
dc.contributor.authorTIELENS, A. G. G. M.
dc.date.created2014
dc.date.issued2015
dc.identifier.issn0004-6361
dc.description.abstractEnThe freezeout of gas-phase species onto cold dust grains can drastically alter the chemistry and the heating-cooling balance of protostellar material. In contrast to well-known species such as carbon monoxide (CO), the freezeout of various carriers of elements with abundances $<10^{-5}$ has not yet been well studied. Our aim here is to study the depletion of chlorine in the protostellar core, OMC-2 FIR 4. We observed transitions of HCl and H2Cl+ towards OMC-2 FIR 4 using the Herschel Space Observatory and Caltech Submillimeter Observatory facilities. Our analysis makes use of state of the art chlorine gas-grain chemical models and newly calculated HCl-H$_{2}$ hyperfine collisional excitation rate coefficients. A narrow emission component in the HCl lines traces the extended envelope, and a broad one traces a more compact central region. The gas-phase HCl abundance in FIR 4 is 9e-11, a factor of only 0.001 that of volatile elemental chlorine. The H2Cl+ lines are detected in absorption and trace a tenuous foreground cloud, where we find no depletion of volatile chlorine. Gas-phase HCl is the tip of the chlorine iceberg in protostellar cores. Using a gas-grain chemical model, we show that the hydrogenation of atomic chlorine on grain surfaces in the dark cloud stage sequesters at least 90% of the volatile chlorine into HCl ice, where it remains in the protostellar stage. About 10% of chlorine is in gaseous atomic form. Gas-phase HCl is a minor, but diagnostically key reservoir, with an abundance of <1e-10 in most of the protostellar core. We find the 35Cl/37Cl ratio in OMC-2 FIR 4 to be 3.2\pm0.1, consistent with the solar system value.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enDepletion of chlorine into HCl ice in a protostellar core
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201424737
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv1411.6483
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A107
bordeaux.volume574
bordeaux.peerReviewedoui
hal.identifierhal-01090994
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01090994v1
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