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Ortho-to-para ratio of interstellar heavy water

hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorVASTEL, C.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorCECCARELLI, C.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorCAUX, E.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorCOUTENS, A.
hal.structure.identifierCentro de Astrobiologia [Madrid] [CAB]
dc.contributor.authorCERNICHARO, J.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorBOTTINELLI, S.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorDEMYK, K.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorFAURE, A.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorWIESENFELD, L.
dc.contributor.authorSCRIBANO, Y.
hal.structure.identifierFORMATION STELLAIRE 2010
dc.contributor.authorBACMANN, A.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorHILY-BLANT, Pierre
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorMARET, S.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorWALTERS, A.
hal.structure.identifierDepartment of Astronomy [Ann Arbor]
dc.contributor.authorBERGIN, E. A.
hal.structure.identifierLabOratoire proCédés énergIe bâtimEnt [LOCIE]
dc.contributor.authorBLAKE, G. A.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorCASTETS, Alain
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorCRIMIER, N.
hal.structure.identifierAstronomical Institute Anton Pannekoek [AI PANNEKOEK]
dc.contributor.authorDOMINIK, C.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorENCRENAZ, P.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
hal.structure.identifierLaboratoire de Radioastronomie [LRA]
dc.contributor.authorGÉRIN, M.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorHENNEBELLE, P.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorKAHANE, C.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
hal.structure.identifierObservatoire de Haute-Provence [OHP]
dc.contributor.authorKLOTZ, A.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorMELNICK, G.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorPAGANI, L.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorPARISE, B.
hal.structure.identifierI. Physikalisches Institut [Köln]
hal.structure.identifierMax Planck Institute for Radio Astronomy
dc.contributor.authorSCHILKE, P.
hal.structure.identifierAMOR 2010
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierFORMATION STELLAIRE 2010
dc.contributor.authorBAUDRY, Alain
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorBELL, T.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorBENEDETTINI, M.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorBOOGERT, A.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorCABRIT, S.
hal.structure.identifierINAF - Osservatorio Astrofisico di Arcetri [OAA]
dc.contributor.authorCASELLI, P.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorCODELLA, C.
hal.structure.identifierMax Planck Institute for Radio Astronomy
dc.contributor.authorCOMITO, C.
hal.structure.identifierLaboratoire de Radioastronomie [LRA]
dc.contributor.authorFALGARONE, E.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorFUENTE, A.
dc.contributor.authorGOLDSMITH, P. F.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorHELMICH, F.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorHENNING, T.
hal.structure.identifierDepartment of Physics [Ohio State University] [OSU]
hal.structure.identifierOhio State Univ, Dept Astron & Chem, Columbus, OH 43210 USA
dc.contributor.authorHERBST, E.
hal.structure.identifierFORMATION STELLAIRE 2010
dc.contributor.authorJACQ, T.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorKAMA, M.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorLANGER, W.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorLEFLOCH, B.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorLIS, D.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorLORD, S.
hal.structure.identifierINAF - Osservatorio Astrofisico di Arcetri [OAA]
dc.contributor.authorLORENZANI, A.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorNEUFELD, D.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorNISINI, B.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorPACHECO, S.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorPEARSON, Justin
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorPHILLIPS, T.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorSALEZ, M.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorSARACENO, P.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorSCHUSTER, K.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorTIELENS, X.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorVAN DER TAK, F.
dc.contributor.authorVAN DER WIEL, M. H. D.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorVITI, S.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorYORKE, H.
hal.structure.identifierFORMATION STELLAIRE 2010
dc.contributor.authorCAIS, Ph.
dc.contributor.authorKRIEG, J. M.
hal.structure.identifierOnsala Space Observatory
dc.contributor.authorOLBERG, M.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorRAVERA, L.
dc.date.issued2010-10
dc.identifier.issn0004-6361
dc.description.abstractEnContext. Despite the low elemental deuterium abundance in the Galaxy, enhanced molecular D/H ratios have been found in the environments of low-mass star-forming regions, and in particular the Class 0 protostar IRAS 16293-2422. Aims: The CHESS (Chemical HErschel Surveys of Star forming regions) key program aims to study the molecular complexity of the interstellar medium. The high sensitivity and spectral resolution of the Herschel/HIFI instrument provide a unique opportunity to observe the fundamental 11,1-00,0 transition of the ortho-D2O molecule, which is inaccessible from the ground, and determine the ortho-to-para D2O ratio. Methods: We detected the fundamental transition of the ortho-D2O molecule at 607.35 GHz towards IRAS 16293-2422. The line is seen in absorption with a line opacity of 0.62 ± 0.11 (1σ). From the previous ground-based observations of the fundamental 11,0-10,1 transition of para-D2O seen in absorption at 316.80 GHz, we estimate a line opacity of 0.26 ± 0.05 (1σ). Results: We show that the observed absorption is caused by the cold gas in the envelope of the protostar. Using these new observations, we estimate for the first time the ortho-to-para D2O ratio to be lower than 2.6 at a 3σ level of uncertainty, which should be compared with the thermal equilibrium value of 2:1. Herschel is an ESA space observatory with science instruments provided by European-led principal Investigator consortia and with important participation from NASA.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enastrochemistry
dc.subject.enISM: molecules
dc.subject.ensubmillimeter: ISM
dc.subject.enISM: abundances
dc.subject.enmolecular processes
dc.subject.enline: identification
dc.title.enOrtho-to-para ratio of interstellar heavy water
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201015101
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1007.4410
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageL31
bordeaux.volume521
bordeaux.peerReviewedoui
hal.identifierhal-00633418
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00633418v1
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