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Herschel-HIFI view of mid-IR quiet massive protostellar objects

hal.structure.identifierFORMATION STELLAIRE 2016
dc.contributor.authorHERPIN, Fabrice
dc.contributor.authorCHAVARRIA, L.
hal.structure.identifierFORMATION STELLAIRE 2016
dc.contributor.authorJACQ, T.
hal.structure.identifierFORMATION STELLAIRE 2016
dc.contributor.authorBRAINE, J.
hal.structure.identifierSRON Netherlands Institute for Space Research [SRON]
dc.contributor.authorVAN DER TAK, F.
dc.contributor.authorWYROWSKI, F.
hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorVAN DISHOECK, E. F.
hal.structure.identifierFORMATION STELLAIRE 2016
dc.contributor.authorBAUDRY, Alain
hal.structure.identifierFORMATION STELLAIRE 2016
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierDanish Meat Research Institute [DMRI]
dc.contributor.authorKRISTENSEN, L.
dc.contributor.authorSCHMALZL, M.
hal.structure.identifierCentro de Geologia [Lisboa]
dc.contributor.authorMATA, J.
dc.date.issued2016
dc.identifier.issn0004-6361
dc.description.abstractEnWe present Herschel/HIFI observations (WISH KP) of 14 water lines in a small sample of galactic massive protostellar objects: NGC6334I(N), DR21(OH), IRAS16272-4837, and IRAS05358+3543. We analyze the gas dynamics from the line profiles. Through modeling of the observations using RATRAN, we estimate outflow, infall, turbulent velocities, molecular abundances, and investigate any correlation with the evolutionary status of each source. The molecular line profiles exhibit a broad component coming from the shocks along the cavity walls associated with the protostars, and an infalling (or expansion for IRAS05358+3543) and passively heated envelope component, with highly supersonic turbulence likely increasing with the distance from the center. Accretion rates between 6.3 10^{-5} and 5.6 10^{-4} \msun yr^{-1} are derived from the infall observed in three of our sources. The outer water abundance is estimated to be at the typical value of a few 10^{-8} while the inner abundance varies from 1.7 10^{-6} to 1.4 10^{-4} with respect to H2 depending on the source. We confirm that regions of massive star formation are highly turbulent and that the turbulence likely increases in the envelope with the distance to the star. The inner abundances are lower than the expected 10^{-4} perhaps because our observed lines do not probe deep enough into the inner envelope, or because photodissociation through protostellar UV photons is more efficient than expected. We show that the higher the infall/expansion velocity in the protostellar envelope, the higher is the inner abundance, maybe indicating that larger infall/expansion velocities generate shocks that will sputter water from the ice mantles of dust grains in the inner region. High-velocity water must be formed in the gas-phase from shocked material.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enHerschel-HIFI view of mid-IR quiet massive protostellar objects
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201527786
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1601.04599
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA139
bordeaux.volume587
bordeaux.peerReviewedoui
hal.identifierhal-01258410
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01258410v1
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