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Water in star-forming regions with Herschel (WISH): II. Evolution of 557 GHz 110-101 emission in low-mass protostars

hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorKRISTENSEN, L. E.
hal.structure.identifierLeiden Observatory [Leiden]
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
dc.contributor.authorVAN DISHOECK, E. F.
hal.structure.identifierDepartment of Astronomy [Ann Arbor]
dc.contributor.authorBERGIN, E. A.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorVISSER, R.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorYILDIZ, U. A.
dc.contributor.authorJOSE-GARCIA, I. San
dc.contributor.authorJORGENSEN, J. K.
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
dc.contributor.authorHERCZEG, G. J.
hal.structure.identifierNatl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada
dc.contributor.authorJOHNSTONE, D.
hal.structure.identifierInstitute of Astronomy [ETH Zürich]
dc.contributor.authorWAMPFLER, S. F.
hal.structure.identifierInstitute of Astronomy [ETH Zürich]
dc.contributor.authorBENZ, A. O.
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
dc.contributor.authorBRUDERER, S.
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.identifierDepartment of Physics and Astronomy [Granville, OH]
dc.contributor.authorDOTY, S. D.
dc.contributor.authorHARSONO, D.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorHERPIN, Fabrice
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorHOGERHEIJDE, M. R.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorKARSKA, A.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorVAN KEMPEN, T. A.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorLISEAU, R.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorNISINI, B.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorTAFALLA, M.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorVAN DER TAK, F.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.
dc.date.created2012-03-30
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEn(Abridged) Water is a key tracer of dynamics and chemistry in low-mass protostars, but spectrally resolved observations have so far been limited in sensitivity and angular resolution. In this first systematic survey of spectrally resolved water emission in low-mass protostellar objects, H2O was observed in the ground-state transition at 557 GHz with HIFI on Herschel in 29 embedded Class 0 and I protostars. Complementary far-IR and sub-mm continuum data (including PACS data from our program) are used to constrain the spectral energy distribution of each source. H2O intensities are compared to inferred envelope and outflow properties and CO 3-2 emission. H2O emission is detected in all objects except one. The line profiles are complex and consist of several kinematic components. The profiles are typically dominated by a broad Gaussian emission feature, indicating that the bulk of the water emission arises in outflows, not the quiescent envelope. Several sources show multiple shock components in either emission or absorption, thus constraining the internal geometry of the system. Furthermore, the components include inverse P-Cygni profiles in 7 sources (6 Class 0, 1 Class I) indicative of infalling envelopes, and regular P-Cygni profiles in 4 sources (3 Class I, 1 Class 0) indicative of expanding envelopes. "Bullets" moving at >50 km/s are seen in 4 Class 0 sources; 3 of these are new detections. In the outflow, the H2O/CO abundance ratio as a function of velocity is nearly the same for all sources, increasing from 10^-3 at <5 km/s to >10^-1 at >10 km/s. The H2O abundance in the outer envelope is low, ~10^-10. The different H2O profile components show a clear evolutionary trend: in the Class 0 sources, emission is dominated by outflow components originating inside an infalling envelope. When the infall diminishes during the Class I phase, the outflow weakens and H2O emission disappears.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enGalaxy Astrophysics
dc.subject.enAstrophysics
dc.subject.enSolar and Stellar Astrophysics
dc.title.enWater in star-forming regions with Herschel (WISH): II. Evolution of 557 GHz 110-101 emission in low-mass protostars
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201118146
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1204.0009
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA8
bordeaux.volume542
bordeaux.peerReviewedoui
hal.identifierhal-00685396
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00685396v1
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