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Water in star forming regions with Herschel (WISH) III. Far-infrared cooling lines in low-mass young stellar objects

hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorKARSKA, A.
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
dc.contributor.authorHERCZEG, G. J.
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorVAN DISHOECK, E. F.
hal.structure.identifierInstitute of Astronomy [ETH Zürich]
dc.contributor.authorWAMPFLER, S. F.
hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorKRISTENSEN, L. E.
hal.structure.identifierCentro de Astrobiologia [Madrid] [CAB]
dc.contributor.authorGOICOECHEA, J. R.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorVISSER, R.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorNISINI, B.
dc.contributor.authorGARCIA, I. San-Jose
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
dc.contributor.authorBRUDERER, S.
dc.contributor.authorSNIADY, P.
dc.contributor.authorDOTY, S.
dc.contributor.authorFEDELE, D.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorYILDIZ, U. A.
hal.structure.identifierInstitute of Astronomy [ETH Zürich]
dc.contributor.authorBENZ, A. O.
hal.structure.identifierDepartment of Astronomy [Ann Arbor]
dc.contributor.authorBERGIN, E.
hal.structure.identifierINAF - Osservatorio Astrofisico di Arcetri [OAA]
dc.contributor.authorCASELLI, P.
hal.structure.identifierFORMATION STELLAIRE 2013
dc.contributor.authorHERPIN, Fabrice
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorHOGERHEIJDE, M. R.
hal.structure.identifierNatl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada
dc.contributor.authorJOHNSTONE, D.
dc.contributor.authorJORGENSEN, J. K.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorLISEAU, R.
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.created2013-01-21
dc.date.issued2013
dc.identifier.issn0004-6361
dc.description.abstractEn(Abridged) Far-infrared Herschel-PACS spectra of 18 low-mass protostars of various luminosities and evolutionary stages are studied. We quantify their far-infrared line emission and the contribution of different atomic and molecular species to the gas cooling budget during protostellar evolution. We also determine the spatial extent of the emission and investigate the underlying excitation conditions. Most of the protostars in our sample show strong atomic and molecular far-infrared emission. Water is detected in 17 objects, including 5 Class I sources. The high-excitation H2O line at 63.3 micron is detected in 7 sources. CO transitions from J=14-13 up to 49-48 are found and show two distinct temperature components on Boltzmann diagrams with rotational temperatures of ~350 K and ~700 K. H2O has typical excitation temperatures of ~150 K. Emission from both Class 0 and I sources is usually spatially extended along the outflow direction but with a pattern depending on the species and the transition. The H2O line fluxes correlate strongly with those of the high-J CO lines, as well as with the bolometric luminosity and envelope mass. They correlate less strongly with OH and not with [OI] fluxes. The PACS data probe at least two physical components. The H2O and CO emission likely arises in non-dissociative (irradiated) shocks along the outflow walls with a range of pre-shock densities. Some OH is also associated with this component, likely resulting from H2O photodissociation. UV-heated gas contributes only a minor fraction to the CO emission observed by PACS, based on the strong correlation between the shock-dominated CO 24-23 line and the CO 14-13 line. [OI] and some of the OH emission probe dissociative shocks in the inner envelope. The total far-infrared cooling is dominated by H2O and CO, with [OI] increasing for Class I sources.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enSolar and Stellar Astrophysics
dc.subject.enAstrophysics
dc.subject.enGalaxy Astrophysics
dc.title.enWater in star forming regions with Herschel (WISH) III. Far-infrared cooling lines in low-mass young stellar objects
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201220028
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.arxiv1301.4821
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA141
bordeaux.volume552
bordeaux.peerReviewedoui
hal.identifierhal-00786919
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00786919v1
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