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Water in star-forming regions with Herschel (WISH). VI. Constraints on UV and X-ray irradiation from a survey of hydrides in low- to high-mass young stellar objects

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.identifierLeiden Observatory [Leiden]
dc.contributor.authorVAN DISHOECK, E. F.,
hal.structure.identifierInstitut Pierre Louis d'Epidémiologie et de Santé Publique [iPLESP]
dc.contributor.authorMELCHIOR, M.,
hal.structure.identifierInstitute of Astronomy [ETH Zürich]
dc.contributor.authorWAMPFLER, S. F.,
hal.structure.identifierSRON Netherlands Institute for Space Research [SRON]
dc.contributor.authorVAN DER TAK, F.,
hal.structure.identifierInstituto de Ciencia de Materiales de Madrid [ICMM]
dc.contributor.authorGOICOECHEA, J. R.,
dc.contributor.authorINDRIOLO, N.,
hal.structure.identifierBergen University College
dc.contributor.authorKRISTENSEN, L. E.,
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorLIS, D. C.,
dc.contributor.authorMOTTRAM, J. C.,
hal.structure.identifierDepartment of Astronomy University of Michigan
dc.contributor.authorBERGIN, E. A.,
dc.contributor.authorCASELLI, P.,
hal.structure.identifierFORMATION STELLAIRE 2016
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.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.identifierPlant Breeding
dc.contributor.authorVISSER, R.,
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.,
dc.date.issued2016-05
dc.identifier.issn0275-1062
dc.description.abstractEnContext. Hydrides are simple compounds containing one or a few hydrogen atoms bonded to a heavier atom. They are fundamental precursor molecules in cosmic chemistry and many hydride ions have become observable in high quality for the first time thanks to the Herschel Space Observatory. Ionized hydrides such as CH+ and OH+ (and also HCO+), which affect the chemistry of molecules such as water, provide complementary information on irradiation by far-UV (FUV) or X-rays and gas temperature. Aims: We explore hydrides of the most abundant heavier elements in an observational survey covering young stellar objects (YSOs) with different mass and evolutionary state. The focus is on hydrides associated with the dense protostellar envelope and outflows, contrary to previous work that focused on hydrides in diffuse foreground clouds. Methods: Twelve YSOs were observed with HIFI on Herschel in six spectral settings providing fully velocity-resolved line profiles as part of the Water in star-forming regions with Herschel (WISH) program. The YSOs include objects of low (Class 0 and I), intermediate, and high mass, with luminosities ranging from 4 L⊙ to 2 × 105 L⊙. Results: The targeted lines of CH+, OH+, H2O+, C+, and CH are detected mostly in blue-shifted absorption. H3O+ and SH+ are detected in emission and only toward some high-mass objects. The observed line parameters and correlations suggest two different origins related to gas entrained by the outflows and to the circumstellar envelope. The derived column densities correlate with bolometric luminosity and envelope mass for all molecules, best for CH, CH+, and HCO+. The column density ratios of CH+/OH+ are estimated from chemical slab models, assuming that the H2 density is given by the specific density model of each object at the beam radius. For the low-mass YSOs the observed ratio can be reproduced for an FUV flux of 2-400 times the interstellar radiation field (ISRF) at the location of the molecules. In two high-mass objects, the UV flux is 20-200 times the ISRF derived from absorption lines, and 300-600 ISRF using emission lines. Upper limits for the X-ray luminosity can be derived from H3O+ observations for some low-mass objects. Conclusions: If the FUV flux required for low-mass objects originates at the central protostar, a substantial FUV luminosity, up to 1.5 L⊙, is required. There is no molecular evidence for X-ray induced chemistry in the low-mass objects on the observed scales of a few 1000 AU. For high-mass regions, the FUV flux required to produce the observed molecular ratios is smaller than the unattenuated flux expected from the central object(s) at the Herschel beam radius. This is consistent with an FUV flux reduced by circumstellar extinction or by bloating of the protostar.Herschel is an ESA space observatory with science instruments provided by a European-led Principal Investigator consortia and with important participation from NASA.
dc.language.isoen
dc.publisherElsevier
dc.subject.enstars: low-mass
dc.subject.enstars: formation
dc.subject.enultraviolet: ISM
dc.subject.enstars: massive
dc.subject.enISM: molecules
dc.subject.enastrochemistry
dc.title.enWater in star-forming regions with Herschel (WISH). VI. Constraints on UV and X-ray irradiation from a survey of hydrides in low- to high-mass young stellar objects
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201525835
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1603.08721
bordeaux.journalChinese Astronomy and Astrophysics
bordeaux.pageA105
bordeaux.volume590
bordeaux.peerReviewedoui
hal.identifierhal-01323874
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01323874v1
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