Show simple item record

dc.contributor.authorSAN JOSE-GARCIA, I.,
dc.contributor.authorMOTTRAM, J. C.,
hal.structure.identifierLeiden Observatory [Leiden]
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
dc.contributor.authorVAN DISHOECK, E. F.,
hal.structure.identifierDanish Meat Research Institute [DMRI]
dc.contributor.authorKRISTENSEN, L. E.,
hal.structure.identifierSRON Netherlands Institute for Space Research [SRON]
dc.contributor.authorVAN DER TAK, F. F. S.,
hal.structure.identifierFORMATION STELLAIRE 2016
dc.contributor.authorBRAINE, J.
hal.structure.identifierFORMATION STELLAIRE 2016
dc.contributor.authorHERPIN, Fabrice
hal.structure.identifierNatl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada
dc.contributor.authorJOHNSTONE, D.,
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorVAN KEMPEN, T. A.,
dc.contributor.authorWYROWSKI, F.,
dc.date.issued2016
dc.identifier.issn0004-6361
dc.description.abstractEnWater probes the dynamics in young stellar objects (YSOs) effectively, especially shocks in molecular outflows. It is a key molecule for exploring whether the physical properties of low-mass protostars can be extrapolated to massive YSOs. As part of the WISH key programme, we investigate the dynamics and the excitation conditions of shocks along the outflow cavity wall as function of source luminosity. Velocity-resolved Herschel-HIFI spectra of the H2O 988, 752, 1097 GHz and 12CO J=10-9, 16-15 lines were analysed for 52 YSOs with bolometric luminosities (L_bol) ranging from <1 to >10^5 L_sun. The profiles of the H2O lines are similar, indicating that they probe the same gas. We see two main Gaussian emission components in all YSOs: a broad component associated with non-dissociative shocks in the outflow cavity wall (cavity shocks) and a narrow component associated with quiescent envelope material. More than 60% of the total integrated intensity of the H2O lines (L_H2O) comes from the cavity shock component. The H2O line widths are similar for all YSOs, whereas those of 12CO 10-9 increase slightly with L_bol. The excitation analysis of the cavity shock component, performed with the non-LTE radiative transfer code RADEX, shows stronger 752 GHz emission for high-mass YSOs, likely due to pumping by an infrared radiation field. As previously found for CO, a strong correlation with slope unity is measured between log(L_H2O) and log(L_bol), which can be extrapolated to extragalactic sources. We conclude that the broad component of H2O and high-J CO lines originate in shocks in the outflow cavity walls for all YSOs, whereas lower-J CO transitions mostly trace entrained outflow gas. The higher UV field and turbulent motions in high-mass objects compared to their low-mass counterparts may explain the slightly different kinematical properties of 12CO 10-9 and H2O
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enLinking low- to high-mass YSOs with Herschel-HIFI observations of water
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201525708
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1511.00357
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A103
bordeaux.volume585
bordeaux.peerReviewedoui
hal.identifierhal-01223685
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01223685v1
bordeaux.COinSctx_ver=Z39.88-2004&amp;rft_val_fmt=info:ofi/fmt:kev:mtx:journal&amp;rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&amp;rft.date=2016&amp;rft.volume=585&amp;rft.spage=id.A103&amp;rft.epage=id.A103&amp;rft.eissn=0004-6361&amp;rft.issn=0004-6361&amp;rft.au=SAN%20JOSE-GARCIA,%20I.,&amp;MOTTRAM,%20J.%20C.,&amp;VAN%20DISHOECK,%20E.%20F.,&amp;KRISTENSEN,%20L.%20E.,&amp;VAN%20DER%20TAK,%20F.%20F.%20S.,&amp;rft.genre=article


Files in this item

FilesSizeFormatView

There are no files associated with this item.

This item appears in the following Collection(s)

Show simple item record