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Anatomy of the massive star-forming region S106. The [O I] 63 μm line observed with GREAT/SOFIA as a versatile diagnostic tool for the evolution of massive stars

hal.structure.identifierI. Physikalisches Institut [Köln]
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierPhysikalisches Institut [Köln]
dc.contributor.authorROELLIG, M.
dc.contributor.authorSIMON, R.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWIESEMEYER, H.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA (UMR_8112)]
dc.contributor.authorGUSDORF, A.
dc.contributor.authorSTUTZKI, J.
dc.contributor.authorGUESTEN, R.
hal.structure.identifierFormation Stellaire
dc.contributor.authorBONTEMPS, S.
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorCOMERÓN, F.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorCSENGERI, T.
dc.contributor.authorADAMS, J. D.
dc.contributor.authorRICHTER, H.
dc.date.issued2018
dc.identifier.issn0004-6361
dc.description.abstractEnThe central area (40"x40") of the bipolar nebula S106 was mapped in the OI line at 63.2 micron with high angular (6") and spectral resolution, using GREAT on board SOFIA. The OI emission distribution is compared to the CO 16-15, CII 158 micron, and CO 11-10 lines, mm-molecular lines, and continuum. It is composed of several velocity components in the range from -30 km/s to 25 km/s. The high-velocity blue- and redshifted emission can be explained as arising from accelerated photodissociated (PDR) gas associated with a dark lane close to the massive binary system S106 IR, and from shocks caused by the stellar wind and/or a disk--envelope interaction. At velocities from -9 to -4 km/s and 0.5 to 8 km/s line wings are observed that we attribute to cooling in PDRs created by the ionizing radiation impinging on the cavity walls. The bulk velocity range is dominated by PDR emission from the clumpy molecular cloud. Modelling the emission in the different velocity ranges with the KOSMA-tau code constrains a radiation field chi of a few times 10^4 and densities n of a few times 10^4 cm^-3. Considering self-absorption of the OI line results in higher densities (up to 10^6 cm^-3) only for the gas component seen at high blue- and red velocities. The dark lane has a mass of 275 Msun and shows a velocity difference of 1.4 km/s along its projected length of 1 pc, determined from H13CO+ 1-0 mapping. It can be interpreted as a massive accretion flow, or the remains of it, linked to S106 IR/FIR. The most likely explanation is that the binary system is at a stage of its evolution where gas accretion is counteracted by the stellar winds and radiation, leading to the very complex observed spatial and kinematic emission distribution of the various tracers.
dc.description.sponsorshipGENeration et Evolution des Structures du milieu InterStellaire - ANR-16-CE92-0035
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enAnatomy of the massive star-forming region S106. The [O I] 63 μm line observed with GREAT/SOFIA as a versatile diagnostic tool for the evolution of massive stars
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201732508
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1806.00991
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A45
bordeaux.volume617
bordeaux.peerReviewedoui
hal.identifierhal-01807753
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01807753v1
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