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Disk fragmentation in high-mass star formation

hal.structure.identifierUniversität zu Köln = University of Cologne
dc.contributor.authorSURI, S.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorBEUTHER, H.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorGIESER, C.
hal.structure.identifierUniversiteit Leiden = Leiden University
dc.contributor.authorAHMADI, A.
hal.structure.identifierUniversität zu Köln = University of Cologne
dc.contributor.authorSÁNCHEZ-MONGE, Á.
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorWINTERS, J.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorLINZ, H.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorHENNING, Th.
hal.structure.identifierINAF - Osservatorio Astrofisico di Arcetri [OAA]
dc.contributor.authorBELTRÁN, M.
dc.contributor.authorBOSCO, F.
hal.structure.identifierINAF - Osservatorio Astrofisico di Arcetri [OAA]
dc.contributor.authorCESARONI, R.
hal.structure.identifierFEMIS 2021
dc.contributor.authorCSENGERI, T.
hal.structure.identifierAcademia Sinica Institute of Astronomy and Astrophysics [ASIAA]
hal.structure.identifierChinese Academy of Sciences [Beijing] [CAS]
hal.structure.identifierNational Astronomical Observatory of Japan [NAOJ]
dc.contributor.authorFENG, S.
dc.contributor.authorHOARE, M.
dc.contributor.authorJOHNSTON, K.
hal.structure.identifierRoyal Observatory Edinburgh [ROE]
dc.contributor.authorKLAASSEN, P.
hal.structure.identifierEberhard Karls Universität Tübingen = University of Tübingen
dc.contributor.authorKUIPER, R.
hal.structure.identifierINAF - Osservatorio Astronomico di Cagliari [OAC]
dc.contributor.authorLEURINI, S.
hal.structure.identifierAstrophysics Research Institute [Liverpool] [ARI]
dc.contributor.authorLONGMORE, S.
hal.structure.identifierUniversity of Leeds
dc.contributor.authorLUMSDEN, S.
dc.contributor.authorMAUD, L.
dc.contributor.authorMOSCADELLI, L.
dc.contributor.authorMÖLLER, T.
dc.contributor.authorPALAU, A.
dc.contributor.authorPETERS, T.
dc.contributor.authorPUDRITZ, R.
dc.contributor.authorRAGAN, S.
dc.contributor.authorSEMENOV, D.
dc.contributor.authorSCHILKE, P.
dc.contributor.authorURQUHART, J.
dc.contributor.authorWYROWSKI, F.
dc.contributor.authorZINNECKER, H.
dc.date.issued2021-11
dc.identifier.issn0004-6361
dc.description.abstractEnContext. Increasing evidence suggests that, similar to their low-mass counterparts, high-mass stars form through a disk-mediated accretion process. At the same time, formation of high-mass stars still necessitates high accretion rates, and hence, high gas densities, which in turn can cause disks to become unstable against gravitational fragmentation. Aims. We study the kinematics and fragmentation of the disk around the high-mass star forming region AFGL 2591-VLA 3 which was hypothesized to be fragmenting based on the observations that show multiple outflow directions. Methods. We use a new set of high-resolution (0′′.19) IRAM/NOEMA observations at 843 μm towards VLA 3 which allow us to resolve its disk, characterize the fragmentation, and study its kinematics. In addition to the 843 μm continuum emission, our spectral setup targets warm dense gas and outflow tracers such as HCN, HC 3 N and SO 2 , as well as vibrationally excited HCN lines. Results. The high resolution continuum and line emission maps reveal multiple fragments with subsolar masses within the inner ~1000 AU of VLA 3. Furthermore, the velocity field of the inner disk observed at 843 μm shows a similar behavior to that of the larger scale velocity field studied in the CORE project at 1.37 mm. Conclusions. We present the first observational evidence for disk fragmentation towards AFGL 2591-VLA 3, a source that was thought to be a single high-mass core. While the fragments themselves are low-mass, the rotation of the disk is dominated by the protostar with a mass of 10.3 ± 1.8 M ⊙ . These data also show that NOEMA Band 4 can obtain the highest currently achievable spatial resolution at (sub-)mm wavelengths in observations of strong northern sources.
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.title.enDisk fragmentation in high-mass star formation
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202140963
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.subject.halPlanète et Univers [physics]
dc.identifier.arxiv2109.04751
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA84
bordeaux.volume655
bordeaux.issue2
bordeaux.peerReviewedoui
hal.identifierhal-03799860
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03799860v1
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