Sökning: onr:"swepub:oai:research.chalmers.se:fd94a532-90a8-4713-9a8b-ad0ef67e5ee1" > Search for high-mas...
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000 | 07500naa a2200637 4500 | |
001 | oai:research.chalmers.se:fd94a532-90a8-4713-9a8b-ad0ef67e5ee1 | |
003 | SwePub | |
008 | 181015s2018 | |||||||||||000 ||eng| | |
024 | 7 | a https://research.chalmers.se/publication/5055542 URI |
024 | 7 | a https://doi.org/10.1051/0004-6361/2018327532 DOI |
024 | 7 | a https://research.chalmers.se/publication/5063272 URI |
024 | 7 | a https://research.chalmers.se/publication/5054012 URI |
024 | 7 | a https://research.chalmers.se/publication/5053762 URI |
040 | a (SwePub)cth | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a art2 swepub-publicationtype |
072 | 7 | a ref2 swepub-contenttype |
100 | 1 | a Csengeri, T.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut |
245 | 1 0 | a Search for high-mass protostars with ALMA revealed up to kilo-parsec scales (SPARKS): I. Indication for a centrifugal barrier in the environment of a single high-mass envelope |
264 | c 2018-09-21 | |
264 | 1 | b EDP Sciences,c 2018 |
338 | a electronic2 rdacarrier | |
520 | a The conditions leading to the formation of the most massive O-type stars are still an enigma in modern astrophysics. To assess the physical conditions of high-mass protostars in their main accretion phase, here we present a case study of a young massive clump selected from the ATLASGAL survey, G328.2551-0.5321. The source exhibits a bolometric luminosity of 1.3 × 104L·, which allows us to estimate that its current protostellar mass lies between ∼11 and 16 M·. We show high angular resolution observations with ALMA that reach a physical scale of ∼400 au. To reveal the structure of this high-mass protostellar envelope in detail at a ∼0.17′′ resolution, we used the thermal dust continuum emission and spectroscopic information, amongst others from the CO (J = 3-2) line, which is sensitive to the high-velocity molecular outflow of the source. We also used the SiO (J = 8-7) and SO2(J = 82,6-71,7) lines, which trace shocks along the outflow, as well as several CH3OH and HC3N lines that probe the gas of the inner envelope in the closest vicinity of the protostar. Our observations of the dust continuum emission reveal a single high-mass protostellar envelope, down to our resolution limit. We find evidence for a compact, marginally resolved continuum source that is surrounded by azimuthal elongations that could be consistent with a spiral pattern. We also report on the detection of a rotational line of CH3OH within its vt= 1 torsionally excited state. This shows two bright emission peaks that are spatially offset from the dust continuum peak and exhibit a distinct velocity component ±4.5 km s-1offset from the systemic velocity of the source. Rotational diagram analysis and models based on local thermodynamic equilibrium assumption require high CH3OH column densities that reach N(CH3OH) = 1.2-2 × 1019cm-2, and kinetic temperatures of the order of 160-200 K at the position of these peaks. A comparison of their morphology and kinematics with those of the outflow component of the CO line and the SO2line suggests that the high-excitation CH3OH spots are associated with the innermost regions of the envelope. While the HC3N v7= 0 (J = 37-36) line is also detected in the outflow, the HC3N v7= 1e (J = 38-37) rotational transition within the first vibrationally excited state of the molecule shows a compact morphology. We find that the velocity shifts at the position of the observed high-excitation CH3OH spots correspond well to the expected Keplerian velocity around a central object with 15 M·consistent with the mass estimate based on the bolometric luminosity of the source. We propose a picture where the CH3OH emission peaks trace the accretion shocks around the centrifugal barrier, pinpointing the interaction region between the collapsing envelope and an accretion disc. The physical properties of the accretion disc inferred from these observations suggest a specific angular momentum several times higher than typically observed towards low-mass protostars. This is consistent with a scenario of global collapse setting on at larger scales that could carry a more significant amount of kinetic energy compared to the core-collapse models of low-mass star formation. Furthermore, our results suggest that vibrationally excited HC3N emission could be a new tracer for compact accretion discs around high-mass protostars. | |
650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
650 | 7 | a NATURVETENSKAPx Fysikx Atom- och molekylfysik och optik0 (SwePub)103022 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Atom and Molecular Physics and Optics0 (SwePub)103022 hsv//eng |
650 | 7 | a NATURVETENSKAPx Fysikx Annan fysik0 (SwePub)103992 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Other Physics Topics0 (SwePub)103992 hsv//eng |
653 | a Stars: massive | |
653 | a Stars: formation | |
653 | a Submillimeter: ISM | |
653 | a Accretion, accretion disks | |
700 | 1 | a Bontemps, S.u Observatoire Aquitain des Sciences de l'Univers, OASU4 aut |
700 | 1 | a Wyrowski, F.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut |
700 | 1 | a Belloche, A.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut |
700 | 1 | a Menten, K.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut |
700 | 1 | a Leurini, S.u Istituto nazionale di astrofisica (INAF)4 aut |
700 | 1 | a Beuther, H.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut |
700 | 1 | a Bronfman, Leonardou Universidad de Chile (UCH),University of Chile (UCH)4 aut |
700 | 1 | a Commerçon, B.u École Normale Supérieure de Lyon4 aut |
700 | 1 | a Chapillon, E.u Institut de Radioastronomie Millimétrique (IRAM),Observatoire Aquitain des Sciences de l'Univers, OASU4 aut |
700 | 1 | a Longmore, S.u Liverpool John Moores University4 aut |
700 | 1 | a Palau, A.u Universidad Nacional Autónoma de México (UNAM),Universidad Nacional Autonoma de Mexico4 aut |
700 | 1 | a Tan, Jonathan,d 1973u University of Virginia,Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)tanj |
700 | 1 | a Urquhart, J. S.u University Of Kent4 aut |
710 | 2 | a Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG)b Observatoire Aquitain des Sciences de l'Univers, OASU4 org |
773 | 0 | t Astronomy and Astrophysicsd : EDP Sciencesg 617q 617x 0004-6361x 1432-0746 |
856 | 4 | u https://research.chalmers.se/publication/506327/file/506327_Fulltext.pdfx primaryx freey FULLTEXT |
856 | 4 | u https://www.aanda.org/articles/aa/pdf/2018/09/aa32753-18.pdf |
856 | 4 8 | u https://research.chalmers.se/publication/505554 |
856 | 4 8 | u https://doi.org/10.1051/0004-6361/201832753 |
856 | 4 8 | u https://research.chalmers.se/publication/506327 |
856 | 4 8 | u https://research.chalmers.se/publication/505401 |
856 | 4 8 | u https://research.chalmers.se/publication/505376 |
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