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Temperature structu...
Temperature structure and kinematics of the IRDC G035.39-00.33
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- Sokolov, V. (författare)
- Max-Planck-Institut für extraterrestrische Physik,Max Planck Institute for Extraterrestrial Physics
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- Wang, K. (författare)
- European Southern Observatory (ESO)
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- Pineda, J.E. (författare)
- Max-Planck-Institut für extraterrestrische Physik,Max Planck Institute for Extraterrestrial Physics
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- Caselli, P. (författare)
- Max-Planck-Institut für extraterrestrische Physik,Max Planck Institute for Extraterrestrial Physics
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- Henshaw, J.D. (författare)
- Liverpool John Moores University
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- Tan, Jonathan (författare)
- University of Florida
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- Fontani, F. (författare)
- Istituto nazionale di astrofisica (INAF)
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- Jiménez-Serra, I. (författare)
- Queen Mary University of London
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- Lim, W. (författare)
- University of Florida
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(creator_code:org_t)
- 2017-10-25
- 2017
- Engelska.
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Ingår i: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 606
- Relaterad länk:
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https://www.aanda.or...
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https://doi.org/10.1...
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https://research.cha...
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Abstract
Ämnesord
Stäng
- © ESO, 2017. Aims. Infrared dark clouds represent the earliest stages of high-mass star formation. Detailed observations of their physical conditions on all physical scales are required to improve our understanding of their role in fueling star formation. Methods. We investigate the large-scale structure of the IRDC G035.39-00.33, probing the dense gas with the classical ammonia thermometer. This allows us to put reliable constraints on the temperature of the extended, pc-scale dense gas reservoir and to probe the magnitude of its non-Thermal motions. Available far-infrared observations can be used in tandem with the observed ammonia emission to estimate the total gas mass contained in G035.39-00.33. Results. We identify a main velocity component as a prominent filament, manifested as an ammonia emission intensity ridge spanning more than 6 pc, consistent with the previous studies on the Northern part of the cloud. A number of additional line-of-sight components are found, and a large-scale linear velocity gradient of ~ 0.2km s -1 pc -1 is found along the ridge of the IRDC. In contrast to the dust temperature map, an ammonia-derived kinetic temperature map, presented for the entirety of the cloud, reveals local temperature enhancements towards the massive protostellar cores. We show that without properly accounting for the line of sight contamination, the dust temperature is 2-3 K larger than the gas temperature measured with NH 3 . Conclusions. While both the large-scale kinematics and temperature structure are consistent with that of starless dark filaments, the kinetic gas temperature profile on smaller scales is suggestive of tracing the heating mechanism coincident with the locations of massive protostellar cores.
Ämnesord
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Nyckelord
- ISM: kinematics and dynamics
- Stars: formation
- ISM: individual objects: G035.39-00.33
- ISM: clouds
Publikations- och innehållstyp
- art (ämneskategori)
- ref (ämneskategori)
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