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Kinematic and thermal structure at the onset of high-mass star formation - ISOSS23053

Published online by Cambridge University Press:  31 March 2017

Simon Bihr ,
Henrik Beuther ,
Hendrik Linz ,
Sarah E. Ragan ,
Jochen Tackenberg ,
Rowan J. Smith ,
Thomas Henning  and
Oliver Krause
Simon Bihr
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
Henrik Beuther
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
Hendrik Linz
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
Sarah E. Ragan
Affiliation:
School of Physics & Astronomy, The University of Leeds, E.C. Stoner Building, Leeds, LS2 9JT, UK email: [email protected]
Jochen Tackenberg
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
Rowan J. Smith
Affiliation:
Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester, M13 9PL, UK email: [email protected]
Thomas Henning
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
Oliver Krause
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany email: [email protected]
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Abstract

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Within the ‘earliest phases of star formation’ (EPoS) Herschel project, we observed the NH3 inversion lines of 6 very young high-mass star-forming regions at high spatial resolution (3-5″) with the JVLA. While the Herschel data provide details about the dust continuum, the ammonia data reveal the kinematics and temperatures. Here we present the exciting star-forming clump ISOSS23053 that shows multiple velocity components. We observe a prominent velocity step within the clump, which could be a sign of colliding or converging flows that triggers star formation. Furthermore, we used the JVLA in the C-array configuration to study this source in more detail and we present the first results from the new data. They support the idea of converging flows, as we observe two components in the NH3(1,1) and (2,2) line, whereas the higher excited NH3(3,3) line shows one component that links the two lower excited lines.

Keywords

Stars: formation - Stars: massive - ISM: clouds - ISM: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S316: Formation, evolution, and survival of massive star clusters , August 2015 , pp. 125 - 126
Copyright
Copyright © International Astronomical Union 2017 

References

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