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Title:
The inception of star cluster formation revealed by [C II] emission around an Infrared Dark Cloud
Authors:
Bisbas, Thomas G.; Tan, Jonathan C.; Csengeri, Timea; Wu, Benjamin; Lim, Wanggi; Caselli, Paola; Güsten, Rolf; Ricken, Oliver; Riquelme, Denise
Affiliation:
AA(Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA; Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany), AB(Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA; Department of Space, Earth & Environment, Chalmers University of Technology, SE-412 96 Gothenburg, Sweden), AC(Max-Planck-Institut für Radioastronomie, auf dem Hügel 69, D-53121 Bonn, Germany), AD(National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan), AE(SOFIA-USRA, NASA Ames Research Center, MS 232-12, Moffett Field, CA 94035, USA), AF(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany), AG(Max-Planck-Institut für Radioastronomie, auf dem Hügel 69, D-53121 Bonn, Germany), AH(Max-Planck-Institut für Radioastronomie, auf dem Hügel 69, D-53121 Bonn, Germany), AI(Max-Planck-Institut für Radioastronomie, auf dem Hügel 69, D-53121 Bonn, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society: Letters, Volume 478, Issue 1, p.L54-L59 (MNRAS Homepage)
Publication Date:
07/2018
Origin:
OUP
Astronomy Keywords:
radiative transfer, ISM: clouds, ISM: kinematics and dynamics
Abstract Copyright:
2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnrasl/sly039
Bibliographic Code:
2018MNRAS.478L..54B

Abstract

We present SOFIA-upGREAT observations of [C II] emission of Infrared Dark Cloud (IRDC) G035.39-00.33, designed to trace its atomic gas envelope and thus test models of the origins of such clouds. Several velocity components of [C II] emission are detected, tracing structures that are at a wide range of distances in the Galactic plane. We find a main component that is likely associated with the IRDC and its immediate surroundings. This strongest emission component has a velocity similar to that of the 13CO(2-1) emission of the IRDC, but offset by ˜3 km s-1 and with a larger velocity width of ˜9 km s-1. The spatial distribution of the [C II] emission of this component is also offset predominantly to one side of the dense filamentary structure of the IRDC. The C II column density is estimated to be of the order of ˜1017-1018 cm-2. We compare these results to the [C II] emission from numerical simulations of magnetized, dense gas filaments formed from giant molecular cloud (GMC) collisions, finding similar spatial and kinematic offsets. These observations and modellingof [C II] add further to the evidence that IRDC G035.39-00.33 has been formed by a process of GMC-GMC collision, which may thus be an important mechanism for initiating star cluster formation.
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