Volume 561, January 2014
|Number of page(s)||10|
|Section||Interstellar and circumstellar matter|
|Published online||06 January 2014|
School of Physics & Astronomy, Cardiff University,
Queens Buildings, The parade,
2 Laboratoire AIM, CEA/DSM-CNRS-Universté Paris Diderot, IRFU/Service d’Astrophysique, C. E. Saclay, 91191 Gif-sur-Yvette Cedex, France
3 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester, M13 9PL, UK
4 IAS, CNRS (UMR 8617), Université Paris-Sud, Bâtiment 121, 91400 Orsay, France
5 Centro de Astrobiología (CSIC-INTA), Ctra. de Torrejón-Ajalvir, km. 4, 28850 Torrejón de Ardoz, Madrid, Spain
6 Institut de Radioastronomie Millimétrique, 300 Rue de la piscine, 38406 Saint-Martin-d’Hères, France
7 Universidad de Granada, 18071 Granada, Spain
8 Max-Planck Institut für Radioastronomie, Auf dem Hügel, 69, 53121 Bonn, Germany
9 School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK
10 Departamento de Astronomía, Universidad de Chile, 36-D Casilla, Santiago, Chile
11 Instituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, Spain
12 Universidad de la Laguna, Dept. Astrofisica, 38206 La Laguna, Tenerife, Spain
13 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Herts, AL10 9AB, UK
Accepted: 31 October 2013
Formation of stars is now believed to be tightly linked to the dynamical evolution of interstellar filaments in which they form. In this paper we analyze the density structure and kinematics of a small network of infrared dark filaments, SDC13, observed in both dust continuum and molecular line emission with the IRAM 30 m telescope. These observations reveal the presence of 18 compact sources amongst which the two most massive, MM1 and MM2, are located at the intersection point of the parsec-long filaments. The dense gas velocity and velocity dispersion observed along these filaments show smooth, strongly correlated, gradients. We discuss the origin of the SDC13 velocity field in the context of filament longitudinal collapse. We show that the collapse timescale of the SDC13 filaments (from 1 Myr to 4 Myr depending on the model parameters) is consistent with the presence of Class I sources in them, and argue that, on top of bringing more material to the centre of the system, collapse could generate additional kinematic support against local fragmentation, helping the formation of starless super-Jeans cores.
Key words: stars: formation / ISM: clouds / ISM: kinematics and dynamics / ISM: structure
Based on observations carried out with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).
Figure 3 and Appendices are available in electronic form at http://www.aanda.org
The FITS files for the N2H+(1–0) Spectra of Fig. 3 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/561/A83
© ESO, 2014
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