The molecular distribution of the IRDC G351.77–0.51
S. Leurini1, T. Pillai2,3, T. Stanke4, F. Wyrowski1, L. Testi4,5, F. Schuller1, K. M. Menten1 and S. Thorwirth6
Max-Planck-Institut für Radioastronomie,
Auf dem Hügel 69,
2 Caltech, 1200 E. California Blvd, Pasadena, CA 91125, USA
3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
4 ESO, Karl-Schwarzschild Strasse 2, 85748 Garching-bei-München, Germany
5 INAF - Osservatorio Astrofisico di Arcetri, Largo Fermi 5, 50125 Firenze, Italy
6 I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
Received: 21 December 2010
Accepted: 11 July 2011
Context. Infrared dark clouds are massive, dense clouds seen in extinction against the IR Galactic background. Many of these objects appear to be on the verge of star and star cluster formation.
Aims. Our aim is to understand the physical properties of IRDCs in very early evolutionary phases. We selected the filamentary IRDC G351.77−0.51, which is remarkably IR quiet at 8 μm.
Methods. As a first step, we observed mm dust continuum emission and rotational lines of moderate and dense gas tracers to characterise different condensations along the IRDC and study the velocity field of the filament.
Results. Our initial study confirms coherent velocity distribution along the infrared dark cloud ruling out any coincidental projection effects. Excellent correlation between MIR extinction, mm continumm emission and gas distribution is found. Large-scale turbulence and line profiles throughout the filament is indicative of a shock in this cloud. Excellent correlation between line width and MIR brightness indicates turbulence driven by local star formation.
Key words: ISM: clouds / stars: formation / stars: protostars / ISM: individual objects: G351.77-0.51
© ESO, 2011