The Molecular Accretion Flow in G10.6-0.4

Details The Molecular Accretion Flow in G10.6-0.4 The Molecular Accretion Flow in G10.6-0.4

2005-06-02

arxiv.org/abs/astro-ph/0506057v1

Astrophys.J. 630 (2005) 987-995

Astronomy and Astrophysics

Astrophysics

20 pages, 6 figures Accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/432254

We have observed the ultracompact HII region G10.6-0.4 with the VLA in 23 GHz continuum and the NH3(3,3) inversion line. By analyzing the optical depth of the line as well as the kinematics, we have detected a flattened, rotating, molecular accretion flow. We detect the fact that the highest column density gas is more flattened, that is, distributed more narrowly, than the lower column density gas, and that there is some inclination of the rotation axis. The rotation is sub-Keplerian, and the molecular gas is not in a rotationally supported disk. We do not find a single massive (proto)star forming in a scaled up version of low mass star formation. Instead, our observations suggest a different mode of clustered massive star formation, in which the accretion flow flattens but does not form an accretion disk. Also in this mode of star formation the central object can be a group of massive stars rather than a single massive star.

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