Authors
Abstract
We have mapped the central region of the HH 111 protostellar system in 1.33 mm continuum, C18O (J = 2 - 1), 13CO (J = 2 - 1), and SO (NJ = 56 - 45) emissions at ~3'' resolution with the Submillimeter Array. There are two sources, VLA 1 (=IRAS 05491+0247) and VLA 2, with the VLA 1 source driving the HH 111 jet. Thermal emission is seen in 1.33 mm continuum tracing the dust in the envelope and the putative disks around the sources. A flattened, toruslike envelope is seen in C18O and 13CO around the VLA 1 source surrounding the dust lane perpendicular to the jet axis, with an inner radius of ~400 AU (1''), an outer radius of ~3200 AU (8''), and a thickness of ~1000 AU (2farcs5). It seems to be infalling toward the center with the conservation of specific angular momentum rather than with a Keplerian rotation as assumed by Yang et al. An inner envelope is seen in SO, with a radius of ~500 AU (1farcs3). The inner part of this inner envelope, which is spatially coincident with the dust lane, seems to have a differential rotation and thus may have formed a rotationally supported disk. The outer part of this inner envelope, however, may have a rotation velocity decreasing toward the center and thus represent a region where an infalling envelope is in transition to a rotationally supported disk. A brief comparison with a collapsing model suggests that the flattened, toruslike envelope seen in C18O and 13CO could result from a collapse of a magnetized rotating toroid.Details
| Publication | The Astrophysical Journal, Volume 694, Issue 2, pp. 1395-1401 (2009). |
| Publication Date | April 2009 |
| DOI | |
| arXiv | arXiv:0812.4877 |
| Bibcode | 2009ApJ...694.1395L |
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| E-Print Comment(s) | 17 pages, 6 figures. Accepted by the ApJ; Astrophys.J.694:1395-1401,2009; Erratum-ibid.700:898,2009; doi:10.1088/0004-637X/694/2/1395; doi:10.1088/0004-637X/700/1/898 |