Shinnaga, Hiroko and Phillips, Thomas G. and Furuya, Ray S. and Cesaroni, Riccardo (2008) Submillimeter observations of the isolated massive dense clump IRAS 20126+4104. Astrophysical Journal, 682 (2). pp. 1103-1113. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20090427-093617847
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We imaged the 350 and 450 μm continuum and CO J = 6–5 line emission of the IRAS 20126+4104 clump at the CSO. The continuum and line observations show that the clump has a radius of ~0.5 pc. The clump has a radial density profile α r^(−1.2) for r ≾ 0.1 pc and has α r^(−2.3) for r ≳ 0.1 pc, which suggests that the inner region is infalling, while the infall wave has not yet reached the outer region. Based on the 350 μm/450 μm flux ratio map, three distinct regions are identified: a bipolar feature that coincides with the large scale CO bipolar outflow; a cocoon-like region that encases the bipolar feature and has a warm surface; and a cold layer outside of the cocoon region. The complex flux ratio pattern indicates that the clump is no longer uniform in terms of temperature as well as dust properties. The CO emission near the systemic velocity traces the dense clump and the outer layer of the clump shows narrow line widths (≾3 km s^(−1)). The clump has a velocity gradient of ~2 km s^(−1) pc^(−1), which we interpret as due to rotation of the clump, as the equilibrium mass (~200 M⊙) is comparable to the LTE mass. Over a scale of ~1 pc, the clump rotates in the opposite sense with respect to the ≾0.03 pc disk associated with the (proto)star. This is one of four objects in high-mass and low-mass star-forming regions for which a discrepancy between the rotation sense of the envelope and the core has been found, suggesting that such a complex kinematics may not be unusual in star-forming regions.
|Additional Information:||© 2008 The American Astronomical Society. Received 2007 September 17; accepted 2008 April 10. This research was performed at the Caltech Submillimeter Observatory, supported by NSF grant AST-0229008. H. S. is grateful to Hiroshige Yoshida for the observational support in 2004 July and Debra Shepherd and J. H. Kawamura for providing us their data. H. S. is indebted to Peter Schilke for his LVG code. Thanks are also due to Thomas A. Bell, John Carpenter, and Roger Hildebrand for valuable comments and discussions. H. S. also thanks the Gildas development team (http://www.iram.fr/IRAMFR/GILDAS), which provides us their data reduction packages. We thank the Hawaiian people for allowing us to observe from the summit of their sacred mountain, Mauna Kea. Facilities: CSO|
|Subject Keywords:||infrared: ISM; ISM: clouds; ISM: jets and outflows; ISM: kinematics and dynamics; ISM: lines and bands; radio continuum: ISM; radio lines: ISM; stars: formation|
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|Deposited By:||Tony Diaz|
|Deposited On:||07 Aug 2009 18:26|
|Last Modified:||26 Dec 2012 10:58|
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