Universität zu Köln

Rolffs, R., Schilke, P., Zhang, Q. and Zapata, L. (2011). Structure of the hot molecular core G10.47+0.03. Astron. Astrophys., 536. LES ULIS CEDEX A: EDP SCIENCES S A. ISSN 0004-6361

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Abstract

Context. The physical structure of hot molecular cores, where forming massive stars have heated up dense dust and gas, but have not yet ionized the molecules, poses a prominent challenge in the research of high-mass star formation and astrochemistry. Aims. We aim at constraining the spatial distribution of density, temperature, velocity field, and chemical abundances in the hot molecular core G10.47+0.03. Methods. With the SubMillimeter Array (SMA), we obtained high spatial and spectral resolution of a multitude of molecular lines at different frequencies, including at 690 GHz. At 345 GHz, our beam size is 0.3 '', corresponding to 3000 AU. We analyze the data using the three-dimensional dust and line radiative transfer code RADMC-3D for vibrationally excited HCN, and myXCLASS for line identification. Results. We find hundreds of molecular lines from complex molecules and high excitations. Even vibrationally excited (HCN)-N-15 at 690 GHz is detected. The HCN abundance at high temperatures is very high, on the order of 10(-5) relative to H-2. Absorption against the dust continuum occurs in twelve transitions, whose shape implies an outflow along the line-of-sight. Outside the continuum peak, the line shapes are indicative of infall. Dust continuum and molecular line emission are resolved at 345/355 GHz, revealing central flattening and rapid radial falloff of the density outwards of 104 AU, best reproduced by a Plummer radial profile of the density. No fragmentation is detected, but modeling of the line shapes of vibrationally excited HCN suggests that the density is clumpy. Conclusions. We conclude that G10.47+0.03 is characterized by beginning of feedback from massive stars, while infall is ongoing. High gas masses (hundreds of M-circle dot) are heated to high temperatures above 300 K, aided by diffusion of radiation in a high-column-density environment. The increased thermal, radiative, turbulent, and wind-driven pressure drives expansion in the central region and is very likely responsible for the central flattening of the density.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Rolffs, R. UNSPECIFIED UNSPECIFIED UNSPECIFIED Schilke, P. UNSPECIFIED UNSPECIFIED UNSPECIFIED Zhang, Q. UNSPECIFIED UNSPECIFIED UNSPECIFIED Zapata, L. UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-484695
DOI:	10.1051/0004-6361/201117112
Journal or Publication Title:	Astron. Astrophys.
Volume:	536
Date:	2011
Publisher:	EDP SCIENCES S A
Place of Publication:	LES ULIS CEDEX A
ISSN:	0004-6361
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language MASSIVE STAR-FORMATION; CONTINUUM OBSERVATIONS; SUBMILLIMETER ARRAY; COLOGNE DATABASE; HII-REGIONS; II REGIONS; SPECTROSCOPY; RESOLUTION; CDMS; LINE Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/48469