An analysis of water line profiles in star formation regions observed by the Submillimeter Wave Astronomy Satellite

被引：27

作者：

Ashby, MLN

Bergin, EA

Plume, R

Carpenter, JM

Neufeld, DA

Chin, G

Erickson, NR

Goldsmith, PF

Harwit, M

Howe, JE

Kleiner, SC

Koch, DG

Patten, BM

Schieder, R

Snell, RL

Stauffer, JR

Tolls, V

Wang, Z

Winnewisser, G

Zhang, YF

Melnick, GJ

机构：

[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[2] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[3] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[4] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[5] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA

[6] Cornell Univ, Natl Astron & Ionosphere Ctr, Dept Astron, Ithaca, NY 14853 USA

[7] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[8] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany

来源：

ASTROPHYSICAL JOURNAL | 2000年 / 539卷 / 02期

基金：

美国国家航空航天局;

关键词：

ISM : clouds; ISM : molecules; radio lines : ISM; stars : formation;

D O I：

10.1086/312842

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present spectral line profiles for the 557 GHz 1(10)-->1(01) ground-state rotational transition of ortho-(H2O)-O-16 for 18 Galactic star formation regions observed by the Submillimeter Wave Astronomy Satellite. Water is unambiguously detected in every source. The line profiles exhibit a wide variety of shapes, including single-peaked spectra and self-reversed profiles. We interpret these profiles using a Monte Carlo code to model the radiative transport. The observed variations in the line profiles can be explained by variations in the relative strengths of the bulk flow and small-scale turbulent motions within the clouds. Bulk flow (infall, outflow) must be present in some cloud cores, and in certain cases this bulk flow dominates the turbulent motions.

引用

页码：L115 / L118

页数：4

共 33 条

[1] Water abundance and velocity structure in S140, ρ Oph A, and B335 [J].