The distribution of water in the high-mass star-forming region NGC 6334 I

被引：30

作者：

Emprechtinger, M. ^{[1
,20
]}

Lis, D. C.

Bell, T.

Phillips, T. G.

Schilke, P. ^{[11
,20
]}

Comito, C. ^{[11
]}

Rolffs, R. ^{[11
]}

van der Tak, F. ^{[16
]}

Ceccarelli, C. ^{[4
]}

Aarts, H. ^{[16
]}

Bacmann, A. ^{[2
,3
,4
]}

Baudry, A. ^{[2
,3
]}

Benedettini, M. ^{[5
]}

Bergin, E. A. ^{[25
]}

Blake, G.

Boogert, A.

Bottinelli, S. ^{[6
,7
]}

Cabrit, S. ^{[9
]}

Caselli, P. ^{[8
]}

Castets, A. ^{[4
]}

Caux, E. ^{[6
,7
]}

Cernicharo, J. ^{[10
]}

Codella, C. ^{[12
]}

Coutens, A.

Crimier, N. ^{[4
,10
]}

Demyk, K. ^{[6
,7
]}

Dominik, C. ^{[13
,14
]}

Encrenaz, P. ^{[9
]}

Falgarone, E. ^{[9
]}

Fuente, A. ^{[15
]}

Gerin, M. ^{[9
]}

Goldsmith, P. ^{[1
]}

Helmich, F. ^{[16
]}

Hennebelle, P. ^{[9
]}

Henning, T. ^{[26
]}

Herbst, E. ^{[17
]}

Hily-Blant, P. ^{[4
]}

Jacq, T. ^{[2
,3
]}

Kahane, C. ^{[4
]}

Kama, M. ^{[13
]}

Klotz, A. ^{[6
,7
]}

Kooi, J.

Langer, W. ^{[1
]}

Lefloch, B. ^{[4
]}

Loose, A. ^{[27
]}

Lord, S.

Lorenzani, A. ^{[12
]}

Maret, S. ^{[4
]}

Melnick, G. ^{[18
]}

Neufeld, D. ^{[19
]}

机构：

[1] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[2] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France

[3] CNRS INSU, UMR 5804, Floirac, France

[4] Univ Grenoble 1, UMR CNRS 5571, Lab Astrophys Grenoble, Grenoble, France

[5] INAF Ist Fis Spazio Interplanetario, Rome, Italy

[6] Univ Toulouse 3, CESR, F-31062 Toulouse, France

[7] CNRS, Toulouse, France

[8] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England

[9] Observ Paris, LERMA UMR CNRS 8112, Meudon, France

[10] CSIC INTA, Ctr Astrobiol, Madrid, Spain

[11] Max Planck Inst Radioastron, D-5300 Bonn, Germany

[12] INAF Osservatorio Astrofis Arcetri, Florence, Italy

[13] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands

[14] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands

[15] IGN Observ Astron Nacl, Alcala De Henares, Spain

[16] Univ Groningen, SRON, Groningen, Netherlands

[17] Ohio State Univ, Columbus, OH 43210 USA

[18] Ctr Astrophys, Cambridge, MA 02138 USA

[19] Johns Hopkins Univ, Baltimore, MD USA

[20] Univ Cologne, Inst Phys, Cologne, Germany

[21] Inst Radio Astron Millimetr, Grenoble, France

[22] Leiden Univ, Leiden Observ, Leiden, Netherlands

[23] UCL, Dept Phys & Astron, London, England

[24] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy

[25] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[26] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[27] Max Planck Inst Sonnenphys Forsch, Lindau, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 521卷

关键词：

stars: formation; ISM: molecules; INTERSTELLAR-MEDIUM; NGC-6334; MASERS; I(N); PROTOSTARS; HIFI; ABUNDANCES; MILLIMETER; OUTFLOW; AMMONIA;

D O I：

10.1051/0004-6361/201015086

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. We present observations of twelve rotational transitions of (H2O)-O-16, (H2O)-O-18, and (H2O)-O-17 toward the massive star-forming region NGC 6334 I, carried out with Herschel/HIFI as part of the guaranteed time key program Chemical HErschel Surveys of Star forming regions (CHESS). We analyze these observations to obtain insights into physical processes in this region. Methods. We identify three main gas components (hot core, cold foreground, and outflow) in NGC 6334 I and derive the physical conditions in these components. Results. The hot core, identified by the emission in highly excited lines, shows a high excitation temperature of similar to 200 K, whereas water in the foreground component is predominantly in the ortho-and para-ground states. The abundance of water varies between 4 x 10(-5) (outflow) and 10(-8) (cold foreground gas). This variation is most likely due to the freeze-out of water molecules onto dust grains. The (H2O)-O-18/(H2O)-O-17 abundance ratio is 3.2, which is consistent with the O-18/O-17 ratio determined from CO isotopologues. The ortho/para ratio in water appears to be relatively low (1.6 +/- 1) in the cold, quiescent gas, but close to the equilibrium value of three in the warmer outflow material (2.5 +/- 0.8).

引用

页数：6

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