Ortho-to-para ratio of interstellar heavy water

被引：43

作者：

Vastel, C. ^{[1
,2
]}

Ceccarelli, C. ^{[3
,4
,5
]}

Caux, E. ^{[1
,2
]}

Coutens, A. ^{[1
,2
]}

Cernicharo, J. ^{[6
]}

Bottinelli, S. ^{[1
,2
]}

Demyk, K. ^{[1
,2
]}

Faure, A. ^{[3
]}

Wiesenfeld, L. ^{[3
]}

Scribano, Y. ^{[7
]}

Bacmann, A. ^{[3
,4
,5
]}

Hily-Blant, P. ^{[3
]}

Maret, S. ^{[3
]}

Walters, A. ^{[1
,2
]}

Bergin, E. A. ^{[8
]}

Blake, G. A.

Castets, A. ^{[3
,4
,5
]}

Crimier, N. ^{[3
,6
]}

Dominik, C. ^{[10
,11
]}

Encrenaz, P. ^{[12
]}

Gerin, M. ^{[12
]}

Hennebelle, P. ^{[12
]}

Kahane, C. ^{[3
]}

Klotz, A. ^{[1
,2
]}

Melnick, G. ^{[13
]}

Pagani, L. ^{[12
]}

Parise, B. ^{[14
]}

Schilke, P. ^{[14
,15
]}

Wakelam, V. ^{[4
,5
]}

Baudry, A. ^{[4
,5
]}

Bell, T.

Benedettini, M. ^{[16
]}

Boogert, A. ^{[9
]}

Cabrit, S. ^{[12
]}

Caselli, P. ^{[17
]}

Codella, C. ^{[18
]}

Comito, C. ^{[14
]}

Falgarone, E. ^{[12
]}

Fuente, A. ^{[19
]}

Goldsmith, P. F. ^{[20
]}

Helmich, F. ^{[21
]}

Henning, T. ^{[22
]}

Herbst, E.

Jacq, T. ^{[4
]}

Kama, M. ^{[10
]}

Langer, W. ^{[20
]}

Lefloch, B. ^{[3
]}

Lis, D.

Lord, S. ^{[9
]}

Lorenzani, A. ^{[18
]}

机构：

[1] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France

[2] CNRS INSU, UMR 5187, Toulouse, France

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

[4] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France

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

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

[7] CNRS, UMR 5209, Lab Interdisciplinaire Carnot Bourgogne, Dijon, France

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

[9] CALTECH, Infared Proc & Anal Ctr, Pasadena, CA 91109 USA

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

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

[12] UCP, UPMC, ENS,UMR CNRS INSU 8112, Lab Etudes Rayonnement & Matiere Astrophys,OP, Paris, France

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

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

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

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

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

[18] INAF Osservatorio Astrofis Arcetri, Florence, Italy

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

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

[21] SRON Netherlands Inst Space Res, Groningen, Netherlands

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

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

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

[25] Inst Radio Astron Millimetr, Grenoble, France

[26] Leiden Univ, Leiden Observ, Leiden, Netherlands

[27] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands

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

[29] Chalmers, Goterborg, Sweden

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 521卷

关键词：

astrochemistry; ISM: molecules; submillimeter: ISM; ISM: abundances; molecular processes; line: identification; PROTOSTAR IRAS 16293-2422; SPECTROSCOPY; CONSTRAINTS; ENVELOPE;

D O I：

10.1051/0004-6361/201015101

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Despite the low elemental deuterium abundance in the Galaxy, enhanced molecular D/H ratios have been found in the environments of low-mass star-forming regions, and in particular the Class 0 protostar IRAS 16293-2422. Aims. The CHESS (Chemical HErschel Surveys of Star forming regions) key program aims to study the molecular complexity of the interstellar medium. The high sensitivity and spectral resolution of the Herschel/HIFI instrument provide a unique opportunity to observe the fundamental 1(1,1)-0(0,0) transition of the ortho-D2O molecule, which is inaccessible from the ground, and determine the ortho-to-para D2O ratio. Methods. We detected the fundamental transition of the ortho-D2O molecule at 607.35 GHz towards IRAS 16293-2422. The line is seen in absorption with a line opacity of 0.62 +/- 0.11 (1 sigma). From the previous ground-based observations of the fundamental 1(1,0)-1(0,1) transition of para-D2O seen in absorption at 316.80 GHz, we estimate a line opacity of 0.26 +/- 0.05 (1 sigma). Results. We show that the observed absorption is caused by the cold gas in the envelope of the protostar. Using these new observations, we estimate for the first time the ortho-to-para D2O ratio to be lower than 2.6 at a 3 sigma level of uncertainty, which should be compared with the thermal equilibrium value of 2:1.

引用

页数：5

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