First detection of ND in the solar-mass protostar IRAS16293-2422

被引：42

作者：

Bacmann, A. ^{[1
,2
,30
]}

Caux, E. ^{[5
,29
]}

Hily-Blant, P. ^{[1
]}

Parise, B. ^{[10
]}

Pagani, L. ^{[7
,8
]}

Bottinelli, S. ^{[5
,29
]}

Maret, S. ^{[1
]}

Vastel, C. ^{[5
,29
]}

Ceccarelli, C. ^{[1
,2
,30
]}

Cernicharo, J. ^{[9
]}

Henning, T. ^{[26
]}

Castets, A. ^{[1
]}

Coutens, A. ^{[5
,29
]}

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

Blake, G. A.

Crimier, N. ^{[1
,9
]}

Demyk, K. ^{[5
,29
]}

Dominik, C. ^{[12
,13
]}

Gerin, M. ^{[28
]}

Hennebelle, P. ^{[28
]}

Kahane, C. ^{[1
]}

Klotz, A. ^{[5
,29
]}

Melnick, G. ^{[18
]}

Schilke, P. ^{[10
,20
]}

Wakelam, V. ^{[2
,30
]}

Walters, A. ^{[5
,29
]}

Baudry, A. ^{[2
,30
]}

Bell, T.

Benedettini, M. ^{[4
]}

Boogert, A. ^{[3
]}

Cabrit, S. ^{[7
,8
]}

Caselli, P. ^{[6
]}

Codella, C. ^{[11
]}

Comito, C. ^{[10
]}

Encrenaz, P. ^{[7
,8
]}

Falgarone, E. ^{[28
]}

Fuente, A. ^{[14
]}

Goldsmith, P. F. ^{[15
]}

Helmich, F. ^{[16
]}

Herbst, E. ^{[17
]}

Jacq, T. ^{[30
]}

Kama, M. ^{[12
]}

Langer, W. ^{[15
]}

Lefloch, B. ^{[1
]}

Lis, D.

Lord, S. ^{[3
]}

Lorenzani, A. ^{[11
]}

Neufeld, D. ^{[19
]}

Nisini, B. ^{[24
]}

Pacheco, S. ^{[1
]}

机构：

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

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

[3] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91109 USA

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

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

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

[7] Observ Paris, LERMA, F-75014 Paris, France

[8] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France

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

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

[11] INAF Osservatorio Astrofis Arcetri, Florence, Italy

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

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

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

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

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

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

[18] Harvard Smithsonian 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 WC1E 6BT, 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] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands

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

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

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

[31] ETH, Inst Astron, CH-8092 Zurich, Switzerland

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 521卷

关键词：

ISM: molecules; stars: formation; DOUBLY DEUTERATED FORMALDEHYDE; STAR-FORMING REGIONS; DEUTERIUM FRACTIONATION; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; CORES; TRANSITION; METHANOL; AMMONIA; CDMS;

D O I：

10.1051/0004-6361/201015102

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. In the past decade, much progress has been made in characterising the processes leading to the enhanced deuterium fractionation observed in the ISM and in particular in the cold, dense parts of star forming regions such as protostellar envelopes. Very high molecular D/H ratios have been found for saturated molecules and ions. However, little is known about the deuterium fractionation in radicals, even though simple radicals often represent an intermediate stage in the formation of more complex, saturated molecules. The imidogen radical NH is such an intermediate species for the ammonia synthesis in the gas phase. Many of these light molecules however have their fundamental transitions in the submillimetre domain and their detection is hampered by the opacity of the atmosphere at these wavelengths. Herschel/HIFI represents a unique opportunity to study the deuteration and formation mechanisms of species not observable from the ground. Aims. We searched here for the deuterated radical ND in order to determine the deuterium fractionation of imidogen and constrain the deuteration mechanism of this species. Methods. We observed the solar-mass Class 0 protostar IRAS16293-2422 with the heterodyne instrument HIFI in Bands 1a (480-560 GHz), 3b (858-961 GHz), and 4a (949-1061 GHz) as part of the Herschel key programme CHESS (Chemical HErschel Survey of Star forming regions). Results. The deuterated form of the imidogen radical ND was detected and securely identified with 2 hyperfine component groups of its fundamental transition (N = 0-1) at 522.1 and 546.2 GHz, in absorption against the continuum background emitted from the nascent protostar. The 3 groups of hyperfine components of its hydrogenated counterpart NH were also detected in absorption. The absorption arises from the cold envelope, where many deuterated species have been shown to be abundant. The estimated column densities are similar to 2 x 10(14) cm(-2) for NH and similar to 1.3 x 10(14) cm(-2) for ND. We derive a very high deuterium fractionation with an [ND]/[NH] ratio of between 30 and 100%. Conclusions. The deuterium fractionation of imidogen is of the same order of magnitude as that in other molecules, which suggests that an efficient deuterium fractionation mechanism is at play. We discuss two possible formation pathways for ND, by means of either the reaction of N+ with HD, or deuteron/proton exchange with NH.

引用

页数：5

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