Water in Star-forming Regions with the Herschel Space Observatory (WISH). I. Overview of Key Program and First Results

被引：200

作者：

van Dishoeck, E. F. ^{[1
,2
]}

Kristensen, L. E. ^{[1
]}

Benz, A. O. ^{[3
]}

Bergin, E. A. ^{[4
]}

Caselli, P. ^{[5
,6
]}

Cernicharo, J. ^{[7
]}

Herpin, F. ^{[8
,9
]}

Hogerheijde, M. R. ^{[1
]}

Johnstone, D. ^{[10
,11
]}

Liseau, R. ^{[12
]}

Nisini, B. ^{[13
]}

Shipman, R. ^{[14
]}

Tafalla, M. ^{[15
]}

van der Tak, F. ^{[14
,16
]}

Wyrowski, F. ^{[17
]}

Aikawa, Y. ^{[18
]}

Bachiller, R. ^{[15
]}

Baudry, A. ^{[8
,9
]}

Benedettini, M. ^{[19
]}

Bjerkeli, P. ^{[12
]}

Blake, G. A. ^{[20
]}

Bontemps, S. ^{[8
,9
]}

Braine, J. ^{[8
,9
]}

Brinch, C. ^{[1
]}

Bruderer, S. ^{[3
]}

Chavarria, L. ^{[8
,9
]}

Codella, C. ^{[6
]}

Daniel, F. ^{[7
]}

de Graauw, Th. ^{[14
]}

Deul, E. ^{[1
]}

di Giorgio, A. M. ^{[19
]}

Dominik, C. ^{[21
,22
]}

Doty, S. D. ^{[23
]}

Dubernet, M. L. ^{[24
,25
]}

Encrenaz, P. ^{[26
,27
]}

Feuchtgruber, H. ^{[2
]}

Fich, M. ^{[28
]}

Frieswijk, W.

Fuente, A. ^{[29
]}

Giannini, T. ^{[13
]}

Goicoechea, J. R. ^{[7
]}

Helmich, F. P. ^{[14
]}

Herczeg, G. J. ^{[2
]}

Jacq, T. ^{[8
,9
]}

Jorgensen, J. K. ^{[30
]}

Karska, A. ^{[2
]}

Kaufman, M. J. ^{[31
]}

Keto, E. ^{[32
]}

Larsson, B. ^{[33
]}

Lefloch, B. ^{[34
]}

机构：

[1] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[2] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[3] ETH, Inst Astron, CH-8093 Zurich, Switzerland

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

[5] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[6] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy

[7] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain

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

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

[10] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada

[11] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada

[12] Chalmers Univ Technol, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden

[13] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[14] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands

[15] Observ Astron Nacl IGN, Madrid 28014, Spain

[16] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands

[17] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[18] Kobe Univ, Dept Earth & Planetary Sci, Kobe, Hyogo 6578501, Japan

[19] Area Ric Tor Vergata, INAF Inst Fis Spazio Interplanetario, I-00133 Rome, Italy

[20] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA

[21] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands

[22] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands

[23] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA

[24] Univ Paris 06, LPMAA UMR CNRS 7092, F-75252 Paris 05, France

[25] Observ Paris, LUTH UMR CNRS 8102, F-92195 Meudon, France

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

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

[28] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada

[29] Observ Astron Nacl, Alcala De Henares 28803, Spain

[30] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark

[31] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA

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

[33] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden

[34] Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, UMR5571, F-38041 Grenoble 9, France

[35] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

[36] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada

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

[38] European So Observ, D-85748 Garching, Germany

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

[40] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada

[41] Inst RadioAstron Milimetr, E-18012 Granada, Spain

[42] UCL, Dept Phys & Astron, London WC1E 6BT, England

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 2011年 / 123卷 / 900期

关键词：

YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; FAR-INFRARED OBSERVATIONS; WAVE-ASTRONOMY-SATELLITE; VELA MOLECULAR CLOUDS; CHESS SPECTRAL SURVEY; GAS-PHASE H2O; HOT CORE; LINE EMISSION; PROTOSTELLAR ENVELOPES;

D O I：

10.1086/658676

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Water In Star-forming regions with Herschel (WISH) is a key program on the Herschel Space Observatory designed to probe the physical and chemical structures of young stellar objects using water and related molecules and to follow the water abundance from collapsing clouds to planet-forming disks. About 80 sources are targeted, covering a wide ranee of luminosities-from low (< 1 L-circle dot) to high (> 10(5) L-circle dot)-and a wide range of evolutionary stages-from cold prestellar cores to warm protostellar envelopes and outflows to disks around young stars. Both the HIFI and PACS instruments are used to observe a variety of lines of H2O, (H2O)-O-18 and chemically related species at the source position and in small maps around the protostars and selected outflow positions. In addition, high-frequency lines of CO, (CO)-C-13, and (CO)-O-18 are obtained with Herschel and are complemented by ground-based observations of dust continuum, HDO, CO and its isotopologs, and other molecules to ensure a self-consistent data set for analysis. An overview of the scientific motivation and observational strategy of the program is given, together with the modeling approach and analysis tools that have been developed. Initial science results are presented. These include a lack of water in cold gas at abundances that are lower than most predictions, strong water emission from shocks in protostellar environments, the importance of UV radiation in heating the gas along outflow walls across the full range of luminosities, and surprisingly widespread detection of the chemically related hydrides OH+ and H2O+ in outflows and foreground gas. Quantitative estimates of the energy budget indicate that H2O is generally not the dominant coolant in the warm dense gas associated with protostars. Very deep limits on the cold gaseous water reservoir in the outer regions of protoplanetary disks are obtained that have profound implications for our understanding of grain growth and mixing in disks.

引用

页码：138 / 170

页数：33

共 14 条

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Mottram, J. C.
Kristensen, L. E.
van Dishoeck, E. F.
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Karska, A.
Visser, R.
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Benz, A. O.
Bergin, E. A.
Caselli, P.
Herpin, F.
Hogerheijde, M. R.
Johnstone, D.
van Kempen, T. A.
Liseau, R.
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Tafalla, M.
van der Tak, F. F. S.
Wyrowski, F.
ASTRONOMY & ASTROPHYSICS, 2014, 572
[2] Water in star-forming regions with Herschel
Kristensen, L. E.
van Dishoeck, E. F.
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Kristensen, L. E.
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Benz, A. O.
Bergin, E. A.
Caselli, P.
Herpin, F.
Hogerheijde, M. R.
Johnstone, D.
Liseau, R.
Nisini, B.
Tafalla, M.
van der Tak, F. F. S.
Wyrowski, F.
Baudry, A.
Benedettini, M.
Bjerkeli, P.
Blake, G. A.
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Bruderer, S.
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