Herschel spectral surveys of star- forming regions Overview of the 555-636 GHz range

被引：96

作者：

Ceccarelli, C. ^{[1
,2
,3
]}

Bacmann, A. ^{[1
,2
,3
]}

Boogert, A. ^{[4
]}

Caux, E. ^{[5
,6
]}

Dominik, C. ^{[7
,8
]}

Lefloch, B. ^{[1
]}

Lis, D.

Schilke, P. ^{[9
,10
]}

van der Tak, F. ^{[11
,12
]}

Caselli, P. ^{[13
,14
]}

Cernicharo, J. ^{[15
]}

Codella, C. ^{[16
]}

Comito, C. ^{[9
]}

Fuente, A. ^{[17
]}

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

Bell, T.

Benedettini, M. ^{[13
]}

Bergin, E. A. ^{[18
]}

Blake, G. A.

Bottinelli, S. ^{[5
,6
]}

Cabrit, S. ^{[19
]}

Castets, A. ^{[1
,2
,3
]}

Coutens, A. ^{[5
,6
]}

Crimier, N. ^{[1
,15
]}

Demyk, K. ^{[5
,6
]}

Encrenaz, P. ^{[19
]}

Falgarone, E. ^{[19
]}

Gerin, M. ^{[19
]}

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

Helmich, F. ^{[11
]}

Hennebelle, P. ^{[19
]}

Henning, T. ^{[21
]}

Herbst, E. ^{[22
]}

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

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

Kahane, C. ^{[1
]}

Kama, M. ^{[7
]}

Klotz, A. ^{[5
,6
]}

Langer, W. ^{[20
]}

Lord, S. ^{[4
]}

Lorenzani, A. ^{[16
]}

Maret, S. ^{[1
]}

Melnick, G. ^{[23
]}

Neufeld, D. ^{[24
]}

Nisini, B. ^{[25
]}

Pacheco, S. ^{[1
]}

Pagani, L. ^{[19
]}

Parise, B. ^{[9
]}

Pearson, J. ^{[20
]}

Phillips, T.

机构：

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

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

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

[4] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA

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

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

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

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

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

[10] Univ Cologne, Inst Phys 1, D-5000 Cologne, Germany

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

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

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

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

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

[16] INAF Osservatorio Astrofis Arcetri, Florence, Italy

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

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

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

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

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

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

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

[24] Johns Hopkins Univ, Baltimore, MD USA

[25] INAF Osservatorio Astronom Roma, Monte Porzio Catone, Italy

[26] Inst RadioAstron Millimetr, Grenoble, France

[27] Leiden Univ, Leiden Observ, Leiden, Netherlands

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

[29] Stockholm Univ, Dept Astron, Chalmers Univ Technol, S-10691 Stockholm, Sweden

[30] Nicholas Copernicus Astron Ctr, Torun, Poland

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

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 521卷

关键词：

astrochemistry; stars: formation; NGC; 6334; I; PROTOSTELLAR SHOCK L1157-B1; MASSIVE YOUNG STARS; DEUTERATED FORMALDEHYDE; HOT CORE; SUBMILLIMETER; MILLIMETER; PROTOSTARS; WATER; I(N);

D O I：

10.1051/0004-6361/201015081

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

High resolution line spectra of star-forming regions are mines of information: they provide unique clues to reconstruct the chemical, dynamical, and physical structure of the observed source. We present the first results from the Herschel key project " Chemical HErschel Surveys of Star forming regions", CHESS. We report and discuss observations towards five CHESS targets, one outflow shock spot and four protostars with luminosities bewteen 20 and 2 x 105 L similar to : L1157-B1, IRAS 16293-2422, OMC2-FIR4, AFGL 2591, and NGC 6334I. The observations were obtained with the heterodyne spectrometer HIFI on board Herschel, with a spectral resolution of 1 MHz. They cover the frequency range 555-636 GHz, a range largely unexplored before the launch of the Herschel satellite. A comparison of the five spectra highlights spectacular differences in the five sources, for example in the density of methanol lines, or the presence./absence of lines from S-bearing molecules or deuterated species. We discuss how these differences can be attributed to the different star-forming mass or evolutionary status.

引用

页数：8

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