Herschel-PACS spectroscopy of the intermediate mass protostar NGC 7129 FIRS 2

被引：19

作者：

Fich, M. ^{[1
]}

Johnstone, D. ^{[2
,3
]}

van Kempen, T. A. ^{[4
,5
]}

McCoey, C. ^{[1
,6
]}

Fuente, A. ^{[7
]}

Caselli, P. ^{[8
,32
]}

Kristensen, L. E. ^{[3
]}

Plume, R. ^{[9
]}

Cernicharo, J. ^{[10
]}

Herczeg, G. J. ^{[11
]}

van Dishoeck, E. F. ^{[4
,11
]}

Wampfler, S. ^{[12
]}

Gaufre, P. ^{[13
]}

Gill, J. J. ^{[14
]}

Javadi, H. ^{[14
]}

Justen, M. ^{[15
]}

Laauwen, W. ^{[16
]}

Luinge, W. ^{[16
]}

Ossenkopf, V. ^{[15
]}

Pearson, J. ^{[14
]}

Bachiller, R. ^{[7
]}

Baudry, A. ^{[13
]}

Benedettini, M. ^{[19
,20
]}

Bergin, E. ^{[20
]}

Benz, A. O. ^{[12
]}

Bjerkeli, P. ^{[17
]}

Blake, G. ^{[21
]}

Bontemps, S. ^{[13
]}

Braine, J. ^{[13
]}

Bruderer, S. ^{[12
]}

Codella, C. ^{[19
]}

Daniel, F. ^{[22
,23
]}

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

Dominik, C. ^{[24
]}

Doty, S. D. ^{[25
]}

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

Giannini, T. ^{[19
]}

Goicoechea, J. R. ^{[10
]}

de Graauw, Th. ^{[16
]}

Helmich, F. ^{[16
]}

Herpin, F. ^{[13
]}

Hogerheijde, M. R. ^{[4
]}

Jacq, T. ^{[13
]}

Jorgensen, J. K. ^{[28
]}

Larsson, B. ^{[29
]}

Lis, D. ^{[21
]}

Liseau, R. ^{[17
]}

Marseille, M. ^{[16
]}

Melnick, G. ^{[4
]}

Nisini, B. ^{[19
]}

机构：

[1] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G, Canada

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

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

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

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

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

[7] IGN Observ Astron Nacl, Alcala De Henares 28800, Spain

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

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

[10] INTA CSIC, Dept Astrophys, CAB, Torrejon De Ardoz 28850, Spain

[11] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany

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

[13] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS INSU, UMR 5804, Floirac, France

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

[15] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany

[16] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands

[17] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden

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

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

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

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

[22] CNRS, Observ Paris Meudon, LERMA, UMR 8112, F-92195 Meudon, France

[23] CSIC, Dept Mol & Infrared Astrophys, Madrid 28006, Spain

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

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

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

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

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

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

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

[31] Univ Cologne, Inst Phys, D-50937 Cologne, Germany

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

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

基金：

美国国家航空航天局;

关键词：

stars: formation; ISM: molecules; YOUNG STELLAR OBJECTS; STAR-FORMATION; HH; 46; EVOLUTION; OUTFLOW; REGIONS; GAS; I;

D O I：

10.1051/0004-6361/201014672

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. We present preliminary results of the first Herschel spectroscopic observations of NGC 7129 FIRS2, an intermediate mass star-forming region. We attempt to interpret the observations in the framework of an in-falling spherical envelope. Methods. The PACS instrument was used in line spectroscopy mode ( R = 1000-5000) with 15 spectral bands between 63 and 185 mu m. This provided good detections of 26 spectral lines seen in emission, including lines of H2O, CO, OH, O I, and C II. Results. Most of the detected lines, particularly those of H2O and CO, are substantially stronger than predicted by the spherical envelope models, typically by several orders of magnitude. In this paper we focus on what can be learned from the detected CO emission lines. Conclusions. It is unlikely that the much stronger than expected line emission arises in the (spherical) envelope of the YSO. The region hot enough to produce such high excitation lines within such an envelope is too small to produce the amount of emission observed. Virtually all of this high excitation emission must arise in structures such as as along the walls of the outflow cavity with the emission produced by a combination of UV photon heating and/or non-dissociative shocks.

引用

页数：5

共 23 条

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