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

M. Fich ; D. Johnstone ; T. A. van Kempen ; C. McCoey ; A. Fuente ; P. Caselli ; L. E. Kristensen ; R. Plume ; J. Cernicharo ; G. J. Herczeg ; E. F. van Dishoeck ; S. Wampfler ; P. Gaufre ; J. J. Gill ; H. Javadi ; M. Justen ; W. Laauwen ; W. Luinge ; V. Ossenkopf ; J. Pearson ; R. Bachiller ; A. Baudry ; M. Benedettini ; E. Bergin ; A. O. Benz ; Per Bjerkeli (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; G. Blake ; S. Bontemps ; J. Braine ; S. Bruderer ; C. Codella ; F. Daniel ; A. M. di Giorgio ; C. Dominik ; S. D. Doty ; P. Encrenaz ; T. Giannini ; J. R. Goicoechea ; T. de Graauw ; F. Helmich ; F. Herpin ; M. R. Hogerheijde ; T. Jacq ; J. K. Jorgensen ; B. Larsson ; D. Lis ; René Liseau (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; M. Marseille ; G. Melnick ; B. Nisini ; Michael Olberg (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium) ; B. Parise ; C. Risacher ; J. Santiago ; P. Saraceno ; R. Shipman ; M. Tafalla ; F. van der Tak ; R. Visser ; F. Wyrowski ; U. A. Yildiz
Astronomy and Astrophysics (0004-6361). Vol. 518 (2010), Article Number: L86 ,
[Artikel, refereegranskad vetenskaplig]

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.

Nyckelord: stars: formation, ISM: molecules, young stellar objects, star-formation, evolution, outflow, regions, i.

Denna post skapades 2010-12-02. Senast ändrad 2015-06-23.
CPL Pubid: 129989


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Institutioner (Chalmers)

Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik (2010-2017)
Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium (2010-2017)


Astronomi, astrofysik och kosmologi

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