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

Fich, M. and Blake, G. and Lis, D. (2010) Herschel-PACS spectroscopy of the intermediate mass protostar NGC 7129 FIRS 2. Astronomy and Astrophysics, 518 . L86. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20101116-095831024

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Abstract

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 μm. This provided good detections of 26 spectral lines seen in emission, including lines of H_(2)O, CO, OH, O I, and C II. Results. Most of the detected lines, particularly those of H_(2)O 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.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201014672DOIArticle
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014672&Itemid=129PublisherArticle
ORCID:
AuthorORCID
Blake, G.0000-0003-0787-1610
Lis, D.0000-0002-0500-4700
Additional Information:© 2010 ESO. Received 31 March 2010; Accepted 15 May 2010; Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. We thank Bruno Merin, Jeroen Bouwman, and Bart VandenBussche of the PACS ICC for all of their help with the data reduction. J.C. and A.F. thank theo Spanish MCINN for funding support under program CONSOLIDER INGENIO 2010 ref: CSD2009-00038, and J.C., under programs AYA2006-14786 and AYA2009-07304. A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This program is made possible thanks to the HIFI guaranteed time program and the PACS instrument builders. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U.Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INT); Sweden: Chalmers University of Technology – MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University – Stockholm Obseratory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC.
Funders:
Funding AgencyGrant Number
Ministerio de Ciencia e Innovación (MCINN)CSD2009-00038
Ministerio de Ciencia e Innovación (MCINN)AYA2006-14786
Ministerio de Ciencia e Innovación (MCINN)AYA2009-07304
Subject Keywords:stars: formation; ISM: molecules
Record Number:CaltechAUTHORS:20101116-095831024
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20101116-095831024
Official Citation: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, P. Bjerkeli, 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, Th. de Graauw, F. Helmich, F. Herpin, M. R. Hogerheijde, T. Jacq, J. K. Jørgensen, B. Larsson, D. Lis, R. Liseau, M. Marseille, G. Melnick, B. Nisini, M. Olberg, B. Parise, C. Risacher, J. Santiago, P. Saraceno, R. Shipman, M. Tafalla, F. van der Tak, R. Visser, F. Wyrowski and U. A. Yıldız A&A 518 L86 (2010) DOI: 10.1051/0004-6361/201014672
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:20827
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:16 Nov 2010 22:53
Last Modified:03 Oct 2019 02:15

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