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Herschel/HIFI spectroscopy of the intermediate mass protostar NGC7129 FIRS 2

Johnstone, D. and Blake, G. A. and Lis, D. (2010) Herschel/HIFI spectroscopy of the intermediate mass protostar NGC7129 FIRS 2. Astronomy and Astrophysics, 521 . Art. No. L41. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20110111-152223622

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Abstract

Herschel/HIFI observations of water from the intermediate mass protostar NGC 7129 FIRS 2 provide a powerful diagnostic of the physical conditions in this star formation environment. Six spectral settings, covering four H_2^(16)O and two H_2^(18)O lines, were observed and all but one H_2^(18)O line were detected. The four H_2 ^(16)O lines discussed here share a similar morphology: a narrower, ≈6km s^(−1), component centered slightly redward of the systemic velocity of NGC7129 FIRS 2 and a much broader, ≈25 km s^(−1) component centered blueward and likely associated with powerful outflows. The narrower components are consistent with emission from water arising in the envelope around the intermediate mass protostar, and the abundance of H_2O is constrained to ≈10^(−7) for the outer envelope. Additionally, the presence of a narrow self-absorption component for the lowest energy lines is likely due to self-absorption from colder water in the outer envelope. The broader component, where the H_2O/CO relative abundance is found to be ≈0.2, appears to be tracing the same energetic region that produces strong CO emission at high J.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201015122DOIArticle
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201015122&Itemid=129PublisherArticle
ORCID:
AuthorORCID
Blake, G. A.0000-0003-0787-1610
Lis, D.0000-0002-0500-4700
Additional Information:© 2010 ESO. Received 1 June 2010, Accepted 23 July 2010, Published online 01 October 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Appendix (page 6) is only available in electronic form at http://www.aanda.org. We thank the HIFI ICC for all of their help with the data reduction, and both the referee and journal editor for critical comments and speed of response. J.C. and A.F. give thanks to 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. 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 Observatory; 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
NASAUNSPECIFIED
Subject Keywords:astrochemistry – stars: formation
Record Number:CaltechAUTHORS:20110111-152223622
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20110111-152223622
Official Citation:Herschel/HIFI spectroscopy of the intermediate mass protostar NGC 7129 FIRS 2 D. Johnstone, M. Fich, C. McCoey, T. A. van Kempen, A. Fuente, L. E. Kristensen, J. Cernicharo, P. Caselli, R. Visser, R. Plume, G. J. Herczeg, E. F. van Dishoeck, S. Wampfler, 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, D. Neufeld, B. Nisini, M. Olberg, B. Parise, J. Pearson, C. Risacher, J. Santiago-García, P. Saraceno, R. Shipman, M. Tafalla, F. van der Tak, F. Wyrowski, U. A. Yıldız, E. Caux, N. Honingh, W. Jellema, R. Schieder, D. Teyssier and N. Whyborn A&A 521 L41 (2010) DOI: 10.1051/0004-6361/201015122
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21716
Collection:CaltechAUTHORS
Deposited By: Benjamin Perez
Deposited On:11 Jan 2011 23:48
Last Modified:31 Aug 2017 03:04

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