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Herschel/HIFI observations of [C II] and [^(13)C II] in photon-dominated regions

Ossenkopf, V. and Röllig, M. and Neufeld, D. A. and Pilleri, P. and Lis, D. C. and Fuente, A. and van der Tak, F. F. S. and Bergin, E. (2013) Herschel/HIFI observations of [C II] and [^(13)C II] in photon-dominated regions. Astronomy and Astrophysics, 550 . Art. No. A57. ISSN 0004-6361. doi:10.1051/0004-6361/201219837. https://resolver.caltech.edu/CaltechAUTHORS:20130329-095151815

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Abstract

Context. Chemical fractionation reactions in the interstellar medium can result in molecular isotopologue abundance ratios that differ by many orders of magnitude from the isotopic abundance ratios. Understanding variations in the molecular abundance ratios through astronomical observations provides a new tool to sensitively probe the underlying physical conditions. Aims. Recently, we have introduced detailed isotopic chemistry into the KOSMA-τ model for photon-dominated regions (PDRs), which allows calculating abundances of carbon isotopologues as a function of PDR parameters. Radiative transfer computations then allow to predict the observed [C II]/[^(13)C II] line intensity ratio for specific geometries. Here, we compare these model predictions with new Herschel observations. Methods. We performed Herschel/HIFI observations of the [C II] 158 μm line in a number of PDRs. In all sources, we observed at least two hyperfine components of the [^(13)C II] transition, allowing determination of the [C II]/[^(13)C II] intensity ratio, using revised intrinsic hyperfine ratios. Comparing the observed line ratios with the predictions from the updated KOSMA-τ model, we identify conditions under which the chemical fractionation effects are important, and not masked by the high optical depth of the main isotopic line. Results. An observable enhancement of the [C II]/[^(13)C II] intensity ratio due to chemical fractionation depends mostly on the source geometry and velocity structure, and to a lesser extent on the gas density and radiation field strength. The enhancement is expected to be largest for PDR layers that are somewhat shielded from UV radiation, but not completely hidden behind a surface layer of optically thick [C II]. In our observations the [C II]/[^(13)C II] integrated line intensity ratio is always dominated by the optical depth of the main isotopic line. However, an enhanced intensity ratio is found for particular velocity components in several sources: in the red-shifted material in the ultracompact H II region Mon R2, in the wings of the turbulent line profile in the Orion Bar, and possibly in the blue wing in NGC 7023. Mapping of the [^(13)C II] lines in the Orion Bar gives a C^+ column density map, which confirms the temperature stratification of the C^+ layer, in agreement with the PDR models of this region. Conclusions. Carbon fractionation can be significant even in relatively warm PDRs, but a resulting enhanced [C II]/[^(13)C II] intensity ratio is only observable for special configurations. In most cases, a reduced [C II]/[^(13)C II] intensity ratio can be used instead to derive the [C II] optical depth, leading to reliable column density estimates that can be compared with PDR model predictions. The C^+ column densities show that, for all sources, at the position of the [C II] peak emission, the dominant fraction of the gas-phase carbon is in the form of C^+.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201219837 DOIArticle
http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201219837&Itemid=129PublisherArticle
ORCID:
AuthorORCID
Ossenkopf, V.0000-0002-8351-3877
Neufeld, D. A.0000-0001-8341-1646
Lis, D. C.0000-0002-0500-4700
Bergin, E.0000-0003-4179-6394
Additional Information:© 2013 ESO. Article published by EDP Sciences. Received 18 June 2012; Accepted 14 November 2012. Published online 24 January 2013. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work was supported by the Deutsche Forschungsgemeinschaft, DFG project number Os 177/1–1 and SFB 956 C1. Additional support for this paper was provided by NASA through an award issued by JPL/Caltech and by Spanish program CONSOLIDER INGENIO 2010, under grant CSD2009-00038 Molecular Astrophysics: The Herschel and ALMA Era (ASTROMOL). We thank Paul Goldsmith and an anonymous referee for many helpful comments. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the US under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands 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, Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronómico Nacional (IGN), Centro de Astrobiología (CSIC-INTA); Sweden: Chalmers University of Technology – MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University – Stockholm Observatory; Switzerland: ETH Zürich, FHNW; USA: Caltech, JPL, NHSC.
Funders:
Funding AgencyGrant Number
Deutsche Forschungsgemeinschaft (DFG)Os 177/1-1
Deutsche Forschungsgemeinschaft (DFG)SFB 956 C1
NASA/JPL/CaltechUNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)CONSOLIDER INGENIO 2010
Ministerio de Ciencia e Innovación (MCINN)CSD2009-00038
Subject Keywords:ISM: abundances; ISM: clouds; ISM: structure
DOI:10.1051/0004-6361/201219837
Record Number:CaltechAUTHORS:20130329-095151815
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130329-095151815
Official Citation:Herschel/HIFI observations of [C II] and [13C II] in photon-dominated regions V. Ossenkopf, M. Röllig, D. A. Neufeld, P. Pilleri, D. C. Lis, A. Fuente, F. F. S. van der Tak and E. Bergin A&A 550 A57 (2013)
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:37686
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:15 May 2013 19:43
Last Modified:09 Nov 2021 23:30

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