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High-Resolution 4.7 Micron Keck/NIRSPEC Spectra of Protostars. II. Detection of the ^(13)CO Isotope in Icy Grain Mantles

Boogert, A. C. A. and Blake, G. A. and Tielens, A. G. G. M. (2002) High-Resolution 4.7 Micron Keck/NIRSPEC Spectra of Protostars. II. Detection of the ^(13)CO Isotope in Icy Grain Mantles. Astrophysical Journal, 577 (1). pp. 271-280. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20120918-115406398

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Abstract

The high-resolution (R = 25,000) infrared M-band spectrum of the massive protostar NGC 7538 IRS 9 shows a narrow absorption feature at 4.779 μm (2092.3 cm^(-1)) that we attribute to the vibrational stretching mode of the ^(13)CO isotope in pure CO icy grain mantles. This is the first detection of ^(13)CO in icy grain mantles in the interstellar medium. The ^(13)CO band is a factor of 2.3 narrower than the apolar component of the ^(12)CO band. With this in mind, we discuss the mechanisms that broaden solid-state absorption bands. It is shown that ellipsoidally shaped pure CO grains fit the bands of both isotopes at the same time. Slightly worse but still reasonable fits are also obtained by CO embedded in N_2-rich ices and thermally processed O_2-rich ices. In addition, we report new insights into the nature and evolution of interstellar CO ices by comparing the very high resolution multicomponent solid ^(12)CO spectrum of NGC 7538 IRS 9 with that of the previously studied low-mass source L1489 IRS. The narrow absorption of apolar CO ices is present in both spectra but much stronger in NGC 7538 IRS 9. It is superposed on a smooth broad absorption feature well fitted by a combination of CO_2 and H_2O-rich laboratory CO ices. The abundances of the latter two ices, scaled to the total H_2O ice column, are the same in both sources. We thus suggest that thermal processing manifests itself as evaporation of apolar ices only and not the formation of CO_2 or polar ices. Finally, the decomposition of the ^(12)CO band is used to derive the ^(12)CO/^(13)CO abundance ratio in apolar ices. A ratio of ^(12)CO/^(13)CO = 71 ± 15 (3 σ) is deduced, in good agreement with gas-phase CO studies (~77) and the solid ^(12)CO_2/^(13)CO_2 ratio of 80 ± 11 found in the same line of sight. The implications for the chemical path along which CO_2 is formed are discussed.


Item Type:Article
Related URLs:
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http://dx.doi.org/10.1086/342176DOIUNSPECIFIED
http://iopscience.iop.org/0004-637X/577/1/271PublisherUNSPECIFIED
Additional Information:© 2002 American Astronomical Society. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. Received 2002 April 6; accepted 2002 May 29. The research of A. C. A. B. and G. A. B. is supported by the SIRTF Legacy Science program and by the Owens Valley Radio Observatory through NSF grant AST 99-81546. We thank the anonymous referee for several useful comments. The authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, none of the observations presented herein would have been possible.
Funders:
Funding AgencyGrant Number
NSFAST-99-81546
Subject Keywords:astrochemistry; infrared: ISM; ISM: abundances; ISM: molecules; stars: formation; stars: individual (NGC 7538 IRS 9)
Record Number:CaltechAUTHORS:20120918-115406398
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20120918-115406398
Official Citation: High-Resolution 4.7 Micron Keck/NIRSPEC Spectra of Protostars. II. Detection of the 13CO Isotope in Icy Grain Mantles A. C. A. Boogert et al. 2002 ApJ 577 271
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:34183
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:18 Sep 2012 20:37
Last Modified:26 Dec 2012 16:12

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