Ice chemistry in embedded young stellar objects in the Large Magellanic Cloud

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Ice chemistry in embedded young stellar objects in the Large Magellanic Cloud

Please use this identifier to cite or link to this item: http://hdl.handle.net/10355/5131

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Title: Ice chemistry in embedded young stellar objects in the Large Magellanic Cloud
Author: Oliveira, J. M.; Loon, J. Th. van; Chen, C. H. R.; Tielens, A. G. G. M.; Sloan, G. C.; Woods, P. M.; Kemper, F.; Indebetouw, R.; Gordon, K. D.; Boyer, M. L.; Shiao, B.; Madden, S.; Speck, Angela K.; Meixner, Margaret; Marengo, M.
Keywords: astrochemistry
galaxies
Magellanic clouds
Date: 2009-12-03
Publisher: American Astronomical Society
Citation: The Astrophysical Journal, 707:1269-1295, 2009 December 20
Abstract: We present spectroscopic observations of a sample of 15 embedded young stellar objects (YSOs) in the Large Magellanic Cloud (LMC). These observations were obtained with the Spitzer Infrared Spectrograph (IRS) as part of the SAGE-Spec Legacy program.We analyze the two prominent ice bands in the IRS spectral range: the bending mode of CO2 ice at 15.2 μm and the ice band between 5 and 7 μm that includes contributions from the bending mode of water ice at 6 μm among other ice species. The 5-7 μm band is difficult to identify in our LMC sample due to the conspicuous presence of polycyclic aromatic hydrocarbon emission superimposed onto the ice spectra. We identify water ice in the spectra of two sources; the spectrum of one of those sources also exhibits the 6.8 μm ice feature attributed in the literature to ammonium and methanol. We model the CO2 band in detail, using the combination of laboratory ice profiles available in the literature. We find that a significant fraction ( 50%) of CO2 ice is locked in a water-rich component, consistent with what is observed for Galactic sources. The majority of the sources in the LMC also require a pure-CO2 contribution to the ice profile, evidence of thermal processing. There is a suggestion that CO2 production might be enhanced in the LMC, but the size of the available sample precludes firmer conclusions. We place our results in the context of the star formation environment in the LMC.
URI: http://hdl.handle.net/10355/5131
ISSN: 1538-4357

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