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dc.contributor.authorOliveira, J. M.
dc.contributor.authorLoon, J. Th. van
dc.contributor.authorChen, C. H. R.
dc.contributor.authorTielens, A. G. G. M.
dc.contributor.authorSloan, G. C.
dc.contributor.authorWoods, P. M.
dc.contributor.authorKemper, F.
dc.contributor.authorIndebetouw, R.
dc.contributor.authorGordon, K. D.
dc.contributor.authorBoyer, M. L.
dc.contributor.authorShiao, B.
dc.contributor.authorMadden, S.
dc.contributor.authorSpeck, Angela K.
dc.contributor.authorMeixner, Margaret
dc.contributor.authorMarengo, M.
dc.date.issued2009-12eng
dc.descriptionhttp://www.iop.org/EJ/article/0004-637X/707/2/1269/apj_707_2_1269.pdf?request-id=762f8343-8c31-4613-a486-277ec46d1b8een
dc.description.abstractWe 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.en
dc.identifier.citationThe Astrophysical Journal, 707:1269-1295, 2009 December 20en
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/10355/5131
dc.publisherAmerican Astronomical Societyen
dc.relation.ispartofPhysics and Astronomy publications (MU)en
dc.relation.ispartofcommunityUniversity of Missouri-Columbia. College of Arts and Sciences. Department of Physics and Astronomy
dc.source.urihttp://www.iop.org/EJ/article/0004-637X/707/2/1269/apj_707_2_1269.pdf?request-id=762f8343-8c31-4613-a486-277ec46d1b8een
dc.subjectastrochemistryen
dc.subjectgalaxiesen
dc.subjectMagellanic cloudsen
dc.subject.lcshCosmochemistryen
dc.subject.lcshCircumstellar matteren
dc.subject.lcshMagellanic Cloudsen
dc.subject.lcshStars -- Formationen
dc.titleIce chemistry in embedded young stellar objects in the Large Magellanic Clouden
dc.typeArticleen


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