2017
DOI: 10.1017/s1743921317006858
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Modeling CO, CO2and H2O Ice Abundances in the Envelopes of Young Stellar Objects in the Magellanic Clouds

Abstract: Massive young stellar objects in the Magellanic Clouds show infrared absorption features corresponding to significant abundances of CO, CO 2 and H 2 O ice along the line of sight, with the relative abundances of these ices differing between the Magellanic Clouds and the Milky Way. CO ice is not detected towards sources in the Small Magellanic Cloud, and upper limits put its relative abundance well below sources in the Large Magellanic Cloud and the Milky Way. We use our gas-grain chemical code MAGICKAL, with m… Show more

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“…Hence, the presence of CH 3 OH in the Magellanic Clouds points to formation in a cold pre-hot core phase. 158 studied the formation of ice mantles in the Magellanic Clouds but instead employed a correct stochastic calculation of the grain chemistry. The relative composition of ices comprising of H 2 O, CO, CO 2 , CH 3 OH, NH 3 and CH 4 were calculated as a function of the interstellar UV radiation field.…”
Section: Chemical Models Of the Lmc And Smcmentioning
confidence: 99%
“…Hence, the presence of CH 3 OH in the Magellanic Clouds points to formation in a cold pre-hot core phase. 158 studied the formation of ice mantles in the Magellanic Clouds but instead employed a correct stochastic calculation of the grain chemistry. The relative composition of ices comprising of H 2 O, CO, CO 2 , CH 3 OH, NH 3 and CH 4 were calculated as a function of the interstellar UV radiation field.…”
Section: Chemical Models Of the Lmc And Smcmentioning
confidence: 99%