Modeling CO, CO${}_2$ and H${}_2$O 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 multiple grain sizes and grain temperatures, and further expand it with a treatment for increased interstellar radiation field intensity to model the elevated dust temperatures observed in the MCs. We also adjust the elemental abundances used in the chemical models, guided by observations of HII regions in these metal-poor satellite galaxies. With a grid of models, we are able to reproduce the relative ice fractions observed in MC massive young stellar objects (MYSOs), indicating that metal depletion and elevated grain temperature are important drivers of the MYSO envelope ice composition. Magellanic Cloud elemental abundances have a sub-galactic C/O ratio, increasing H${}_2$O ice abundances relative to the other ices; elevated grain temperatures favor CO${}_2$ production over H${}_2$O and CO. The observed shortfall in CO in the Small Magellanic Cloud can be explained by a combination of reduced carbon abundance and increased grain temperatures. The models indicate that a large variation in radiation field strength is required to match the range of observed LMC abundances. CH${}_3$OH abundance is found to be enhanced in low-metallicity models, providing seed material for complex organic molecule formation in the Magellanic Clouds.

Accepted in ApJ 20 pages, 8 figures, 6 tables

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• ALMA Observations of Molecular Complexity in the Large Magellanic Cloud: The N105 Star-Forming Region
• Complex Organic Molecules in Star-Forming Regions of the Magellanic Clouds
• Cracking the Puzzle of CO2 Formation on Interstellar Ices. Quantum Chemical and Kinetic Study of the CO + OH -> CO2 + H Reaction
• A multiline study of a high-mass young stellar object in the Small Magellanic Cloud with ALMA: The detection of methanol gas at 0.2 solar metallicity
• CHEMOUT: CHEMical complexity in star-forming regions of the OUTer Galaxy. II. Methanol formation at low metallicity
• Chemical Kinetics Simulations of Ice Chemistry on Porous Versus Non-Porous Dust Grains
• Near-infrared spectroscopy of embedded protostars in the massive metal-poor star-forming region NGC 346
• A multigrain-multilayer astrochemical model with variable desorption energy for surface species
• MAGellanic Outflow and chemistry Survey (MAGOS): Hot cores in the LMC
• Molecular Formation in Low-Metallicity Hot Cores