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This study aims to elucidate a possible link between chemical properties ofices in star-forming regions and environmental characteristics of the hostgalaxy. We performed 3--4 micron spectroscopic observations toward nineembedded high-mass YSOs in the Large Magellanic Cloud (LMC) with the ISAAC atthe VLT. Additionally, we analyzed archival ISAAC data of two LMC YSOs. As aresult, we detected absorption bands due to solid H2O and CH3OH as well as the3.47 micron absorption band. The 3.53 micron CH3OH ice absorption band for theLMC YSOs is found to be absent or very weak compared to that seen towardGalactic sources. The result suggests the low abundance of CH3OH ice in theLMC. The 3.47 micron absorption band is detected toward six out of eleven LMCYSOs. We found that the 3.47 micron band and the H2O ice band correlatesimilarly between the LMC and Galactic samples, but the LMC sources seem torequire a slightly higher H2O ice threshold for the appearance of the 3.47micron band. For the LMC sources with relatively large H2O ice optical depths,we found that the strength ratio of the 3.47 micron band relative to the waterice band is only marginally lower than those of the Galactic sources. Wepropose that grain surface reactions at a relatively high dust temperature(warm ice chemistry) are responsible for the observed characteristics of icechemical compositions in the LMC. We suggest that this warm ice chemistry isone of the important characteristics of interstellar and circumstellarchemistry in low metallicity environments. The low abundance of CH3OH in thesolid phase implies that formation of complex organic molecules frommethanol-derived species is less efficient in the LMC. For the 3.47 micronband, the observed difference in the water ice threshold may suggest that amore shielded environment is necessary for the formation of the 3.47 micronband carrier in the LMC.

VLT/ISAAC infrared spectroscopy of embedded high-mass YSOs in the Large Magellanic Cloud: Methanol and the 3.47 micron band