High Methanol to Water Ratio Found in Planet-Forming Zone

High-resolution mid-IR spectroscopy of the Class I protostar SVS13-A, using EXES on board SOFIA, has revealed a surprisingly high methanol to water ratio in its planet-forming zone. The detection of several H2O and CH3OH absorption lines indicates the presence of warm gas with rotational temperatures of approximately 140-170 K. Remarkably, the methanol column density is about four times higher than that of water, exceeding typical interstellar ice ratios. This unusual ratio may be attributed to selective sublimation due to the distribution of binding energies or ice stratification within the inner envelope. These observations provide a direct link between ice sublimation and gas-phase chemistry in the innermost regions of the protostar, where planets are expected to form and inherit the chemical composition of their natal environment. The findings highlight the diagnostic power of high-resolution mid-infrared spectroscopy in uncovering hidden chemical layers and the ice-to-gas transition in embedded protostars. Further research is needed to fully understand the processes that lead to the observed methanol to water ratio and its implications for the chemical composition of forming planets.

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