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CO Line Profiles in Accreting Ices
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DOI：10.3847/1538-4357/ae6111.png)
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Abstract
En 中文
We investigate how the infrared absorption profile of the solid-state CO stretching mode reflects the chemical and structural environments produced during ice growth under astrophysically relevant conditions. Using two complementary deposition protocols, classical isothermal codeposition at 12 K and a temperature-decreasing ramp that simulates accretion during grain cooling, we produce a set of mixed and layered CO ices containing H2O, NH3, CH4, CO2, and CH3OH. The resulting laboratory CO spectra are decomposed into a library of Gaussian components, each associated with a specific chemical and structural microenvironment. Within this framework, variations in the CO line profile can be related to differences in ice structure and local chemical composition. We apply this laboratory-based approach to JWST observations of two molecular cloud sight lines and one protoplanetary disc. The molecular cloud spectra are consistent with CO residing predominantly in layered, chemically evolved environments, whereas the disc spectrum requires additional components associated with mixed or reprocessed ices. A small, consistent set of components from our experimental library is sufficient to reproduce all the observed CO features. This suggests that only a few specific CO microenvironments dominate these astrophysical ices, providing a useful reference point for future multicomponent laboratory and observational studies of astrophysical ice mantles.
Keywords:
CARBON-MONOXIDE
INFRARED-SPECTROSCOPY
BAND PROFILES
SOLID CO
INTERSTELLAR
EVOLUTION
CORES
Journal
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5.4
Papers:
8.3W
Citations:
32.0W
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