Detection of the elusive dangling OH ice features at ~2.7 μm in Chamaeleon I with JWST NIRCam

Noble, J. A.; Fraser, H. J.; Smith, Z. L.; Dartois, E.; Boogert, A. C. A.; Cuppen, H. M.; Dickinson, H. J.; Dulieu, F.; Egami, E.; Erkal, J.; Giuliano, B. M.; Husquinet, B.; Lamberts, T.; Maté, B.; McClure, M. K.; Palumbo, M. E.; Shimonishi, T.; Sun, F.; Bergner, J. B.; Brown, W. A.; Caselli, P.; Congiu, E.; Drozdovskaya, M. N.; Herrero, V. J.; Ioppolo, S.; Jimenez-Serra, I.; Linnartz, H.; Melnick, G. J.; McGuire, B. A.; Oberg, K. I.; Perotti, G.; Qasim, D.; Rocha, W. R. M. and Urso, R. G. (2024). Detection of the elusive dangling OH ice features at ~2.7 μm in Chamaeleon I with JWST NIRCam. Nature Astronomy (Early Access).

DOI: https://doi.org/10.1038/s41550-024-02307-7

Abstract

Ascertaining the morphology and composition of the icy mantles covering dust grains in dense, cold regions of the interstellar medium is essential to developing accurate astrochemical models, determining conditions for ice formation, constraining chemical interactions in and on icy grains and understanding how ices withstand space radiation. The widely observed infrared spectroscopic signature of H₂O ice at ~3 μm discriminates crystalline from amorphous structures in interstellar ices. Weaker bands seen only in laboratory ice spectra at ~2.7 μm, termed ‘dangling OH’ (dOH), are attributed to water molecules not fully bound to neighbouring water molecules and are often considered as tracing the degree of ice compaction. We exploit the high sensitivity of JWST NIRCam to detect two dOH features at 2.703 and 2.753 μm along multiple lines of sight probing the dense cloud Chamaeleon I, attributing these signatures to unbound dOH in cold water ice and dOH in interaction with other molecular species. These detections open a path to using the dOH features as tracers of the formation, composition, morphology and evolution of icy grains during the star and planet formation process.

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