Gas-phase and Surface Chemistry in the Massive Star-Forming Region RCW\,120

Abstract

We analysed broadband emission spectra of a dense molecular clump in RCW 120, obtained with the APEX telescope in the 200--260 GHz range, in order to investigate molecular formation pathways in regions of massive star formation at an early evolutionary stage. We examined the correlations between the molecular column densities derived under the LTE assumption. An excess of methanol was found in the southern part of the dense clump relative to its northern part, while the abundances of other molecules, such as CH${}_3$CN and CH${}_3$CCH, remain comparable. The methanol abundance is also elevated relative to that of other oxygen-bearing molecules, such as OCS and SO. To identify possible causes of the enhanced methanol abundance in the southern part of the clump, we carried out simulations with the astrochemical model Presta in a two-phase approximation, accounting for chemical processes both in the gas phase and in the mantles of dust grains. The modelling shows that the enhanced gas-phase methanol abundance may be due to photodesorption from icy mantles. At Av values between $4^m$ and $6^m$, methanol desorbs efficiently from the ice mantles of dust grains upon interaction with photons, but is not yet destroyed by UV radiation in the gas phase. A strong linear correlation between molecular column densities indicates that the molecules form in the same phase --- either in the gas phase or on dust. Their integrated intensity maps may nevertheless differ, as is the case for CCH and CH${}_3$CN. If two molecules form in different phases --- one in the gas phase and the other in dust mantles --- no correlation is observed, as for CCH and CH${}_3$OH. The weak correlation between methanol and the oxygen-bearing molecules that form on dust suggests that only the upper part of the dust mantles, rich in CO ice, is destroyed in the southern part of the clump.

Published: 03 December 2025

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Cited by in corpus (1)

• MOLLId: software for automatic identification of spectral molecular lines in the sub-millimeter and millimeter bands and its application to the spectra of protostars from the region RCW 120