Survey of Ices toward Massive Young Stellar Objects. I. OCS, CO, OCN−, and CH3OH

Abstract An important tracer of the origin and evolution of cometary ices is the comparison with ices found in dense clouds and toward young stellar objects (YSOs). We present a survey of ices in the 2–5 μ m spectra of 23 massive YSOs, taken with the NASA InfraRed Telescope Facility SpeX spectrometer. The 4.90 μ m absorption band of OCS ice is detected in 20 sight lines, more than 5 times the previously known detections. The absorption profile shows little variation and is consistent with OCS embedded in CH 3 OH-rich ices, and proton-irradiated H 2 S or SO 2 -containing ices. The OCS column densities correlate well with those of CH 3 OH and OCN − , but not with H 2 O and apolar CO ice. This association of OCS with CH 3 OH and OCN − firmly establishes their formation location deep inside dense clouds or protostellar envelopes. The median composition of this ice phase toward massive YSOs, as a percentage of H 2 O, is CO:CH 3 OH:OCN − :OCS = 24:20:1.53:0.15. CS, due to its low abundance, is likely not the main precursor to OCS. Sulfurization of CO is likely needed, although the source of this sulfur is not well constrained. Compared to massive YSOs, low-mass YSOs and dense clouds have similar or somewhat lower CO and CH 3 OH ice abundances, but less OCN − and more apolar CO, while OCS awaits detection. Comets tend to be underabundant in carbon-bearing species, but this does not appear to be the case for OCS, perhaps signalling OCS production in protoplanetary disks.