Limits on HDS/H_2S abundance ratios in hot molecular cores

Details Limits on HDS/H_2S abundance ratios in hot molecular cores Limits on HDS/H_2S abundance ratios in hot molecular cores

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...346..227h&link_type=abstract

Astronomy and Astrophysics, v.346, p.227-232 (1999)

Astronomy and Astrophysics

Astrophysics

19

Molecular Processes, Stars: Formation, Ism: Abundances, Ism: H Ii Regions, Ism: Molecules

Scientific paper

We have searched for HDS emission in a small number of hot cores. Using observations of H_2(34) S, we have derived upper limits to the [HDS]/[H_2S] abundance ratio. The upper limits, which are close to 10(-3) can be interpreted in two ways, depending on whether grain surface reactions contribute to the formation of H_2S. If grains do not dominate, then the H_2S observed is formed in hot, post-shocked gas and a ratio close to the cosmic [D]/[H] ratio is expected for [HDS]/[H_2S]. This scenario is consistent with our upper limits and with the relatively low abundance ratio found for [HDO]/[H_2O] in hot cores but does not seem to account for all of the molecular [D]/[H] ratios observed in hot cores. If grains do dominate the formation of H_2S, then the observed upper limit to the ratio is consistent with the formation of `hot core ices' at a temperature of 60-80 K, { close to the temperature at which cometary ices are thought to form.}

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