First Detection of Doubly Deuterated Hydrogen Sulfide

Vastel, C.; Phillips, T. G.; Ceccarelli, C.; Pearson, John C.

doi:10.1086/378261

Cited by 107 publications

(82 citation statements)

References 28 publications

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“…Singly and doubly deuterated hydrogen sulfide have been detected in a few dark clouds Vastel et al 2003) with a significant fractionation level of ∼ 10%. The fractionation is sensitive to the temperature since HDS and D 2 S are not detected in hot cores, despite their large H 2 S column densities.…”

Section: Sulfur and Other Heavy Element Hydridesmentioning

confidence: 99%

Interstellar Hydrides

Gérin

Neufeld

Goicoechea

2016

Annu. Rev. Astron. Astrophys.

129

171

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Interstellar hydrides -that is, molecules containing a single heavy element atom with one or more hydrogen atoms -were among the first molecules detected outside the solar system. They lie at the root of interstellar chemistry, being among the first species to form in initially-atomic gas, along with molecular hydrogen and its associated ions. Because the chemical pathways leading to the formation of interstellar hydrides are relatively simple, the analysis of the observed abundances is relatively straightforward and provides key information about the environments where hydrides are found. Recent years have seen rapid progress in our understanding of interstellar hydrides, thanks largely to far-IR and submillimeter observations performed with the Herschel Space Observatory. In this review, we will discuss observations of interstellar hydrides, along with the advanced modeling approaches that have been used to interpret them, and the unique information that has thereby been obtained.

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Section: Sulfur and Other Heavy Element Hydridesmentioning

confidence: 99%

Interstellar Hydrides

Gérin

Neufeld

Goicoechea

2016

Annu. Rev. Astron. Astrophys.

129

171

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“…Following this discovery, other doubly or triply deuterated molecules have been detected having similarly high D/H enhancements: ammonia (Roueff et al 2000;Loinard et al 2001;van der Tak et al 2002; Based on observations with the IRAM 30 m telescope in Spain and with The James Clerk Maxwell Telescope, operated by The Joint Astronomy Centre on behalf of the Particle Physics and Astronomy Research Council of the United Kingdom, the Netherlands Organisation of Scientific Research, and the National Research Council of Canada. Lis et al 2002), methanol (Parise et al 2002) and hydrogen sulfide (Vastel et al 2003).…”

Section: Introductionmentioning

confidence: 99%

HDO abundance in the envelope of the solar-type protostar IRAS 16293–2422

Parise¹,

Caux²,

Castets

et al. 2005

A&A

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Abstract. We present IRAM 30 m and JCMT observations of HDO lines towards the solar-type protostar IRAS 16293−2422. Five HDO transitions have been detected on-source, and two were unfruitfully searched for towards a bright spot of the outflow of IRAS 16293−2422. We interpret the data by means of the Ceccarelli et al. (1996) model, and derive the HDO abundance in the warm inner and cold outer parts of the envelope. The emission is well explained by a jump model, with an inner abundance x HDO in = 1 × 10 −7 and an outer abundance x HDO out ≤ 1 × 10 −9 (3σ). This result is in favor of HDO enhancement due to ice evaporation from the grains in the inner envelope. The deuteration ratio HDO/H 2 O is found to be f in = 3% and f out ≤ 0.2% (3σ) in the inner and outer envelope respectively and therefore, the fractionation also undergoes a jump in the inner part of the envelope. These results are consistent with the formation of water in the gas phase during the cold prestellar core phase and storage of the molecules on the grains, but do not explain why observations of H 2 O ices consistently derive a H 2 O ice abundance of several 10 −5 to 10 −4 , some two orders of magnitude larger than the gas phase abundance of water in the hot core around IRAS 16293−2422.

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“…This leads to a very efficient transfer of deuterium to other species (see, e.g., Roberts et al 2003, Walmsley et al 2004. This theory is supported by various observational results (Caselli et al 1999, Roueff et al 2000, Vastel et al 2003, Vastel et al 2004, Crapsi et al 2005 protonation followed by dissociative recombination reactions, but for H 2 CO recent theoretical work has shown that this route is inefficient (Osamura et al 2005). Extremely high D 2 CO/H 2 CO ratios have been observed towards both prestellar and protostellar cores and are increasingly taken to be evidence of active grain surface chemistry and desorption (e.g., Ceccarelli et al 2001, Bacmann et al 2003.…”

Section: Introductionmentioning

confidence: 78%

Models and observations of deuterated molecules in protostellar cores

Roberts¹

2008

Proc. IAU

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Abstract. Measuring the deuterium fractionation in different molecules can allow one to determine the physical conditions in the gas and to differentiate between gas-phase and grain surface chemical processing. Observations of molecular D/H ratios in different species towards the dense gas surrounding low-mass protostars are presented and are compared with model simulations. These consider gas-phase chemistry, accretion and desorption, and reactions on grain surfaces during the initial stages of core collapse.

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First Detection of Doubly Deuterated Hydrogen Sulfide

Cited by 107 publications

References 28 publications

Interstellar Hydrides

Interstellar Hydrides

HDO abundance in the envelope of the solar-type protostar IRAS 16293–2422

Models and observations of deuterated molecules in protostellar cores

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