2004
DOI: 10.1086/421265
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Detection of D 2 H + in the Dense Interstellar Medium

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Cited by 152 publications
(182 citation statements)
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“…To our knowledge this work has produced the only rather firm detection of the 692 GHz line so far. Vastel et al (2004) estimated the H 2 D + (o) and D 2 H + (p) column densities from the observed line profiles by assuming line-of-sight homogeneity and an excitation temperature of T ex = 10 K. We assumed that these column densities are approximately valid, and adjusted the fractional abundances accordingly. The physical model of the core was adopted from Stark et al (2004), allowing for the fact that the cloud is probably nearer than previously thought (120 pc, Lombardi et al 2008).…”
Section: Hydrostatic Modelsmentioning
confidence: 99%
See 1 more Smart Citation
“…To our knowledge this work has produced the only rather firm detection of the 692 GHz line so far. Vastel et al (2004) estimated the H 2 D + (o) and D 2 H + (p) column densities from the observed line profiles by assuming line-of-sight homogeneity and an excitation temperature of T ex = 10 K. We assumed that these column densities are approximately valid, and adjusted the fractional abundances accordingly. The physical model of the core was adopted from Stark et al (2004), allowing for the fact that the cloud is probably nearer than previously thought (120 pc, Lombardi et al 2008).…”
Section: Hydrostatic Modelsmentioning
confidence: 99%
“…11 Vastel et al (2004), but the lines are too broad, probably because the assumed kinetic temperature is too high. We return to this issue in Sect.…”
Section: Hydrostatic Modelsmentioning
confidence: 99%
“…Methanol deuteration is thus likely to be produced completely by active grain-surface chemistry, controlled by the atomic D content of the accreting gas. The high atomic D/H ratio required to account for the observed fractionation (0.1-0.2, Parise et al 2002) has been explained by invoking an efficient transfer of atomic deuterium from the HD main reservoir via the intermediate H 2 D + /D 2 H + ions (Roberts et al 2003;Parise et al 2006), which are very abundant in the CO-depleted pre-stellar gas (e.g., Caselli et al 2003;Phillips & Vastel 2003;Vastel et al 2004;Parise et al 2011). Presently, all the measured methanol deuterations have been satisfactorily reproduced by the most recent coupled gas-grain models (Taquet et al 2012;Aikawa et al 2012), Article published by EDP Sciences A27, page 1 of 8 thus supporting the hypothesis that D-fractionation in methanol is a distinctive relic of the protostars' past history.…”
Section: Introductionmentioning
confidence: 99%
“…The detection of multiply deuterated isotopologues of H + 3 (e.g. Caselli et al 2003;Vastel et al 2004) motivated Roberts et al (2003Roberts et al ( , 2004 to release a new version of their model in which multiply deuterated isotopologues of H + 3 are taken into account. Their results revealed that the inclusion of D2H + and D + 3 enhances the fractionation of ionic and neutral species because it allows more deuterium to transfer to other species in dark clouds.…”
Section: Introductionmentioning
confidence: 99%