Detection of Interstellar H[TINF]2[/TINF]D[TSUP]+[/TSUP] Emission

Stark, R.; Tak, F. F. S. van der; Dishoeck, E. F. van

doi:10.1086/312182

Cited by 104 publications

(94 citation statements)

References 23 publications

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“…In parallel, a number of recent gas phase models studies indicate that the presence of grains and therefore freeze out of species can favor deuterium enrichment reactions indirectly (Roberts et al 2002;Tiné et al 2000). Observations of high abundances of H 2 D + support the scenario in which deuteration proceed efficiently when other molecules are frozen out onto grains (Stark et al 1999). …”

Section: A Possible Scenario For Deuterium Enrichment?mentioning

confidence: 70%

Revisiting the solid HDO/H$_\mathsf{2}$O abundances

Dartois

Thi

Geballe

et al. 2003

A&A

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Abstract. We revisit the reported detection and upper limits on HDO in ice mantles present in the molecular cloud environments of the massive young protostars Gl 2136 and W33 A, using independent VLT-ISAAC and UKIRT-CGS4 spectroscopic observations. We also present VLT and UKIRT spectra of RAFGL 7009 near the HDO absorption wavelength and reanalyze the ISO-SWS spectral data for NGC 7538 IRS9, Orion-BN and S140. We demonstrate that the previously reported detections of HDO in W33 A and NGC 7538 IRS9 are incorrect. We present an in-depth analysis that shows that, besides the sensitivity limits, detection of low levels of HDO is difficult in amorphous ice mantles when features from solid methanol, a common grain mantle constituent, are present. We discuss the specific problems arising in the ISO data in this wavelength range for NGC 7538 IRS9. Using VLT-ISAAC observations, we also investigate the HDO/H 2 O ratio toward the intermediate mass stars IRAS 05329-0728 and IRAS 08448-4343. Our derived upper limits for the D/H ratio in water ice range from HDO/H 2 O < 1% to 0.2% in the different sources, and we discuss these limits in comparison with values derived in other environments.

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Section: A Possible Scenario For Deuterium Enrichment?mentioning

confidence: 70%

Revisiting the solid HDO/H$_\mathsf{2}$O abundances

Dartois

Thi

Geballe

et al. 2003

A&A

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“…Stark et al 1999Stark et al , 2004Pillai et al 2012), DCN (e.g. Wilson et al 1973;van Dishoeck et al 1995), HDO (Henkel et al 1987;van Dishoeck et al 1995), and DCO + (Penzias 1979;Butner & Loren 1988).…”

Section: Introductionunclassified

Deuterium chemistry of dense gas in the vicinity of low-mass and massive star-forming regions

Awad

Viti

Bayet

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The standard interstellar ratio of deuterium to hydrogen (D/H) atoms is ∼ 1.5×10 −5 . However, the deuterium fractionation is in fact found to be enhanced, to different degrees, in cold, dark cores, hot cores around massive star forming regions, lukewarm cores, and warm cores (hereafter, hot corinos) around low-mass star forming regions. In this paper, we investigate the overall differences in the deuterium chemistry between hot cores and hot corinos. We have modelled the chemistry of dense gas around low-mass and massive star forming regions using a gas-grain chemical model. We investigate the influence of varying the core density, the depletion efficiency of gaseous species on to dust grains, the collapse mode and the final mass of the protostar on the chemical evolution of star forming regions. We find that the deuterium chemistry is, in general, most sensitive to variations of the depletion efficiency on to grain surfaces, in agreement with observations. In addition, the results showed that the chemistry is more sensitive to changes in the final density of the collapsing core in hot cores than in hot corinos. Finally, we find that ratios of deuterated sulphur bearing species in dense gas around hot cores and corinos may be good evolutionary indicators in a similar way as their non deuterated counterparts.

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“…Multiple detections of H 2 D + and doubly deuterated H + 3 , D 2 H + , have followed in both starless and protostellar cores (Caselli et al 2003;Stark et al 2004;Vastel et al 2004), including a recent survey of H 2 D + emission toward 16 objects by Caselli et al (2008). Walmsley et al (2004) show that the H 2 D + abundance determined for the dark core L1544 by Caselli et al (2003) is consistent with a "complete depletion" model, where heavy elements such as C, N, and O (and, consequently, molecules containing these elements) are missing from the gas phase at the highest core densities.…”

Section: Introductionmentioning

confidence: 99%

The Initial Conditions of Clustered Star Formation. Iii. The Deuterium Fractionation of the Ophiuchus B2 Core

Friesen

Francesco

Myers

et al. 2010

ApJ

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We present N 2 D + 3-2 (IRAM), and H 2 D + 1 11 -1 10 and N 2 H + 4-3 (JCMT) maps of the small cluster-forming Ophiuchus B2 core in the nearby Ophiuchus molecular cloud. In conjunction with previously published N 2 H + 1-0 observations, the N 2 D + data reveal the deuterium fractionation in the high-density gas across Oph B2. The average deuterium fractionation R D = N (N 2 D + )/N(N 2 H + ) ∼ 0.03 over Oph B2, with several small scale R D peaks and a maximum R D = 0.1. The mean R D is consistent with previous results in isolated starless and protostellar cores. The column density distributions of both H 2 D + and N 2 D + show no correlation with total H 2 column density. We find, however, an anticorrelation in deuterium fractionation with proximity to the embedded protostars in Oph B2 to distances 0.04 pc. Destruction mechanisms for deuterated molecules require gas temperatures greater than those previously determined through NH 3 observations of Oph B2 to proceed. We present temperatures calculated for the dense core gas through the equating of non-thermal line widths for molecules (i.e., N 2 D + and H 2 D + ) expected to trace the same core regions, but the observed complex line structures in B2 preclude finding a reasonable result in many locations. This method may, however, work well in isolated cores with less complicated velocity structures. Finally, we use R D and the H 2 D + column density across Oph B2 to set a lower limit on the ionization fraction across the core, finding a mean x e,lim few × 10 −8 . Our results show that care must be taken when using deuterated species as a probe of the physical conditions of dense gas in star-forming regions.

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Detection of Interstellar H[TINF]2[/TINF]D[TSUP]+[/TSUP] Emission

Cited by 104 publications

References 23 publications

Revisiting the solid HDO/H$_\mathsf{2}$O abundances

Revisiting the solid HDO/H$_\mathsf{2}$O abundances

Deuterium chemistry of dense gas in the vicinity of low-mass and massive star-forming regions

The Initial Conditions of Clustered Star Formation. Iii. The Deuterium Fractionation of the Ophiuchus B2 Core

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