Observations of the H2S toward OMC-1

Minh, Y. C.; Ziurys, L. M.; Irvine, William M.; McGonagle, D.

doi:10.1086/169103

Cited by 67 publications

(37 citation statements)

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“…At low temperatures this has the effect that most 13 C nuclei become incorporated into 13 CO, leading to a relative depletion of 13 C in other interstellar molecules. This can have the secondary consequence that molecules formed on grains should have 12 C/ 13 C ratios similar to that of the accreted CO molecules in their carbonyl or carboxyl functional Blake et al (1987), Turner (1990), Minh et al (1990), Mangum et al (1991), Bergin et al (2010), Esplugues et al (2013), Neill et al (2013). Entry for DNC is from the sample of Fontani et al (2014) groups, whereas other functional groups formed by addition of C atoms should be relatively depleted in 13 C (Charnley et al 2004).…”

Section: Interstellar Isotopic Fractionationmentioning

confidence: 99%

Cometary Isotopic Measurements

et al. 2015

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Section: Interstellar Isotopic Fractionationmentioning

confidence: 99%

Cometary Isotopic Measurements

et al. 2015

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“…This overabundance could reflect a large abundance of S in the gas, although the CS abundance seems normal. It could also mean that the absorbing gas at z = 0.89 is not that quiescent and that H 2 S molecules could be released from dust grains either by intense UV radiation from star forming regions or by shocks generated by young stellar objects, as is observed in the Orion (KL) outflow (Minh et al 1990). The very wide absorption profile observed in a few pc-large SW absorbing cloud may support this last scenario.…”

Section: Molecular Column Densitiesmentioning

confidence: 99%

Probing isotopic ratios atz= 0.89: molecular line absorption in front of the quasar PKS 1830-211

Müller

Guèlin

Dumke

et al. 2006

A&A

137

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With the Plateau de Bure interferometer, we have measured the C, N, O and S isotopic abundance ratios in the arm of a spiral galaxy with a redshift of 0.89. The galaxy is seen face-on according to HST images. Its bulge intercepts the line of sight to the radio-loud quasar PKS 1830−211, giving rise at mm wavelengths to two Einstein images located each behind a spiral arm. The arms appear in absorption in the lines of several molecules, giving the opportunity to study the chemical composition of a galaxy only a few Gyr old. The isotopic ratios in this spiral galaxy differ markedly from those observed in the Milky Way. The 17 O/ 18 O and 14 N/ 15 N ratios are low, as one would expect from an object too young to let low mass stars play a major role in the regeneration of the gas.

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“…b Source average from Hatchell et al (1998b) . e Orion Plateau: Sutton et al (1995); Minh et al (1990). c Orion Bar: Jansen et al (1995) .…”

Section: Physical Structurementioning

confidence: 99%

Sulphur chemistry in the envelopes of massive young stars

Tak

Boonman²,

Braakman³

et al. 2003

A&A

139

150

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Abstract. The sulphur chemistry in nine regions in the earliest stages of high-mass star formation is studied through singledish submillimeter spectroscopy. The line profiles indicate that 10-50% of the SO and SO 2 emission arises in high-velocity gas, either infalling or outflowing. For the low-velocity gas, excitation temperatures are 25 K for H 2 S, 50 K for SO, H 2 CS, NS and HCS + , and 100 K for OCS and SO 2 , indicating that most observed emission traces the outer parts (T < 100 K) of the molecular envelopes, except high-excitation OCS and SO 2 lines. Abundances in the outer envelopes, calculated with a Monte Carlo program, using the physical structures of the sources derived from previous submillimeter continuum and CS line data, are ∼10 −8 for OCS, ∼10 −9 for H 2 S, H 2 CS, SO and SO 2 , and ∼10 −10 for HCS + and NS. In the inner envelopes (T > 100 K) of six sources, the SO 2 abundance is enhanced by a factor of ∼100-1000. This region of hot, abundant SO 2 has been seen before in infrared absorption, and must be small, < ∼ 0. 2 (180 AU radius). The derived abundance profiles are consistent with models of envelope chemistry which invoke ice evaporation at T ∼ 100 K. Shock chemistry is unlikely to contribute. A major sulphur carrier in the ices is probably OCS, not H 2 S as most models assume. The source-to-source abundance variations of most molecules by factors of ∼10 do not correlate with previous systematic tracers of envelope heating. Without observations of H 2 S and SO lines probing warm ( > ∼ 100 K) gas, sulphur-bearing molecules cannot be used as evolutionary tracers during star formation.

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Observations of the H2S toward OMC-1

Cited by 67 publications

References 0 publications

Cometary Isotopic Measurements

Cometary Isotopic Measurements

Probing isotopic ratios atz= 0.89: molecular line absorption in front of the quasar PKS 1830-211

Sulphur chemistry in the envelopes of massive young stars

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