The detection of hot ethanol in G34.3+0.15

Millar, T. J.; Macdonald, G. H.; Habing, R. J.

doi:10.1093/mnras/273.1.25

Cited by 42 publications

(27 citation statements)

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“…This is in contrast to dark clouds (20 K), where gas-phase C 2 H 5 OH is not observed. [7][8][9] It is thought that the origin of these high gas-phase abundances arises from the evaporation of chemically rich icy mantles, caused by the heat generated by new born stars.…”

Section: Discussionmentioning

confidence: 99%

Thermally induced mixing of water dominated interstellar ices

Burke

Wolff

Edridge

et al. 2008

Phys. Chem. Chem. Phys.

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Section: Discussionmentioning

confidence: 99%

Thermally induced mixing of water dominated interstellar ices

Burke

Wolff

Edridge

et al. 2008

Phys. Chem. Chem. Phys.

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“…Nomura & Millar (2004) examined the chemical structure of this region and gave an overview of the observed species and their abundances along with some comparisons to their model predictions. Single molecule investigations like ethanol have been performed by Millar et al (1995). Nummelin et al (1998b) examined CH 3 CHO and c-C 2 H 4 O but also gave abundances for methanol, ethanol and dimethyl ether (DME).…”

Section: Source Selectionmentioning

confidence: 99%

“…2. The column density of H 2 towards G34.26 has been estimated by Millar et al (1995) Sandell (2000). McCutcheon et al (2000) took several spectra in the range between 334 and 348 GHz using the JCMT.…”

Section: Source Selectionmentioning

confidence: 99%

Trans-ethyl methyl ether in space

Fuchs

Fuchs²,

Giesen³

et al. 2005

A&A

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An extensive search for the complex molecule trans-ethyl methyl ether towards several hot core regions has been performed. Using the IRAM 30 m telescope and the SEST 15 m we looked at several frequencies where trans-ethyl methyl ether has strong transitions, as well as lines which are particularly sensitive to the physical conditions in which the molecule can be found. We included G34.26, NGC 6334(I), Orion KL, and W51e2 which have previously been proven to have a rich chemistry of complex molecules. Our observations cannot confirm the tentative Orion KL detection made by Charnley et al. (2001) within their stated column density limits, but we confirm the existence of the trans-ethyl methyl ether towards W51e2 with a column density of 2 × 10 14 cm −2 . The dimethyl ether/methanol ratio of 0.6 as well as the newly found ethyl methyl ether/ethanol ratio of 0.13 indicate relative high abundances of ethers toward W51e2. Furthermore, the observation of ethyl methyl ether also confirms the importance of ethanol as a grain mantle constituent. We present new upper limits of around 8 × 10 13 cm −2 for the column densities of the molecule toward Orion KL, G34.26, NGC 6334(I) and estimate the column density towards SgrB2(N) to be of the same order. The W51e2 observations are discussed in more detail.

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“…[1][2][3][4][5][6] In addition, both ethanol and OH have been detected in interstellar molecular clouds and star forming regions (hot and cold cores) such as W3(OH) and Sgr B2, where temperatures can reach as low as 40 K. [7][8][9][10][11][12][13] Millar et al 12 suggested that ethanol could potentially be used as a chemical clock for hot cores if the kinetics of its reactions with species including the hydroxyl radical were better understood at temperatures pertinent to such environments. Conducting kinetic studies with species known to be present in these cold environments is important for the advancement of chemical models of these regions.…”

Section: Introductionmentioning

confidence: 99%

Measurements of Rate Coefficients for Reactions of OH with Ethanol and Propan-2-ol at Very Low Temperatures

et al. 2014

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The low temperature kinetics of the reactions of OH with ethanol and propan-2-ol have been studied using a pulsed Laval nozzle apparatus coupled with pulsed laser photolysis -laser induced fluorescence (PLP-LIF) spectroscopy. The rate coefficients for both reactions have been found to increase significantly as the temperature is lowered, by~a factor of 18 between 293 and 54 K for ethanol, and by~10 between 298 and 88 K for OH + propan-2-ol. The pressure dependence of the rate coefficients provide evidence for two reaction channels; a zero pressure bimolecular abstraction channel leading to products and collisional stabilization of a weakly bound OH-alcohol complex. The presence of the abstraction channel at low temperatures is rationalized by a quantum mechanical tunneling mechanism, most likely through the barrier to hydrogen abstraction from the OH moiety on the alcohol.

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The detection of hot ethanol in G34.3+0.15

Cited by 42 publications

References 0 publications

Thermally induced mixing of water dominated interstellar ices

Thermally induced mixing of water dominated interstellar ices

Trans-ethyl methyl ether in space

Measurements of Rate Coefficients for Reactions of OH with Ethanol and Propan-2-ol at Very Low Temperatures

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