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molecules:ism:oxiran [2019/10/24 09:32] – mueller | molecules:ism:oxiran [2023/06/09 13:56] (current) – mueller | ||
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**[[https:// | **[[https:// | ||
// | // | ||
- | The Haystack, Nobeyama, and SEST telescopes were used to detect 10 lines from the 1< | + | The Haystack, Nobeyama, and SEST telescopes were used to detect 10 lines from the 1< |
+ | \\ | ||
Subsequently, | Subsequently, | ||
A. Nummelin, J. E. Dickens, P. Bergman, Å. Hjalmarson, W. M. Irvine, M. Ikeda, and M. Ohishi,\\ | A. Nummelin, J. E. Dickens, P. Bergman, Å. Hjalmarson, W. M. Irvine, M. Ikeda, and M. Ohishi,\\ | ||
**[[https:// | **[[https:// | ||
- | //Astron. Astrophys.// | + | //Astron. Astrophys.// |
+ | \\ | ||
The molecule was also detected in three Galactic center molecular clouds which have low dust temperatures (10–20 K), | The molecule was also detected in three Galactic center molecular clouds which have low dust temperatures (10–20 K), | ||
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**[[https:// | **[[https:// | ||
// | // | ||
- | The column density relative to methanol is reasonable. However, since only one transition was observed, these detections should be viewed with caution. | + | The column density relative to methanol is reasonable. However, since only one transition was observed, these detections should be viewed with caution.\\ |
+ | \\ | ||
J. M. Lykke, A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, R. T. Garrod, H. S. P. Müller, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, | J. M. Lykke, A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, R. T. Garrod, H. S. P. Müller, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, | ||
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**[[https:// | **[[https:// | ||
// | // | ||
- | This report is the first one on the detection of ethylene oxide around a low-mass protostar. The Protostellar Interferometric Line Survey (PILS) was carried out with ALMA in its Band 7 (329 – 363 GHz). A total of 20 lines were assigned to oxirane. | + | This report is the first one on the detection of ethylene oxide around a low-mass protostar. The Protostellar Interferometric Line Survey (PILS) was carried out with ALMA in its Band 7 (329 – 363 GHz). A total of 20 lines were assigned to oxirane.\\ |
+ | \\ | ||
+ | A. Bacmann, A. Faure, and J. Berteaud\\ | ||
+ | gave an account of\\ | ||
+ | **[[https:// | ||
+ | //ACS Earth Space Chem.// **3**, 1000 (2019).\\ | ||
+ | They used the IRAM 30 m telescope to detect some lines at 3 and 2 mm toward L1689B.\\ | ||
+ | \\ | ||
+ | |||
+ | H. S. P. Müller, J. K. Jørgensen, J.-C. Guillemin, F. Lewen, and S. Schlemmer\\ | ||
+ | presented the\\ | ||
+ | **[[https:// | ||
+ | //Mon. Not. R. Astron. Soc.// **518**, 185 (2023).\\ | ||
+ | 17 lines, corresponging to 19 transitions with 4 ≤ //J// ≤ 13 with diverse values of // | ||
+ | \\ | ||
+ | |||
+ | H. S. P. Müller, J. K. Jørgensen, J.-C. Guillemin, F. Lewen, and S. Schlemmer\\ | ||
+ | presented more recently the\\ | ||
+ | **[[https:// | ||
+ | //J. Mol. Spectrosc.// | ||
+ | As in the case of the mono-deuterated oxirane above, lines were identifies in the PILS data. | ||
+ | Five or six lines are essentially unblended and have a sufficient signal-to-noise ratio, | ||
+ | two more lines are blended, and the combination of the contributions account nicely for the emission lines. | ||
+ | So the identification was deemed to be somewhat tentative in this line-rich survey. | ||
+ | From the estimate of the column density, one can derive a degree of deuteration per H atom of ~0.16, | ||
+ | compared to ~0.036 per H atom in the case of // | ||
+ | Such an enhancement of the degree of deuteration per H atom has also been seen for other | ||
+ | doubly deuterated molecules compared to their mono-deuerated variants, such as CHD< | ||
+ | CHD< | ||
+ | \\ | ||
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- | Contributor(s): | + | Contributor(s): |
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