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molecules:ism:methylformiat [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:methylformiat [2019/03/14 15:55] – mueller | ||
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More recently, it has also been detected toward low-mass star-forming regions:\\ | More recently, it has also been detected toward low-mass star-forming regions:\\ | ||
S. Cazaux, A. G. G. M. Tielens, C. Ceccarelli, A. Castets, V. Wakelam, E. Caux, B. Parise, D. Teyssier,\\ | S. Cazaux, A. G. G. M. Tielens, C. Ceccarelli, A. Castets, V. Wakelam, E. Caux, B. Parise, D. Teyssier,\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
The molecule was also detected in several Galactic center molecular clouds which have low dust temperatures (10–20 K), | The molecule was also detected in several Galactic center molecular clouds which have low dust temperatures (10–20 K), | ||
M. A. Requena-Torres, | M. A. Requena-Torres, | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
In addition, the identification of torsionally excited HC(O)OCH< | In addition, the identification of torsionally excited HC(O)OCH< | ||
K. Kobayashi, K. Ogata, S. Tsunekawa, and S. Takano,\\ | K. Kobayashi, K. Ogata, S. Tsunekawa, and S. Takano,\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
20 U-lines from four different line surveys in the frequency range 97 to 160 GHz were assigned. | 20 U-lines from four different line surveys in the frequency range 97 to 160 GHz were assigned. | ||
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The detection of both < | The detection of both < | ||
M. Carvajal, L. Margulès, B. Tercero, K. Demyk, I. Kleiner, J. C. Guillemin, V. Lattanzi, A. Walters, J. Demaison, G. Wlodarczak, T. R. Huet, H. Møllendal, V. V. Ilyushin, and J. Cernicharo, | M. Carvajal, L. Margulès, B. Tercero, K. Demyk, I. Kleiner, J. C. Guillemin, V. Lattanzi, A. Walters, J. Demaison, G. Wlodarczak, T. R. Huet, H. Møllendal, V. V. Ilyushin, and J. Cernicharo, | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
L. Margulès, T. R. Huet, J. Demaison, M. Carvajal, I. Kleiner, H. Møllendal, B. Tercero, N. Marcelino, and J. Cernicharo\\ | L. Margulès, T. R. Huet, J. Demaison, M. Carvajal, I. Kleiner, H. Møllendal, B. Tercero, N. Marcelino, and J. Cernicharo\\ | ||
reported on the\\ | reported on the\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used to search for the acid-deuterated isotopolog. The tentative D to H ratio of 0.02 to 0.06 in the compact ridge part of the source is not unusual. | Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used to search for the acid-deuterated isotopolog. The tentative D to H ratio of 0.02 to 0.06 in the compact ridge part of the source is not unusual. | ||
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K. Demyk, S. Bottinelli, E. Caux, C. Vastel, C. Ceccarelli, C. Kahane, and A. Castets\\ | K. Demyk, S. Bottinelli, E. Caux, C. Vastel, C. Ceccarelli, C. Kahane, and A. Castets\\ | ||
reported shortly thereafter on\\ | reported shortly thereafter on\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
The degree of deuteration is similar in both sub-sources A and B, about 0.06. | The degree of deuteration is similar in both sub-sources A and B, about 0.06. | ||
Line 49: | Line 49: | ||
B. Tercero, L. Margulès, M. Carvajal, R. A. Motiyenko, T. R. Huet, E. A. Alekseev, I. Kleiner, J. C. Guillemin, H. Møllendal, and J. Cernicharo\\ | B. Tercero, L. Margulès, M. Carvajal, R. A. Motiyenko, T. R. Huet, E. A. Alekseev, I. Kleiner, J. C. Guillemin, H. Møllendal, and J. Cernicharo\\ | ||
reported on the\\ | reported on the\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used again to search for the < | Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used again to search for the < | ||
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L. H. Coudert, B. J. Drouin, B. Tercero, J. Cernicharo, J.-C. Guillemin, R. A. Motiyenko, and L. Margulès\\ | L. H. Coudert, B. J. Drouin, B. Tercero, J. Cernicharo, J.-C. Guillemin, R. A. Motiyenko, and L. Margulès\\ | ||
reported on\\ | reported on\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used once more to search for the methyl-deuterated isotopolog. The D to H ratio of 0.02 to 0.06 in the compact ridge part of the source is not unusual, but is three times lower per H atom than the tentatively derived value for the acid-deuterated isotopolog. | Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used once more to search for the methyl-deuterated isotopolog. The D to H ratio of 0.02 to 0.06 in the compact ridge part of the source is not unusual, but is three times lower per H atom than the tentatively derived value for the acid-deuterated isotopolog. | ||
+ | |||
+ | S. Manigand, H. Calcutt, J. K. Jørgensen, V. Taquet, H. S. P. Müller, A. Coutens, S. F. Wampfler, N. Ligterink, M. N. Drozdovskaya, | ||
+ | reported on\\ | ||
+ | **[[https:// | ||
+ | //Astron. Astrophys.// | ||
+ | The isotopolog was detected toward source B as well as toward source A. The deuteration per H atom is about 12 and 8 %, respectively, | ||
The so-called //trans// conformer, with the carbonyl oxygen pointing away from the methyl group, is very much higher (about 25 kJ/mol or about 3000 K) in energy than the so-called //cis// conformer. Nevertheless, | The so-called //trans// conformer, with the carbonyl oxygen pointing away from the methyl group, is very much higher (about 25 kJ/mol or about 3000 K) in energy than the so-called //cis// conformer. Nevertheless, | ||
J. L. Neill, M. T. Muckle, D. P. Zaleski, A. L. Steber, B. H. Pate, V. Lattanzi, S. Spezzano, M. C. McCarthy, and A. J. Remijan,\\ | J. L. Neill, M. T. Muckle, D. P. Zaleski, A. L. Steber, B. H. Pate, V. Lattanzi, S. Spezzano, M. C. McCarthy, and A. J. Remijan,\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
The line survey covers the 1 to 50 GHz region. The three //K// = 0 transitions with // | The line survey covers the 1 to 50 GHz region. The three //K// = 0 transitions with // | ||
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