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molecules:ism:methylformiat [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:methylformiat [2019/10/24 09:38] (current) – mueller | ||
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Methyl formate, HC(O)OCH< | Methyl formate, HC(O)OCH< | ||
R. D. Brown, J. G. Crofts, P. D. Godfrey, F. F. Gardner, B. J. Robinson, and J. B. Whiteoak,\\ | R. D. Brown, J. G. Crofts, P. D. Godfrey, F. F. Gardner, B. J. Robinson, and J. B. Whiteoak,\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
// | // | ||
The //A// component of the 1< | The //A// component of the 1< | ||
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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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More recently,\\ | More recently,\\ | ||
S. Takano, Y. Sakai, S. Kakimoto, M. Sasaki, and K. Kobayashi reported on the\\ | S. Takano, Y. Sakai, S. Kakimoto, M. Sasaki, and K. Kobayashi reported on the\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
//Publ. Astron. Soc. Japan// **64**, Art. No. 89 (2012).\\ | //Publ. Astron. Soc. Japan// **64**, Art. No. 89 (2012).\\ | ||
Four new lines were observed newly with the Nobeyama 45 m radio telescope near 90 GHz together with several transitions of the ground and the first excited torsional state. 15 additional lines were detected in two published line surveys. The derived vibrational temperature of about 125 K was higher than the rotational temperature of around 50 K, possibly indicating infrared pumping. Since the torsional modes are rather weak, it may be more likely that infrared pumping took place via some small amplitude vibration and subsequent intermolecular energy redistribution. However, as the authors indicated, collisional excitation cannot be ruled out a being responsible for the vibrational temperature being apparently higher than the rotational one. | Four new lines were observed newly with the Nobeyama 45 m radio telescope near 90 GHz together with several transitions of the ground and the first excited torsional state. 15 additional lines were detected in two published line surveys. The derived vibrational temperature of about 125 K was higher than the rotational temperature of around 50 K, possibly indicating infrared pumping. Since the torsional modes are rather weak, it may be more likely that infrared pumping took place via some small amplitude vibration and subsequent intermolecular energy redistribution. However, as the authors indicated, collisional excitation cannot be ruled out a being responsible for the vibrational temperature being apparently higher than the rotational one. | ||
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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 < | ||
Line 55: | Line 55: | ||
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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