molecules:ism:methylformiat

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molecules:ism:methylformiat [2019/10/24 09:38] – muellermolecules:ism:methylformiat [2025/07/07 13:53] (current) – mueller
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 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,\\
 **[[https://doi.org/10.1086/378038|The Hot Core around the Low-mass Protostar IRAS 16293-2422: Scoundrels Rule!]]**\\ **[[https://doi.org/10.1086/378038|The Hot Core around the Low-mass Protostar IRAS 16293-2422: Scoundrels Rule!]]**\\
-//Astrophys. J.// **593**, L51–L55 (2003).+//Astrophys. J.// **593**, L51–L55 (2003).\\ 
  
 The molecule was also detected in several Galactic center molecular clouds which have low dust temperatures (10–20 K), even lower rotational temperatures (around 10 K), which are moderately dense (a few tenthousand molecules per cubic centimeter), but which are kinetically moderately warm (about 100 K or more). Several transitions were detected with the IRAM 30 m telescope in the 3 mm range by\\ The molecule was also detected in several Galactic center molecular clouds which have low dust temperatures (10–20 K), even lower rotational temperatures (around 10 K), which are moderately dense (a few tenthousand molecules per cubic centimeter), but which are kinetically moderately warm (about 100 K or more). Several transitions were detected with the IRAM 30 m telescope in the 3 mm range by\\
 M. A. Requena-Torres, J. Martín-Pintado, A. Rodríguez-Franco, S. Martín, N. J. Rodríguez-Fernández, and P. de Vicente,\\ M. A. Requena-Torres, J. Martín-Pintado, A. Rodríguez-Franco, S. Martín, N. J. Rodríguez-Fernández, and P. de Vicente,\\
 **[[https://doi.org/10.1051/0004-6361:20065190|Organic Molecules in the Galactic Center – Hot Core Chemistry without Hot Cores]]**\\ **[[https://doi.org/10.1051/0004-6361:20065190|Organic Molecules in the Galactic Center – Hot Core Chemistry without Hot Cores]]**\\
-//Astron. Astrophys.// **455**, 971–985 (2006).+//Astron. Astrophys.// **455**, 971–985 (2006).\\ 
 +\\ 
  
 In addition, the identification of torsionally excited HC(O)OCH<sub>3</sub> was reported in\\ In addition, the identification of torsionally excited HC(O)OCH<sub>3</sub> was reported in\\
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 **[[https://doi.org/10.1086/512977|Torsionally Excited Methyl Formate in Orion KL]]**\\ **[[https://doi.org/10.1086/512977|Torsionally Excited Methyl Formate in Orion KL]]**\\
 //Astrophys. J.// **657**, L17–L19 (2007).\\ //Astrophys. J.// **657**, L17–L19 (2007).\\
-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.\\ 
  
 More recently,\\ More recently,\\
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 **[[https://ui.adsabs.harvard.edu/abs/2012PASJ...64...89T|Detection of Methyl Formate in the Second Torsionally Excited State (//v<sub>t</sub>// = 2) in Orion KL]]**\\ **[[https://ui.adsabs.harvard.edu/abs/2012PASJ...64...89T|Detection of Methyl Formate in the Second Torsionally Excited State (//v<sub>t</sub>// = 2) in Orion KL]]**\\
 //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.\\ 
 +\\ 
  
 The detection of both <sup>13</sup>C isotopomers of methyl formate was reported by\\ The detection of both <sup>13</sup>C isotopomers of methyl formate was reported by\\
 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,\\
 **[[https://doi.org/10.1051/0004-6361/200811456|Rotational Spectrum of <sup>13</sup>C<sub>2</sub>-Methyl Formate (HCOO<sup>13</sup>CH<sub>3</sub>) and Detection of the Two <sup>13</sup>C-Methyl Formate in Orion]]**\\ **[[https://doi.org/10.1051/0004-6361/200811456|Rotational Spectrum of <sup>13</sup>C<sub>2</sub>-Methyl Formate (HCOO<sup>13</sup>CH<sub>3</sub>) and Detection of the Two <sup>13</sup>C-Methyl Formate in Orion]]**\\
-//Astron. Astrophys.// **500**, 1109–1118 (2009).+//Astron. Astrophys.// **500**, 1109–1118 (2009).\\ 
  
 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\\
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 **[[https://doi.org/10.1088/0004-637X/714/2/1120|Rotational Spectrum and Tentative Detection of DCOOCH<sub>3</sub>-Methyl Formate in Orion]]**\\ **[[https://doi.org/10.1088/0004-637X/714/2/1120|Rotational Spectrum and Tentative Detection of DCOOCH<sub>3</sub>-Methyl Formate in Orion]]**\\
 //Astrophys. J.// **714**, 1120–1132 (2010).\\ //Astrophys. J.// **714**, 1120–1132 (2010).\\
-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.\\ 
  
 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\\
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 **[[https://doi.org/10.1051/0004-6361/200913830|TIMASSS: the IRAS16293-2422 Millimeter and Submillimeter Spectral Survey: Tentative Detection of Deuterated Methyl Formate (DCOOCH<sub>3</sub>)]]**\\ **[[https://doi.org/10.1051/0004-6361/200913830|TIMASSS: the IRAS16293-2422 Millimeter and Submillimeter Spectral Survey: Tentative Detection of Deuterated Methyl Formate (DCOOCH<sub>3</sub>)]]**\\
 //Astron. Astrophys.// **517**, Art. No. A17 (2010).\\ //Astron. Astrophys.// **517**, Art. No. A17 (2010).\\
-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.\\ 
  
 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\\
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 **[[https://doi.org/10.1051/0004-6361/201117072|Microwave and Submillimeter Spectroscopy and First ISM Detection of <sup>18</sup>O-Methyl Formate]]**\\ **[[https://doi.org/10.1051/0004-6361/201117072|Microwave and Submillimeter Spectroscopy and First ISM Detection of <sup>18</sup>O-Methyl Formate]]**\\
 //Astron. Astrophys.// **538**, Art. No. A119 (2012).\\ //Astron. Astrophys.// **538**, Art. No. A119 (2012).\\
-Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used again to search for the <sup>18</sup>O isotopomers. The <sup>13</sup>C to <sup>18</sup>O of about 13 is rather reasonable. The <sup>12</sup>C to <sup>13</sup>C and <sup>16</sup>O to <sup>18</sup>O appear to be too small by a factor of about two, likely because of neglect of opacity.+Their Orion KL molecular line survey carried out with the IRAM 30 m telescope was used again to search for the <sup>18</sup>O isotopomers. The <sup>13</sup>C to <sup>18</sup>O of about 13 is rather reasonable. The <sup>12</sup>C to <sup>13</sup>C and <sup>16</sup>O to <sup>18</sup>O appear to be too small by a factor of about two, likely because of neglect of opacity.\\ 
  
 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\\
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 **[[https://doi.org/10.1088/0004-637X/779/2/119|The First Astrophysical Detection, Terahertz Spectrum, and Database for the Monodeuterated Species of Methyl Formate HCOOCH<sub>2</sub>D]]**\\ **[[https://doi.org/10.1088/0004-637X/779/2/119|The First Astrophysical Detection, Terahertz Spectrum, and Database for the Monodeuterated Species of Methyl Formate HCOOCH<sub>2</sub>D]]**\\
 //Astrophys. J.// **779**, Art. No. 119 (2013).\\ //Astrophys. J.// **779**, Art. No. 119 (2013).\\
-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, L. E. Kristensen, M. H. D. van der Wiel, and T. L. Bourke,\\ S. Manigand, H. Calcutt, J. K. Jørgensen, V. Taquet, H. S. P. Müller, A. Coutens, S. F. Wampfler, N. Ligterink, M. N. Drozdovskaya, L. E. Kristensen, M. H. D. van der Wiel, and T. L. Bourke,\\
Line 63: Line 74:
 **[[https://doi.org/10.1051/0004-6361/201832844|The ALMA-PILS Survey: The First Detection of Doubly-deuterated Methyl Formate (CHD<sub>2</sub>OCHO) in the ISM]]**\\ **[[https://doi.org/10.1051/0004-6361/201832844|The ALMA-PILS Survey: The First Detection of Doubly-deuterated Methyl Formate (CHD<sub>2</sub>OCHO) in the ISM]]**\\
 //Astron. Astrophys.// **623** (2019) Art. No. A69.\\ //Astron. Astrophys.// **623** (2019) Art. No. A69.\\
-The isotopolog was detected toward source B as well as toward source A. The deuteration per H atom is about 12 and 8 %, respectively, considerably higher than about 6 and 28 %, respectively, for the singly deuterated isotopomers.+The isotopolog was detected toward source B as well as toward source A. The deuteration per H atom is about 12 and 8 %, respectively, considerably higher than about 6 and 28 %, respectively, for the singly deuterated isotopomers.\\ 
 +\\ 
  
 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, it has been characterized in the laboratory recently and was detected tentatively in the cooler, probably more diffuse parts of Sagittarius B2(N) where the chemistry deviates significantly from LTE. The work has been described by\\ 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, it has been characterized in the laboratory recently and was detected tentatively in the cooler, probably more diffuse parts of Sagittarius B2(N) where the chemistry deviates significantly from LTE. The work has been described by\\
Line 69: Line 82:
 **[[https://doi.org/10.1088/0004-637X/755/2/153|Laboratory and Tentative Interstellar Detection of Trans-Methyl Formate Using the Publicly Available Green Bank Telescope Primos Survey]]**\\ **[[https://doi.org/10.1088/0004-637X/755/2/153|Laboratory and Tentative Interstellar Detection of Trans-Methyl Formate Using the Publicly Available Green Bank Telescope Primos Survey]]**\\
 //Astrophys. J.// **755**, Art. No. 153 (2012).\\ //Astrophys. J.// **755**, Art. No. 153 (2012).\\
-The line survey covers the 1 to 50 GHz region. The three //K// = 0 transitions with //J"// = 0 to 2 were detected for both //A// and //E// internal rotation components. In addition, one //K// = 1 was detected for the //A// component. Two additional //K// = 1 transitions each were barely recognizable in the noise, the intensities being compatible with the model. The detection is probably not far from a definitive one.+The line survey covers the 1 to 50 GHz region. The three //K// = 0 transitions with //J"// = 0 to 2 were detected for both //A// and //E// internal rotation components. In addition, one //K// = 1 was detected for the //A// component. Two additional //K// = 1 transitions each were barely recognizable in the noise, the intensities being compatible with the model. The detection is probably not far from a definitive one.\\ 
 + 
 + 
 +M. Sanz-Novo, G. Molpeceres, V. M. Rivilla, and I. Jimenez-Serra\\ 
 +reinvestigated the\\ 
 +**[[https://doi.org/10.1051/0004-6361/202554686|Conformational Isomerism of Methyl Formate: New Detections of the Higher-energy //trans// Conformer and Theoretical Insights]]**\\ 
 +//Astron. Astrophys.// **698**, Art. No. A36 (2025).\\ 
 +The conformer was identified in G+0.693−0.027, close to the Galactic center, and in L1157−B1. Both are cold and shocked sources, the latter one is considered to be a prototypical shock region. The //syn// to //anti// ("//cis//" to "//trans//") ratios are about 72 and 34, respectively, about factors of 7 and 3 higher than in the Sagittarius B2(N) envelope mentioned above.\\ 
 +\\
  
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-Contributor(s): H. S. P. Müller; 02, 2007; 04, 2011; 07, 2012; 08, 2012; 11, 2016; 03, 2019+Contributor(s): H. S. P. Müller; 02, 2007; 04, 2011; 07, 2012; 08, 2012; 11, 2016; 03, 2019; 07, 2025
  
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