Show pageOld revisionsBacklinksBack to top This page is read only. You can view the source, but not change it. Ask your administrator if you think this is wrong. ===== On the Detection of Methyl Formate, HC(O)OCH3, in the ISM ===== Methyl formate, HC(O)OCH<sub>3</sub>, is a typical hot core molecule. It is very abundant in massive star-forming regions. It was detected first in emission in Sgr B2 by\\ R. D. Brown, J. G. Crofts, P. D. Godfrey, F. F. Gardner, B. J. Robinson, and J. B. Whiteoak,\\ **[[https://ui.adsabs.harvard.edu/abs/1975ApJ...197L..29B|Discovery of Interstellar Methyl Formate]]**\\ //Astrophys. J.// **197**, L29–L31 (1975).\\ The //A// component of the 1<sub>10</sub> – 1<sub>11</sub> near 1610 GHz was clearly seen with the Parkes 64 m telescope, and there was evidence for the //E// component close by.\\ 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,\\ **[[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). 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,\\ **[[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). In addition, the identification of torsionally excited HC(O)OCH<sub>3</sub> was reported in\\ K. Kobayashi, K. Ogata, S. Tsunekawa, and S. Takano,\\ **[[https://doi.org/10.1086/512977|Torsionally Excited Methyl Formate in Orion KL]]**\\ //Astrophys. J.// **657**, L17–L19 (2007).\\ 20 U-lines from four different line surveys in the frequency range 97 to 160 GHz were assigned. More recently,\\ S. Takano, Y. Sakai, S. Kakimoto, M. Sasaki, and K. Kobayashi reported on the\\ **[[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).\\ 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\\ 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]]**\\ //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\\ reported on the\\ **[[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).\\ 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\\ reported shortly thereafter on\\ **[[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).\\ 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\\ reported on the\\ **[[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).\\ 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\\ reported on\\ **[[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).\\ 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,\\ reported on\\ **[[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.\\ 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\\ 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,\\ **[[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).\\ 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. ---- Contributor(s): H. S. P. Müller; 02, 2007; 04, 2011; 07, 2012; 08, 2012; 11, 2016; 03, 2019 ---- molecules/ism/methylformiat.txt Last modified: 2019/10/24 09:38by mueller