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 Methanol, CH<sub>3</sub>OH, in the ISM ===== Methanol was one of the earliest molecules to be detected by means of radio astronomy. A plethora of reports deserve mentioning here. Therefore, this documentation may well be incomplete for quite a while.\\ J. A. Ball, C. A. Gottlieb, A. E. Lilley, and H. E. Radford\\ gave an account of the\\ **[[https://ui.adsabs.harvard.edu/abs/1970ApJ...162L.203B/abstract|Detection of Methyl Alcohol in Sagittarius]]**\\ //Astrophys. J.// **162**, L203–L210 (1970).\\ They used the 140-foot Greenbank radio telescope for the 1<sub>10</sub> – 1<sub>11</sub> transition near 834 MHz to detect methanol in emission from Sagittarius (Sgr) A and B2.\\ \\ C. A. Gottlieb, J. A. Ball, E. W. Gottlieb, and D. F. Dickinson\\ investigated\\ **[[https://ui.adsabs.harvard.edu/abs/1979ApJ...227..422G/abstract|Interstellar Methyl Alcohol]]**\\ //Astrophys. J.// **227**, 422–432 (1979).\\ They used the 11 m Kitt Peak radio telescope to search for the //J// = 2 – 1 transitions of CH<sub>3</sub>OH, <sup>13</sup>CH<sub>3</sub>OH, and CH<sub>3</sub>OD in the 3 mm region toward several galactic sources. CH<sub>3</sub>OH was detected toward 14 sources, at least the majority of these are hot-core sources. The identification of <sup>13</sup>CH<sub>3</sub>OH lines toward Sgr B2 may well be correct (the <sup>12</sup>C to <sup>13</sup>C ratio of somewhat less than 10 is probably affected by opacity of the CH<sub>3</sub>OH lines), but the identification of CH<sub>3</sub>OD toward the same source is definitively incorrect; see for example:\\ A. Belloche, H. S. P. Müller, R. T. Garrod, and K. M. Menten\\ **[[https://doi.org/10.1051/0004-6361/201527268|Exploring Molecular Complexity with ALMA (EMoCA): Deuterated Complex Organic Molecules in Sagittarius B2(N2)]]**\\ //Astron. Astrophys.// **587**, Art. No. A91 (2016).\\ \\ F. F. Gardner, J. B. Whiteoak, J. Reynolds, W. L. Peters, and T. B. H. Kuiper\\ announced the\\ **[[https://doi.org/10.1093/mnras/240.1.35P|First Detection of the <sup>18</sup>O Isotope of Methanol]]**\\ //Mon. Not. R. Astron. Soc.// **240**, 35P–40P (1989).\\ The NASA's 70 m dish at Tidbinbilla was used to detect the //J<sub>K</sub>// = 2<sub>0</sub> − 3<sub>−1</sub> transition of CH<sub>3</sub><sup>18</sup>OH near 11.6 GHz toward Sgr B2. The derived <sup>16</sup>O to <sup>18</sup>O ratio of 210 ± 40 is in line with other results obtained toward the galactic center.\\ \\ R. Mauersberger, C. Henkel, T. Jacq, C. M. Walmsley\\ detected\\ **[[https://ui.adsabs.harvard.edu/abs/1988A%26A...194L...1M/abstract|Deuterated Methanol in Orion]]**\\ //Astron. Astrophys.// **194**, L1−L4 (1988).\\ About one dozen transitions of CH<sub>3</sub>OD were detected with good signal-to-noise ratios toward Orion KL between 110 and 230 GHz using the IRAM 30 m telescope.\\ \\ T. Jacq, C. M. Walmsley, R. Mauersberger, T. Anderson, E. Herbst, F. C. De Lucia\\ gave an account of the\\ **[[https://ui.adsabs.harvard.edu/abs/1993A%26A...271..276J/abstract|Detection of interstellar CH<sub>2</sub>DOH]]**\\ //Astron. Astrophys.// **271**, 276–281 (1993).\\ The IRAM 30 m telescope was employed to detect six lines of CH<sub>2</sub>DOH toward Orion-IRc2 between 90 and 230 GHz. Several CH<sub>3</sub>OD transitions were observed newly around 136 GHz. The abundance of CH<sub>2</sub>DOH was estimated to be slightly higher (by up to 50 %) than that of CH<sub>3</sub>OD.\\ \\ B. Parise, C. Ceccarelli, A. G. G. M. Tielens, E. Herbst, B. Lefloch, E. Caux, A. Castets, I. Mukhopadhyay, L. Pagani, and L. Loinard\\ announced the\\ **[[https://doi.org/10.1051/0004-6361:20021131|Detection of Doubly-deuterated Methanol in the Solar-type Protostar IRAS 16293−2422]]**\\ //Astron. Astrophys.// **393**, L49–L53 (2002).\\ About a dozen lines of CHD<sub>2</sub>OH were detected between 89 and 224 GHz with very modest to good signal-to-noise ratios employing the IRAM 30 m telescope. The CH<sub>2</sub>DOH isotopolog has an abundance about five times higher. The comparisons to CH<sub>3</sub>OH are incorrect because of severe opacity of these lines.\\ \\ In addition,\\ B. Parise, C. Ceccarelli, A. G. G. M. Tielens, A. Castets, E. Caux, B. Lefloch, and S. Maret\\ were\\ **[[https://doi.org/10.1051/0004-6361:20054476|Testing Grain Surface Chemistry: a Survey of Deuterated Formaldehyde and Methanol in Low-mass Class 0 Protostars]]**\\ //Astron. Astrophys.// **453**, 949–958 (2006).\\ CHD<sub>2</sub>OH was also found toward the low-mass protostars IRAS 2, IRAS 4A, and IRAS 4B in the NGC 1333 molecular cloud.\\ \\ B. Parise, A. Castets, E. Herbst, E. Caux, C. Ceccarelli, I. Mukhopadhyay, and A. G. G. M. Tielens\\ gave an account of the\\ **[[https://doi.org/10.1051/0004-6361:20034490|First Detection of Triply-deuterated Methanol]]**\\ //Astron. Astrophys.// **416**, 159–163 (2004).\\ A dozen lines of CD<sub>3</sub>OH were detected around 158 GHz toward IRAS 16293−2422 with very modest to reasonable signal-to-noise ratios employing the IRAM 30 m telescope. The column density of CH<sub>3</sub>OH was derived from that of <sup>13</sup>CH<sub>3</sub>OH. The CH<sub>3</sub>OH : CH<sub>2</sub>DOH : CHD<sub>2</sub>OH : CD<sub>3</sub>OH ratios were about 126 : 38 : 7.7 : 1.\\ \\ ------- F. J. Lovas, R. D. Suenram, L. E. Snyder, J. M. Hollis, and R. M. Lees\\ reported on the\\ **[[https://ui.adsabs.harvard.edu/abs/1982ApJ...253..149L/abstract|Detection of the Torsionally Excited State of Methanol in Orion A]]**\\ //Astrophys. J.// **253**, 149–153 (1982).\\ Three lines partaining to four transitions of torsionally excited methanol were detected with the 11 m Kitt Peak radio telescope at 3 mm.\\ \\ V. V. Ilyushin, H. S. P. Müller, J. K. Jørgensen, S. Bauerecker, C. Maul, Y. Bakhmat, E. A. Alekseev, O. Dorovskaya, S. Vlasenko, F. Lewen, S. Schlemmer, K. Berezkin, and R. M. Lees\\ investigated the\\ **[[https://doi.org/10.1051/0004-6361/202142326|Rotational and Rovibrational Spectroscopy of CD<sub>3</sub>OH with an Account of CD<sub>3</sub>OH toward IRAS 16293−2422]]**\\ //Astron. Astrophys.// **658**, Art. No. A127 (2022).\\ Using the Protostellar Interferometric Line Survey carried out with ALMA, several lines of torsionally excited CD<sub>3</sub>OH were detected between 329 and 363 GHz; nine unblended or only slightly blended lines of this vibrationally excited state were shown in a figure around 350.6 GHz. The rotational temperature was ~225 K, and the CH<sub>3</sub>OH to CD<sub>3</sub>OH ratio was about 300. Lines of torsionally excited deuterated methanol will be more prominent for <sup>12</sup>C isotopologs containing fewer D atoms.\\ \\ ---- Contributor(s): H. S. P. Müller; 04, 2022 ---- molecules/ism/ch3oh.txt Last modified: 2022/04/29 13:56by mueller