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molecules:ism:ch3oh [2022/04/28 14:39] – mueller | molecules:ism:ch3oh [2022/04/29 13:56] (current) – mueller |
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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.\\ | 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\\ | J. A. Ball, C. A. Gottlieb, A. E. Lilley, and H. E. Radford\\ |
reported on the\\ | gave an account of the\\ |
**[[https://ui.adsabs.harvard.edu/abs/1970ApJ...162L.203B/abstract|Detection of Methyl Alcohol in Sagittarius]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1970ApJ...162L.203B/abstract|Detection of Methyl Alcohol in Sagittarius]]**\\ |
//Astrophys. J.// **162**, L203–L210 (1970).\\ | //Astrophys. J.// **162**, L203–L210 (1970).\\ |
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C. A. Gottlieb, J. A. Ball, E. W. Gottlieb, and D. F. Dickinson\\ | C. A. Gottlieb, J. A. Ball, E. W. Gottlieb, and D. F. Dickinson\\ |
reported on\\ | investigated\\ |
**[[https://ui.adsabs.harvard.edu/abs/1979ApJ...227..422G/abstract|Interstellar Methyl Alcohol]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1979ApJ...227..422G/abstract|Interstellar Methyl Alcohol]]**\\ |
//Astrophys. J.// **227**, 422–432 (1979).\\ | //Astrophys. J.// **227**, 422–432 (1979).\\ |
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F. F. Gardner, J. B. Whiteoak, J. Reynolds, W. L. Peters, and T. B. H. Kuiper\\ | F. F. Gardner, J. B. Whiteoak, J. Reynolds, W. L. Peters, and T. B. H. Kuiper\\ |
reported on the\\ | announced the\\ |
**[[https://doi.org/10.1093/mnras/240.1.35P|First Detection of the <sup>18</sup>O Isotope of Methanol]]**\\ | **[[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).\\ | //Mon. Not. R. Astron. Soc.// **240**, 35P–40P (1989).\\ |
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| 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.\\ |
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| 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.\\ |
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| 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.\\ |
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| 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.\\ |
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| 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.\\ |
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F. J. Lovas, R. D. Suenram, L. E. Snyder, J. M. Hollis, and R. M. Lees\\ | F. J. Lovas, R. D. Suenram, L. E. Snyder, J. M. Hollis, and R. M. Lees\\ |
**[[https://ui.adsabs.harvard.edu/abs/1982ApJ...253..149L/abstract|Detection of the Torsionally Excited State of Methanol in Orion A]]**\\ | **[[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).\\ | //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. | Three lines partaining to four transitions of torsionally excited methanol were detected with the 11 m Kitt Peak radio telescope at 3 mm.\\ |
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| 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.\\ |
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