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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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| **[[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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