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--- molecules:ism:ch3oh [2022/04/28 14:51] – mueller
+++ molecules:ism:ch3oh [2022/04/29 13:56] (current) – mueller
@@ Line 3: / Line 3: @@
 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\\
-reported on the\\
+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).\\
@@ Line 10: / Line 10: @@
 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]]**\\
 //Astrophys. J.// **227**, 422–432 (1979).\\
@@ Line 20: / Line 20: @@
 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]]**\\
 //Mon. Not. R. Astron. Soc.// **240**, 35P–40P (1989).\\
@@ Line 27: / Line 27: @@
 R. Mauersberger, C. Henkel, T. Jacq, C. M. Walmsley\\
-reported on\\
+detected\\
 **[[https://ui.adsabs.harvard.edu/abs/1988A%26A...194L...1M/abstract|Deuterated Methanol in Orion]]**\\
 //Astron. Astrophys.// **194**, L1−L4 (1988).\\
@@ Line 33: / Line 33: @@
 \\
+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.\\
+\\
 -------
@@ Line 40: / Line 67: @@
 **[[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.
+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.\\
+\\
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