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--- molecules:ism:ch3oh [2022/04/29 13:15] – mueller
+++ molecules:ism:ch3oh [2022/04/29 13:56] (current) – mueller
@@ Line 44: / Line 44: @@
 **[[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 between 89 and 224 GHz were detected 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.\\
+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.\\
+\\
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@@ Line 55: / 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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