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| H. S. P. Müller, V. V. Ilyushin, A. Belloche, F. Lewen, and S. Schlemmer\\ | H. S. P. Müller, V. V. Ilyushin, A. Belloche, F. Lewen, and S. Schlemmer\\ |
| reported on an\\ | reported on an\\ |
| **[[https://doi.org/10.1051/0004-6361/202451011|Investigation of the Rotational Spectrum of CH<sub>3</sub><sup>17</sup>OH and its Tentative Detection toward Sagittarius B2(N)]]**\\ | **[[https://doi.org/10.1051/0004-6361/202451011|Investigation of the Rotational Spectrum of CH3(17)OH and its Tentative Detection toward Sagittarius B2(N)]]**\\ |
| //Astron. Astrophys.// **688**, Art. No. A201 (2023).\\ | //Astron. Astrophys.// **688**, Art. No. A201 (2024).\\ |
| | The authors report a tentative detection of this isotopolog in the ReExploring Molecular Complexity with ALMA survey at 3 mm. Only one unblended and one partially blended line were identified, many more were severely bleded or too weak. The derived CH<sub>3</sub><sup>18</sup>OH to CH<sub>3</sub><sup>17</sup>OH ratio of ~3.3 is along <sup>18</sup>O to <sup>17</sup>O ratios found for other molecules in the Galactic Center as is the CH<sub>3</sub><sup>16</sup>OH to CH<sub>3</sub><sup>18</sup>OH ratio of 240.\\ |
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| | More recently,\\ |
| | Y. Watanabe, T. Oyama, A. Tamanai, S. Zeng, and N. Sakai\\ |
| | reported on\\ |
| | **[[https://doi.org/10.1051/0004-6361/202556325|Observation of CH3(17)OH and CH3(18)OH in Orion KL: A new Tool to Study Star Formation History]]**\\ |
| | //Astron. Astrophys.// **705**, Art. No. A132 (2026).\\ |
| | The authors analyzed archival ALMA data near 231.89 GHz and 236.5 GHz and derived a CH<sub>3</sub><sup>18</sup>OH to CH<sub>3</sub><sup>17</sup>OH ratio of ~3.4–3.5, which corresponds to the expected <sup>18</sup>O/<sup>17</sup>O ratio at this galactocentric distance, reiteration the potential of methanol as a proble into the <sup>18</sup>O/<sup>17</sup>O ratio, as already done by Müller et al. in the previous paragraph.\\ |
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| //Astron. Astrophys.// **687**, Art. No. A220 (2024).\\ | //Astron. Astrophys.// **687**, Art. No. A220 (2024).\\ |
| Unsurprisingly, the authors detected in their PILS data also many lines of CH<sub>3</sub>OD in //v//<sub>t</sub> = 1. These lines were instrumental in determing the rotational temperature of ~190 K, which is in accord with ~225 K mentioned in the previous paragraph, but considerably lower than the estimated ~300 K earlier. Adopting earlier values, the amount of CH<sub>3</sub>OD is ~0.32 % that of CH<sub>3</sub>OH, and the CH<sub>2</sub>DOH to CH<sub>3</sub>OD ratio is ~22.5, which translates into a deuteration ratio per H atom of ~7.5.\\ | Unsurprisingly, the authors detected in their PILS data also many lines of CH<sub>3</sub>OD in //v//<sub>t</sub> = 1. These lines were instrumental in determing the rotational temperature of ~190 K, which is in accord with ~225 K mentioned in the previous paragraph, but considerably lower than the estimated ~300 K earlier. Adopting earlier values, the amount of CH<sub>3</sub>OD is ~0.32 % that of CH<sub>3</sub>OH, and the CH<sub>2</sub>DOH to CH<sub>3</sub>OD ratio is ~22.5, which translates into a deuteration ratio per H atom of ~7.5.\\ |
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| | H. S. P. Müller, V. V. Ilyushin, A. Belloche, F. Lewen, and S. Schlemmer\\ |
| | reported on an\\ |
| | **[[https://doi.org/10.1051/0004-6361/202451011|Investigation of the Rotational Spectrum of CH<sub>3</sub><sup>17</sup>OH and its Tentative Detection toward Sagittarius B2(N)]]**\\ |
| | //Astron. Astrophys.// **688**, Art. No. A201 (2023).\\ |
| | The authors report a tentative detection of torsionally excited CH<sub>3</sub><sup>18</sup>OH in the ReExploring Molecular Complexity with ALMA survey at 3 mm besides several a clear identification of this isotopolog in its ground torsional state.\\ |
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| Contributor(s): H. S. P. Müller; 04, 2022; 08, 2024 | Contributor(s): H. S. P. Müller; 04, 2022; 08, 2024; 02, 2026 |
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