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| molecules:ism:ch3oh [2026/02/09 11:53] – mueller | molecules:ism:ch3oh [2026/04/13 12:16] (current) – mueller |
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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.\\ | 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.// **688**, Art. No. A201 (2023).\\ | //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.\\ | 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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| | === (Far) Infrared Observations of Methanol === |
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| | S. L. Nickerson, N. Rangwala, K. Sung, X. Huang, E. J. Montiel, C. DeWitt, V. J. M. Le Gouellec, S. W. J. Colgan, J. Dittmann, J. P. Fonfría, G. M. Harper, K. E. Kraemer, J. Li, C. A. Nixon, M. F. Rashman, C. Sousa-Silva, A. G. G. M. Tielens, and W. D. Vacca\\ |
| | announced\\ |
| | **[[https://doi.org/10.3847/2041-8213/adf632|The Discovery of 25 μm Interstellar Methanol]]**\\ |
| | //Astrophys. J. Lett. // **989**, Art. No. L51 (2025).\\ |
| | More than 70 transitions were detected with EXES on board of SOFIA toward the massive protostar NGC 7538 IRS 1. Most of the transitions belong to the torsional overtone 2//v//<sub>12</sub>, some also to the torsional fundamental //v//<sub>12</sub>. The derived rotational temperature as well as the column density agree with submillimeter observations.\\ |
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| Contributor(s): H. S. P. Müller; 04, 2022; 08, 2024; 02, 2026 | Contributor(s): H. S. P. Müller; 04, 2022; 08, 2024; 02, 2026; 04, 2026 |
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