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| //Astron. Astrophys.// **705**, Art. No. A132 (2026).\\ | //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.\\ | 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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| | A. Belloche, S. Spezzano, A. Coutens, M. N. Drozdovskaya, J. K. Jørgensen, J.-E. Lee, A. L. Plunkett, D. Harsono, S. Maret, F. Cruz-Sáenz de Miera, J.-H. Jeong, P. Nazari, Y.-L. Yang, H.-S. Yun, and S. Zeng\\ |
| | described\\ |
| | **[[https://doi.org/10.1051/0004-6361/202659642|Complex Organic Molecules in Protostars with ALMA Spectral Surveys (COMPASS) − VII. First Interstellar Detection of Fully Deuterated Methanol]]**\\ |
| | //Astron. Astrophys.// **714**, Art. No. A55 (2026).\\ |
| | CD<sub>3</sub>OD, along with many other methanol isotopologs, was detected toward IRAS4A2 in the NGC 1333 molecular cloud in the course of the molecular line survey mentioned in the title and carried with ALMA between 279.0 and 311.7 GHz. Deuteration is very high in the methyl group with the abundance of CHD<sub>2</sub>OH being only slightly smaller than that of CH<sub>2</sub>DOH and CD<sub>3</sub>OH only slightly less than half of CHD<sub>2</sub>OH. Deuteration is less pronounced in the hydroxyl group, as commonly observed, the abundance of CH<sub>3</sub>OD is about a factor of 1.5 lower than that of CD<sub>3</sub>OH, and the ratio between CD<sub>3</sub>OH and CD<sub>3</sub>OD is ~22.5. CH<sub>3</sub><sup>17</sup>OH was also detected clearly a factor of 4 less than CH<sub>3</sub><sup>18</sup>OH. The detection of numerous isotopologs in their excited torsional states is unsurprising because of a rotational temperature of ~200 K. The lack of laboratory data accounts for CH<sub>2</sub>DOH and CHD<sub>2</sub>OH being not detected in torsionally excited states.\\ |
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| | MPIfR issued press releases **[[https://www.mpifr-bonn.mpg.de/pressemeldungen/2026/erster-nachweis-von-schwerem-methanol-im-weltraum?c=8727|in German]]** and in **[[https://www.mpifr-bonn.mpg.de/pressreleases/2026/first-detection-of-heavy-methanol-in-space|in English]]**. Press releases were also issued by other participating institutions.\\ |
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| === (Far) Infrared observations of Methanol === | === (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\\ | 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; 04, 2026 | Contributor(s): H. S. P. Müller; 04, 2022; 08, 2024; 02, 2026; 04, 2026; 10, 2026 |
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