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| molecules:ism:dms [2025/02/26 14:24] – mueller | molecules:ism:dms [2025/02/26 14:46] (current) – mueller |
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| **[[https://doi.org/10.3847/2041-8213/adafa7|On the Abiotic Origin of Dimethyl Sulfide: Discovery of Dimethyl Sulfide in the Interstellar Medium]]**\\ | **[[https://doi.org/10.3847/2041-8213/adafa7|On the Abiotic Origin of Dimethyl Sulfide: Discovery of Dimethyl Sulfide in the Interstellar Medium]]**\\ |
| //Astrophys. J. Lett.// **980**, Art. No. L37 (2025).\\ | //Astrophys. J. Lett.// **980**, Art. No. L37 (2025).\\ |
| Dimethyl sulfide, (CH<sub>3</sub>)<sub>2</sub>S, was identified in the course of a molecular line survey of the Galactic center cold molecular cloud G+0.693−0.027 carried out with the Yebes 40 m and IRAM 30 m radio telescopes. Several //b//-type lines with 2 ≤ //J// ≤ 9, //K<sub>c</sub>// ≤ 4, and with unresolved internal rotation splitting were assigned with reasonable signal-to-noise ratios, but a number of these are blended to different amounts. Both molecules have excitation temperatures of about 15 K, and propene has an about three times higher column density than isobutene. Isobutene is only the second molecules with a branched carbon chain after isopropyl cyanide.\\ | Dimethyl sulfide, (CH<sub>3</sub>)<sub>2</sub>S, was identified in the course of a molecular line survey of the Galactic center cold molecular cloud G+0.693−0.027 carried out with the Yebes 40 m and IRAM 30 m radio telescopes. Several //b//-type lines with 2 ≤ //J// ≤ 9, //K<sub>a</sub>// ≤ 4, and with unresolved internal rotation splitting were assigned with reasonable signal-to-noise ratios, but a number of these are blended to different amounts. The excitation temperatures was determined as 13 ± 3 K. Its column density is about a factor of 30 lower than than of its oxigen homolog dimethyl ether and about a factor of 1.6 lower than its ethanethiol isomer.\\ |
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