This shows you the differences between two versions of the page.
| Both sides previous revision Previous revision | |
| molecules:ism:dms [2025/02/26 14:46] – mueller | molecules:ism:dms [2025/02/26 14:46] (current) – mueller |
|---|
| **[[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. 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.\\ | 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.\\ |
| \\ | \\ |
| |