This shows you the differences between two versions of the page.
| Both sides previous revision Previous revision Next revision | Previous revision |
| molecules:ism:vynh2 [2021/12/06 14:04] – mueller | molecules:ism:vynh2 [2022/03/08 14:52] (current) – mueller |
|---|
| //Astrophys. J. Lett.// **920** (2021), Art. No. L27.\\ | //Astrophys. J. Lett.// **920** (2021), Art. No. L27.\\ |
| Vinylamine (C<sub>2</sub>H<sub>3</sub>NH<sub>2</sub>) was detected through five un- or slightly blended transitions and four partially blended transitions with 4 ≤ //J// ≤ 9 and //K<sub>a</sub>// ≤ 3 in the course of an unbiased molecular line survey of the quiescent giant molecular cloud G+0.693−0.027, about 1' north-east of Sagittarius B2(N), carried out with the IRAM 30 m dish at 3 mm. The lines were modeled quite well employing an LTE fit with //T//<sub>rot</sub> = 18 ± 3 K. Vinylamine is about a factor of 50 less abundant than methylamine.\\ | Vinylamine (C<sub>2</sub>H<sub>3</sub>NH<sub>2</sub>) was detected through five un- or slightly blended transitions and four partially blended transitions with 4 ≤ //J// ≤ 9 and //K<sub>a</sub>// ≤ 3 in the course of an unbiased molecular line survey of the quiescent giant molecular cloud G+0.693−0.027, about 1' north-east of Sagittarius B2(N), carried out with the IRAM 30 m dish at 3 mm. The lines were modeled quite well employing an LTE fit with //T//<sub>rot</sub> = 18 ± 3 K. Vinylamine is about a factor of 50 less abundant than methylamine.\\ |
| Using additional observations with the Yebes 40 m dish at 7 mm, the authors identify tentatively four lines of ethylamine (C<sub>2</sub>H<sub>5</sub>NH<sub>2</sub>) with modest signal-to-noise ratio that appear to be not or only slightly blended and three that are somewhat more blended. The fit results suggest that ethylamine would be about a factor of 125 less abundant than methylamine.\\ | Using additional observations with the Yebes 40 m dish at 7 mm, the authors identify tentatively four lines of ethylamine (C<sub>2</sub>H<sub>5</sub>NH<sub>2</sub>) with modest signal-to-noise ratio that appear to be not or only slightly blended and three that are somewhat more blended. The fit results suggest that ethylamine would be about a factor of 125 less abundant than methylamine. The identification appears to be very reasonable. Therefore, the molecule shows now up in the table as tentatively detected.\\ |
| |
| ---- | ---- |
| |
| Contributor(s): H. S. P. Müller; 12, 2021 | Contributor(s): H. S. P. Müller; 12, 2021; 03, 2022 |
| |
| ---- | ---- |
| |