S. Zeng, I. Jiménez-Serra, V. M. Rivilla, J. Martín-Pintado, L. F. Rodríguez-Almeida, B. Tercero, P. de Vicente, F. Rico-Villas, L. Colzi, S. Martín, and M. A. Requena-Torres
reported on
Probing the Chemical Complexity of Amines in the ISM: Detection of Vinylamine (C<sub>2</sub>H<sub>3</sub>NH<sub>2</sub>) and Tentative Detection of Ethylamine (C<sub>2</sub>H<sub>5</sub>NH<sub>2</sub>)
Astrophys. J. Lett. 920 (2021), Art. No. L27.
Vinylamine (C2H3NH2) was detected through five un- or slightly blended transitions and four partially blended transitions with 4 ≤ J ≤ 9 and Ka ≤ 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 Trot = 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 (C2H5NH2) 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.


Contributor(s): H. S. P. Müller; 12, 2021


  • molecules/ism/vynh2.txt
  • Last modified: 2021/12/06 14:04
  • by mueller