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| molecules:extragalactic:l-c3h_extragalactic [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:extragalactic:l-c3h_extragalactic [2019/10/22 16:22] (current) – mueller |
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| S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\ | S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\ |
| used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\ | used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201117096|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]**\\ | **[[https://doi.org/10.1051/0004-6361/201117096|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]**\\ |
| //Astron. Astrophys.// **535**, (2011) Art. No. A103.\\ | //Astron. Astrophys.// **535**, (2011) Art. No. A103.\\ |
| Propynylidyne, //l//-C<sub>3</sub>H, was identified by its //J// = 7/2 – 5/2 transition of the lower energy fine structure component <sup>2</sup>Π<sub>1/2</sub> with a rest frequency of 76.2 GHz. The Λ-doubling was marginally resolved, the H-hyperfine structure was not resolved. The detection can probably be viewed as secure because of the strong signal and the moderate line number density. | Propynylidyne, //l//-C<sub>3</sub>H, was identified by its //J// = 7/2 – 5/2 transition of the lower energy fine structure component <sup>2</sup>Π<sub>1/2</sub> with a rest frequency of 76.2 GHz. The Λ-doubling was marginally resolved, the H-hyperfine structure was not resolved. The detection can probably be viewed as secure because of the strong signal and the moderate line number density. |
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| Contributor(s): H. S. P. Müller; 5, 2012 | Contributor(s): H. S. P. Müller; 5, 2012 |
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