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| molecules:ism:mgc3n [2019/10/07 17:38] – mueller | molecules:ism:mgc3n [2021/09/03 17:25] – mueller |
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| ===== Detection of Magnesium Monocyanoacetylide, MgC<sub>3</sub>N, toward CW Leonis ===== | ===== Detection of Magnesium Monocyanoacetylides toward CW Leonis ===== |
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| J. Cernicharo, C. Cabezas, J. R. Pardo, M. Agúndez, C. Bermúdez, L. Velilla-Prieto, F. Tercero, J. A. López-Pérez, J. D. Gallego, J. P. Fonfría, G. Quintana-Lacaci, M. Guélin, and Y. Endo\\ | J. Cernicharo, C. Cabezas, J. R. Pardo, M. Agúndez, C. Bermúdez, L. Velilla-Prieto, F. Tercero, J. A. López-Pérez, J. D. Gallego, J. P. Fonfría, G. Quintana-Lacaci, M. Guélin, and Y. Endo\\ |
| MgC<sub>3</sub>N and MgC<sub>4</sub>H]]**\\ | MgC<sub>3</sub>N and MgC<sub>4</sub>H]]**\\ |
| //Astron. Astrophys.// **630**, Art. No. L2 (2019).\\ | //Astron. Astrophys.// **630**, Art. No. L2 (2019).\\ |
| The 40 m Centro Astronómico de Yebes dish and the IRAM 30 m dish were employed to observed 22 rotational transitions of magnesium monocyanoacetylide, MgC<sub>3</sub>N, between //N'// = 12 and 40 and between 33 and 111 GHz toward the famous near-by carbon-rich AGB star CW Leonis. Many transitions show decent to good signal-to-noise ratios and are not or only slightly blended. Fine structure splitting is well-resolved at lower frequencies. The astronomical data were employed to derive spectroscopic parameters in the absence of laboratory data. | The 40 m Centro Astronómico de Yebes dish and the IRAM 30 m dish were employed to observed 22 rotational transitions of magnesium monocyanoacetylide, MgC<sub>3</sub>N, between //N'// = 12 and 40 and between 33 and 111 GHz toward the famous near-by carbon-rich AGB star CW Leonis. Many transitions show decent to good signal-to-noise ratios and are not or only slightly blended. Fine structure splitting is well-resolved at lower frequencies. The astronomical data were employed to derive spectroscopic parameters in the absence of laboratory data.\\ |
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| | J. R. Pardo, C. Cabezas, J. P. Fonfría, M. Agúndez, B. Tercero, P. de Vicente, M. Guélin and J. Cernicharo |
| | reported on\\ |
| | **[[https://doi.org/10.1051/0004-6361/202141671|Magnesium Radicals MgC<sub>5</sub>N and MgC<sub>6</sub>H in IRC +10216]]**\\ |
| | //Astron. Astrophys.// **652**, Art. No. L13 (2021).\\ |
| | The 40 m Centro Astronómico de Yebes dish was employed to observe 15 rotational transitions of magnesium cyanodiacetylide, MgC<sub>5</sub>N, with //N"// = 27 to 41 between 31.0 and 50.3 GHz toward the famous near-by carbon-rich AGB star CW Leonis. Some of the transitions displayed resolved fine structure (FS) splitting. 14 transitions appear to be unblended or only slightly blended. The identification of a new species is unambiguous. The identification of the carrier may be viewed with slight caution in the absence of laboratory data. However, the FS spltting is a very strong indicator that the identification is unambiguous as well. It is very interesting to note that MgC<sub>5</sub>N has a column density only a factor of two lower than that of MgC<sub>3</sub>N, but about a factor of six higher than that of MgCN. The authors justified this by their likely formation which involves radiative association reactions of Mg<sup>+</sup> with HC<sub>2n+1</sub>N. These ratios are similar to thos of the isoelectronic MgC<sub>6</sub>H. MgNC is about a factor of three more abundant than MgC<sub>5</sub>N.\\ |
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| Contributor(s): H. S. P. Müller; 10, 2019 | |
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| | Contributor(s): H. S. P. Müller; 10, 2019; 09, 2021 |
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