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| molecules:ism:phcn [2026/08/13 12:16] – mueller | molecules:ism:phcn [2026/08/13 12:32] (current) – mueller |
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| **[[https://doi.org/10.1038/s41550-020-01253-4|Ubiquitous aromatic carbon chemistry at the earliest stages of star formation]]**\\ | **[[https://doi.org/10.1038/s41550-020-01253-4|Ubiquitous aromatic carbon chemistry at the earliest stages of star formation]]**\\ |
| //Nat. Astron.// **5**, 181–187 (2021).\\ | //Nat. Astron.// **5**, 181–187 (2021).\\ |
| Benzonitrile was detected by the same method as in the first reference toward four additional dark clouds, Serpens 1A, 1B, 2, and L1521F. The HC<sub>7</sub>N///c//-C<sub>6</sub>H<sub>5</sub>CN ratio was found to be around 5 for the first threre sources and ~17 for L1521F, compared with ~23 in TMC-1 derivewd from the previous entry.\\ | Benzonitrile was detected by the same method as in the first reference toward four additional dark clouds, Serpens 1A, 1B, 2, and L1521F. The HC<sub>7</sub>N///c//-C<sub>6</sub>H<sub>5</sub>CN ratio was found to be around 5 for the first threre sources and ~17 for L1521F. The last value is very similar to the one in TMC-1 derivewd from the previous entry.\\ |
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| V. M. Rivilla, D. San Andrés, M. Sanz-Novo, L. Colzi, I. Jiménez-Serra, A. López-Gallifa, A. Martínez-Henares, A. Megías, S. Martín, B. Tercero, S. Zeng, J. Loreau, M. Ben Khalifa, M. A. Requena-Torres and P. de Vicente \\ | V. M. Rivilla, D. San Andrés, M. Sanz-Novo, L. Colzi, I. Jiménez-Serra, A. López-Gallifa, A. Martínez-Henares, A. Megías, S. Martín, B. Tercero, S. Zeng, J. Loreau, M. Ben Khalifa, M. A. Requena-Torres and P. de Vicente \\ |
| announced\\ | announced\\ |
| **[[https://doi.org/10.1051/0004-6361/202660367|Ubiquitous aromatic carbon chemistry at the earliest stages of star formation]]**\\ | **[[https://doi.org/10.1051/0004-6361/202660367|Aromatic Rings in the Central Molecular Zone: Benzonitrile]]**\\ |
| //Astron. Astrophys.// **712**, Art. No. A128 (2026).\\ | //Astron. Astrophys.// **712**, Art. No. A128 (2026).\\ |
| | The molecule was detected in two kinetically warmer, rotationally cold clouds G+0.693−0.027 and G+0.633−0.0604 close to the Galactic center in the course of molecular line surveys with the Yebes 40 m dish. The HC<sub>7</sub>N///c//-C<sub>6</sub>H<sub>5</sub>CN ratios of ~2.15 and ~2.4 are even lower than the values reported earlier. Additional values of comparison are given from other publications, including a value of ~30 in Lupus-1A.\\ |
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