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| molecules:ism:h2cn [2021/10/13 14:13] – mueller | molecules:ism:h2cn [2021/10/13 14:16] – mueller |
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| **[[https://doi.org/10.1051/0004-6361/201935010|Isocyanogen Formation in the Cold Interstellar Medium]]**,\\ | **[[https://doi.org/10.1051/0004-6361/201935010|Isocyanogen Formation in the Cold Interstellar Medium]]**,\\ |
| //Astron. Astrophys.// **625**, art. no. A91 (2019).\\ | //Astron. Astrophys.// **625**, art. no. A91 (2019).\\ |
| A molecular line survey of the prestellar cor L1544 between 71.74 and 115.87 GHz was carried out with the IRAM 30 m telescope. Methyleneamidogen was observed through six hyperfine transitions around 73.4 GHz.\\ | A molecular line survey of the prestellar core L1544 between 71.74 and 115.87 GHz was carried out with the IRAM 30 m telescope. Methyleneamidogen was observed through six hyperfine transitions around 73.4 GHz.\\ |
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| **[[https://doi.org/10.1051/0004-6361/202141491|Interstellar Detection of the Simplest Aminocarbyne H<sub>2</sub>NC: An ignored but Abundant Molecule]]**,\\ | **[[https://doi.org/10.1051/0004-6361/202141491|Interstellar Detection of the Simplest Aminocarbyne H<sub>2</sub>NC: An ignored but Abundant Molecule]]**,\\ |
| //Astron. Astrophys.// **654**, art. no. A45 (2021).\\ | //Astron. Astrophys.// **654**, art. no. A45 (2021).\\ |
| The authors give accounts on methyleneamidogen in the L483 and B1-b protostellar objects from earlier molecular line surveys carried out at 3 mm using the IRAM 30 m telescope. The molecule was **not** detected in corresponding data of the prestellar core TMC-1. The column densities of H<sub>2</sub>CN and H<sub>2</sub>NC were essentially the same in the first two sources.\\ | The authors give accounts on methyleneamidogen in the L483 and B1-b protostellar objects from earlier molecular line surveys carried out at 3 mm using the IRAM 30 m telescope; the L483 results were mentioned in an earlier publication, but only a column density was given. The molecule was **not** detected in corresponding data of the prestellar core TMC-1. The column densities of H<sub>2</sub>CN and H<sub>2</sub>NC were essentially the same in the first two sources.\\ |
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