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| molecules:ism:cyanomethanimin [2019/02/27 12:26] – external edit 127.0.0.1 | molecules:ism:cyanomethanimin [2019/10/23 22:08] (current) – mueller |
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| ===== The Detection of Cyanomethanimine in the ISM ===== | ===== The Detection of Cyanomethanimine in the ISM ===== |
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| Cyanomethanimine, HNCHCN, is a slightly unsaturated sibling of [[http://www.astro.uni-koeln.de/site/vorhersagen/molecules/ism/AAN.html|aminoacetonitrile]], H<sub>2</sub>NCH<sub>2</sub>CN. It has been identified recently by\\ | Cyanomethanimine, HNCHCN, is a slightly unsaturated sibling of [[molecules:ism:aan|aminoacetonitrile]], H<sub>2</sub>NCH<sub>2</sub>CN. It has been identified recently by\\ |
| D. P. Zaleski, N. A. Seifert, A. L. Steber, M. T. Muckle, R. A. Loomis, J. F. Corby, O. Martinez, Jr., K. N. Crabtree, P. R. Jewell, J. M. Hollis, F. J. Lovas, D. Vasquez, J Nyiramahirw, N. Sciortino, K. Johnson, M. C. McCarthy, A. J. Remijan, and B. H. Pate,\\ | D. P. Zaleski, N. A. Seifert, A. L. Steber, M. T. Muckle, R. A. Loomis, J. F. Corby, O. Martinez, Jr., K. N. Crabtree, P. R. Jewell, J. M. Hollis, F. J. Lovas, D. Vasquez, J Nyiramahirw, N. Sciortino, K. Johnson, M. C. McCarthy, A. J. Remijan, and B. H. Pate,\\ |
| **[[http://dx.doi.org/10.1088/2041-8205/765/1/L10|Detection of //E//-Cyanomethanimine toward Sagittarius B2(N) in the Green Bank Telescope PRIMOS Survey]]**\\ | **[[https://doi.org/10.1088/2041-8205/765/1/L10|Detection of //E//-Cyanomethanimine toward Sagittarius B2(N) in the Green Bank Telescope PRIMOS Survey]]**\\ |
| //Astrophys. J// **765**, Art. No. 10 (2013).\\ | //Astrophys. J// **765**, Art. No. 10 (2013).\\ |
| 8 rotational transitions were detected for the higher energy //E//-conformer and none for the lower energy //Z//-conformer. The non-observation of the //Z//-conformer was attributed to the much smaller dipole moment components. The transitions had //J// < 5 and //K<sub>a</sub>// < 1, occured between 9 and 48 GHz and were all seen in absorption. Some transitions displayed <sup>14</sup>N hyperfine splitting. The lines were detected in the two well known velocity components 64 km/s and 82 km/s, though (partial) overlap occured for the latter in some lines. A rotational temperature of about 8 K was derived.\\ | 8 rotational transitions were detected for the higher energy //E//-conformer and none for the lower energy //Z//-conformer. The non-observation of the //Z//-conformer was attributed to the much smaller dipole moment components. The transitions had //J// < 5 and //K<sub>a</sub>// < 1, occured between 9 and 48 GHz and were all seen in absorption. Some transitions displayed <sup>14</sup>N hyperfine splitting. The lines were detected in the two well known velocity components 64 km/s and 82 km/s, though (partial) overlap occured for the latter in some lines. A rotational temperature of about 8 K was derived.\\ |
| These, as well as other observations of fairly complex molecules toward Sgr B2(N) at apperently low rotational temperatures, may be related to findings by\\ | These, as well as other observations of fairly complex molecules toward Sgr B2(N) at apperently low rotational temperatures, may be related to findings by\\ |
| M. A. Requena-Torres, J. Martín-Pintado, A. Rodríguez-Franco, S. Martín, N. J. Rodríguez-Fernández, and P. de Vicente,\\ | M. A. Requena-Torres, J. Martín-Pintado, A. Rodríguez-Franco, S. Martín, N. J. Rodríguez-Fernández, and P. de Vicente,\\ |
| **[[http://dx.doi.org/10.1051/0004-6361:20065190|Organic Molecules in the Galactic Center – Hot Core Chemistry without Hot Cores]]**\\ | **[[https://doi.org/10.1051/0004-6361:20065190|Organic Molecules in the Galactic Center – Hot Core Chemistry without Hot Cores]]**\\ |
| //Astron. Astrophys.// **455**, 971–985 (2006);\\ | //Astron. Astrophys.// **455**, 971–985 (2006);\\ |
| and by\\ | and by\\ |
| M. A. Requena-Torres, J. Martín-Pintado, S. Martín, and M. R. Morris,\\ | M. A. Requena-Torres, J. Martín-Pintado, S. Martín, and M. R. Morris,\\ |
| **[[http://dx.doi.org/10.1086/523627|The Galactic Center: The Largest Oxygen-bearing Organic Molecule Repository]]**\\ | **[[https://doi.org/10.1086/523627|The Galactic Center: The Largest Oxygen-bearing Organic Molecule Repository]]**\\ |
| //Astrophys. J.// **672**, 352–360 (2008). | //Astrophys. J.// **672**, 352–360 (2008). |
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| V. M. Rivilla, J. Martín-Pintado, I. Jiménez-Serra, S. Zeng, S. Martín, J. Armijos-Abendañdo, M. A. Requena-Torres, R. Aladro, and D. Riquelme\\ | V. M. Rivilla, J. Martín-Pintado, I. Jiménez-Serra, S. Zeng, S. Martín, J. Armijos-Abendañdo, M. A. Requena-Torres, R. Aladro, and D. Riquelme\\ |
| reported on\\ | reported on\\ |
| **[[http://dx.doi.org/10.1093/mnrasl/sly228|Abundant Z-cyanomethanimine in the Interstellar Medium: Paving the Way to the Synthesis of Adenine]]**\\ | **[[https://doi.org/10.1093/mnrasl/sly228|Abundant Z-cyanomethanimine in the Interstellar Medium: Paving the Way to the Synthesis of Adenine]]**\\ |
| //Mon. Not. R. Soc. Astron.// **483**, L114–L119 (2019).\\ | //Mon. Not. R. Soc. Astron.// **483**, L114–L119 (2019).\\ |
| The results were obtained in the course of a line survey of the Galactic center source G 0.693–0.03 at 3 mm using the IRAM 30 m dish; additional observation around 1.3 cm were carried out with the GBT 100 m dish. The E-conformer was also identified. The Z/E ratio of about six indicated thermal equilibrium at the kinetic temperature of the cloud. The excitation temperature, in contrast, is rather cold, about 8 K. | The results were obtained in the course of a line survey of the Galactic center source G 0.693–0.03 at 3 mm using the IRAM 30 m dish; additional observation around 1.3 cm were carried out with the GBT 100 m dish. The E-conformer was also identified. The Z/E ratio of about six indicated thermal equilibrium at the kinetic temperature of the cloud. The excitation temperature, in contrast, is rather cold, about 8 K. |
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| Contributor(s): H. S. P. Müller; 02, 2013; 01, 2019 | Contributor(s): H. S. P. Müller; 02, 2013; 01, 2019 |
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