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| molecules:ism:hccnc [2019/10/23 17:04] – mueller | molecules:ism:hccnc [2024/04/08 17:57] – mueller |
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| **[[https://ui.adsabs.harvard.edu/abs/1992ApJ...386L..51K|Detection of Isocyanoacetylene HCCNC in TMC-1]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1992ApJ...386L..51K|Detection of Isocyanoacetylene HCCNC in TMC-1]]**\\ |
| //Astrophys. J.// **386**, L51 (1992).\\ | //Astrophys. J.// **386**, L51 (1992).\\ |
| The Nobeyama 45 m telescope was used to detect the //J// = 4 – 3, 5 – 4, and 9 – 8 transitions near 39.7, 49.7, and 89.4 GHz. The [[http://www.astro.uni-koeln.de/site/vorhersagen/molecules/ism/HNC3.html|HNC<sub>3</sub>]] isomer was found shortly thereafter, whereas the HC<sub>3</sub>N isomer had been known for a considerable time. | The Nobeyama 45 m telescope was used to detect the //J// = 4 – 3, 5 – 4, and 9 – 8 transitions near 39.7, 49.7, and 89.4 GHz. The [[http://www.astro.uni-koeln.de/site/vorhersagen/molecules/ism/HNC3.html|HNC<sub>3</sub>]] isomer was found shortly thereafter, whereas the HC<sub>3</sub>N isomer had been known for a considerable time.\\ |
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| P. D. Gensheimer reported on\\ | P. D. Gensheimer reported on\\ |
| **[[https://doi.org/10.1023/A:1000744924767|Observations of HCCNC and HNCCC in IRC+10216]]**\\ | **[[https://doi.org/10.1023/A:1000744924767|Observations of HCCNC and HNCCC in IRC+10216]]**\\ |
| //Astrophys. Space Sci.// **251**, 199 (1997).\\ | //Astrophys. Space Sci.// **251**, 199 (1997).\\ |
| The IRAM 30 m telescope was used to detect the //J// = 9 – 8, 14 – 13, and 21 – 20 transitions near 89.4, 139.1, and 208.6 GHz. The HC<sub>3</sub>N to HCCNC ratio is around 150, somewhat higher than in TMC-1. | The IRAM 30 m telescope was used to detect the //J// = 9 – 8, 14 – 13, and 21 – 20 transitions near 89.4, 139.1, and 208.6 GHz. The HC<sub>3</sub>N to HCCNC ratio is around 150, somewhat higher than in TMC-1.\\ |
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| A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito\\ | A. Belloche, H. S. P. Müller, K. M. Menten, P. Schilke, and C. Comito\\ |
| **[[https://doi.org/10.1051/0004-6361/201321096|Complex Organic Molecules in the Interstellar Medium: IRAM 30 m Line Survey of Sagittarius B2(N) and (M)]]**\\ | **[[https://doi.org/10.1051/0004-6361/201321096|Complex Organic Molecules in the Interstellar Medium: IRAM 30 m Line Survey of Sagittarius B2(N) and (M)]]**\\ |
| //Astron. Astrophys.// **559**, Art. No. A47 (2013).\\ | //Astron. Astrophys.// **559**, Art. No. A47 (2013).\\ |
| The //J// = 10 – 9 and 11 – 10 transitions near 99.4 and 109.3 GHz were detected, the latter possibly blended with part of a methyl formate transitions. Overall, this detections is tentative. | The //J// = 10 – 9 and 11 – 10 transitions near 99.4 and 109.3 GHz were detected, the latter possibly blended with part of a methyl formate transitions. Overall, this detections is tentative.\\ |
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| C. Vastel, K. Kawaguchi, D. Quénard, M. Ohishi, B. Lefloch, R. Bachiller, and H. S. P. Müller\\ | C. Vastel, K. Kawaguchi, D. Quénard, M. Ohishi, B. Lefloch, R. Bachiller, and H. S. P. Müller\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201731262|The Observed Chemical Structure of L1544]]**\\ | **[[http://dx.doi.org/10.1051/0004-6361/201731262|The Observed Chemical Structure of L1544]]**\\ |
| //Astron. Astrophys.// **606**, Art. No. A82 (2017)\\ | //Astron. Astrophys.// **606**, Art. No. A82 (2017)\\ |
| by S. Spezzano, P. Caselli, L. Bizzocchi, B. M. Giuliano, and V. Lattanzi. | by S. Spezzano, P. Caselli, L. Bizzocchi, B. M. Giuliano, and V. Lattanzi.\\ |
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| | J. Cernicharo, N. Marcelino, M. Agúndez, C. Bermúdez, C. Cabezas, B. Tercero, and J. R. Pardo\\ |
| | reported on the\\ |
| | **[[https://doi.org/10.1051/0004-6361/202039274|Discovery of HC<sub>4</sub>NC in TMC-1: A study of the isomers of HC<sub>3</sub>N, HC<sub>5</sub>N, and HC<sub>7</sub>N]]**\\ |
| | //Astron. Astrophys.// **642**, Art. No. L8 (2020).\\ |
| | The authors report the detections of the <sup>13</sup>C isotopomers of HCCNC as well as that of DCCNC. The observations were obtained with the Yebes 40m radio telescope in the course of a line survey covering 31.0–50.3 GHz.\\ |
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| | J. Cernicharo, B. Tercero, C. Cabezas, M. Agúndez, E. Roueff, R. Fuentetaja, N. Marcelino, and P. de Vicente\\ |
| | carried out more recently a\\ |
| | **[[https://doi.org/10.1051/0004-6361/202348822|Study of the HCCNC and HNCCC isotopologs in TMC-1]]**\\ |
| | //Astron. Astrophys.// **682**, Art. No. L13 (2024).\\ |
| | They reported in the framework of improved data of the above survey the detection of HCC<sup>15</sup>NC with a <sup>14</sup>N/<sup>15</sup>N ratio of roughly 240, slightly lower than ~317 obtained for HC<sub>3</sub>N. However, this value may be affected by a probable but at that time unrecognized blending of the //J// = 5 − 4 transition of HCC<sup>15</sup>NC (J. Cernicharo, private communication). They also redetermined the <sup>12</sup>C/<sup>13</sup>C ratios. The values are ~95 with scatter that is insignificant with respect to the uncertainties. These values are somewhat lower than ~65 usually found in the the local ISM, but very similar to values of HNC<sub>3</sub> <sup>13</sup>C isotopomers and to two of the three HC<sub>3</sub>N <sup>13</sup>C isotopomers. An H/D ratio of ~31 was reported, but it appears again as if the //J// = 5 − 4 transition of DCCNC is too strong. The ratio from 4 − 3 alone would be closer to ~55 observed for HNC<sub>3</sub> and HC<sub>3</sub>N.\\ |
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| Contributor(s): H. S. P. Müller; 12, 2017 | Contributor(s): H. S. P. Müller; 12, 2017; 11, 2020; 04, 2024 |
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