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molecules:ism:vcn [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:vcn [2019/10/24 09:25] (current) – mueller |
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Vinyl cyanide, C<sub>2</sub>H<sub>3</sub>CN, aka acrylonitrile or propenenitrile, has been detected first toward Sgr B2:\\ | Vinyl cyanide, C<sub>2</sub>H<sub>3</sub>CN, aka acrylonitrile or propenenitrile, has been detected first toward Sgr B2:\\ |
F. F. Gardner and G. Winnewisser,\\ | F. F. Gardner and G. Winnewisser,\\ |
**[[http://cdsads.u-strasbg.fr/abs/1975ApJ...195L.127G|The Detection of Interstellar Vinyl Cyanide (Acrylonitrile)]]**,\\ | **[[https://ui.adsabs.harvard.edu/abs/1975ApJ...195L.127G|The Detection of Interstellar Vinyl Cyanide (Acrylonitrile)]]**,\\ |
//Astrophys. J.// **195**, L127–L130 (1975). | //Astrophys. J.// **195**, L127–L130 (1975). |
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The molecule was also detected in the dark cloud TMC-1:\\ | The molecule was also detected in the dark cloud TMC-1:\\ |
H.E. Matthews and T.J. Sears,\\ | H.E. Matthews and T.J. Sears,\\ |
**[[http://adsabs.harvard.edu/abs/1983ApJ...272..149M|The Detection of Vinyl Cyanide in TMC-1]]**,\\ | **[[https://ui.adsabs.harvard.edu/abs/1983ApJ...272..149M|The Detection of Vinyl Cyanide in TMC-1]]**,\\ |
//Astrophys. J.// **272**, 149–153 (1983). | //Astrophys. J.// **272**, 149–153 (1983). |
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It was seen also in one of three translucent clouds (CB 17):\\ | It was seen also in one of three translucent clouds (CB 17):\\ |
B. E. Turner, R. Terzieva, and E. Herbst,\\ | B. E. Turner, R. Terzieva, and E. Herbst,\\ |
**[[http://dx.doi.org/10.1086/307300|The Physics and Chemistry of Small Translucent Molecular Clouds. XII. More Complex Species Explainable by Gas-Phase Processes]]**\\ | **[[https://doi.org/10.1086/307300|The Physics and Chemistry of Small Translucent Molecular Clouds. XII. More Complex Species Explainable by Gas-Phase Processes]]**\\ |
//Astrophys. J.// **518**, 699–732 (1999). | //Astrophys. J.// **518**, 699–732 (1999). |
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Quite recently, C<sub>2</sub>H<sub>3</sub>CN was among several molecules detected with the IRAM 30 m telecope in the circumstellar envelope of the carbon-rich AGB star CW Leo, aka IRC +10216:\\ | Quite recently, C<sub>2</sub>H<sub>3</sub>CN was among several molecules detected with the IRAM 30 m telecope in the circumstellar envelope of the carbon-rich AGB star CW Leo, aka IRC +10216:\\ |
M. Agúndez, J. P. Fonfría Expósito, J. Cernicharo, J. R. Pardo and M. Guélin,\\ | M. Agúndez, J. P. Fonfría Expósito, J. Cernicharo, J. R. Pardo and M. Guélin,\\ |
**[[http://dx.doi.org/10.1051/0004-6361:20078956|Detection of Circumstellar CH<sub>2</sub>CHCN, CH<sub>2</sub>CN, CH<sub>3</sub>CCH, and H<sub>2</sub>CS]]**\\ | **[[https://doi.org/10.1051/0004-6361:20078956|Detection of Circumstellar CH<sub>2</sub>CHCN, CH<sub>2</sub>CN, CH<sub>3</sub>CCH, and H<sub>2</sub>CS]]**\\ |
//Astron. Astrophys.// **479**, 493–501 (2008). | //Astron. Astrophys.// **479**, 493–501 (2008). |
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Vinyl cyanide in its two lowest vibrational states //v//<sub>11</sub> = 1 (in plane CCN bend; 239 cm<sup>–1</sup>) and //v//<sub>15</sub> = 1 (out of plane CCN bend; 340 cm<sup>–1</sup>) has been detected toward Sgr B2(N):\\ | Vinyl cyanide in its two lowest vibrational states //v//<sub>11</sub> = 1 (in plane CCN bend; 239 cm<sup>–1</sup>) and //v//<sub>15</sub> = 1 (out of plane CCN bend; 340 cm<sup>–1</sup>) has been detected toward Sgr B2(N):\\ |
A. Nummelin, P. Bergman,\\ | A. Nummelin, P. Bergman,\\ |
**[[http://cdsads.u-strasbg.fr/abs/1999A%26A...341L..59N|Vibrationally Excited Vinyl Cyanide in Sgr B2(N)]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1999A%26A...341L..59N|Vibrationally Excited Vinyl Cyanide in Sgr B2(N)]]**\\ |
//Astron. Astrophys.// **341**, L59–L62 (1999).\\ | //Astron. Astrophys.// **341**, L59–L62 (1999).\\ |
Previously, three and two lines, respectively, detected in an Orion KL survey have been assigned to vinyl cyanide in its //v//<sub>11</sub> = 1 and //v//<sub>15</sub> = 1 states:\\ | Previously, three and two lines, respectively, detected in an Orion KL survey have been assigned to vinyl cyanide in its //v//<sub>11</sub> = 1 and //v//<sub>15</sub> = 1 states:\\ |
P. Schilke, T. D. Groesbeck, G. A. Blake, and T. G. Phillips,\\ | P. Schilke, T. D. Groesbeck, G. A. Blake, and T. G. Phillips,\\ |
**[[http://dx.doi.org/10.1086/312948|A Line Survey of Orion KL from 325 to 360 GHz]]**,\\ | **[[https://doi.org/10.1086/312948|A Line Survey of Orion KL from 325 to 360 GHz]]**,\\ |
//Astrophys. J. Suppl. Ser.// **108**, 301–337 (1997). | //Astrophys. J. Suppl. Ser.// **108**, 301–337 (1997). |
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Observations of <sup>13</sup>C singly substituted species in Sgr B2(N) have been reported:\\ | Observations of <sup>13</sup>C singly substituted species in Sgr B2(N) have been reported:\\ |
H. S. P. Müller, A. Belloche, K. M. Menten, C. Comito, and P. Schilke,\\ | H. S. P. Müller, A. Belloche, K. M. Menten, C. Comito, and P. Schilke,\\ |
**[[http://dx.doi.org/10.1016/j.jms.2008.03.016|Rotational Spectroscopy of Isotopic Vinyl Cyanide, H<sub>2</sub>C=CH–C≡N, in the Laboratory and in Space]]**,\\ | **[[https://doi.org/10.1016/j.jms.2008.03.016|Rotational Spectroscopy of Isotopic Vinyl Cyanide, H<sub>2</sub>C=CH–C≡N, in the Laboratory and in Space]]**,\\ |
//J. Mol. Spectrosc.// **250**, 319–325 (2008).\\ | //J. Mol. Spectrosc.// **250**, 319–325 (2008).\\ |
The astronomical observations are based on a molecular line survey carried out with the IRAM 30 m telescope at 3 mm with additional measurements at 2 and 1.3 mm. | The astronomical observations are based on a molecular line survey carried out with the IRAM 30 m telescope at 3 mm with additional measurements at 2 and 1.3 mm. |
The molecular line survey, mentioned in the previous paragraph, was described in detail by\\ | The molecular line survey, mentioned in the previous paragraph, was described in detail by\\ |
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:\\ |
**[[http://dx.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).\\ |
A total of six excited vibrational states of vinyl cyanide were observed in this work. They are //v//<sub>11</sub> = 1, //v//<sub>15</sub> = 1, which both were seen before, plus newly //v//<sub>11</sub> = 2, //v//<sub>11</sub> = //v//<sub>15</sub> = 1, //v//<sub>11</sub> = 3, and //v//<sub>11</sub> = 3. The latter state has a vibrational energy of about 688 cm<sup>–1</sup> or about 990 K. | A total of six excited vibrational states of vinyl cyanide were observed in this work. They are //v//<sub>11</sub> = 1, //v//<sub>15</sub> = 1, which both were seen before, plus newly //v//<sub>11</sub> = 2, //v//<sub>11</sub> = //v//<sub>15</sub> = 1, //v//<sub>11</sub> = 3, and //v//<sub>11</sub> = 3. The latter state has a vibrational energy of about 688 cm<sup>–1</sup> or about 990 K. |
A. López, B. Tercero, Z. Kisiel, A. M. Daly, C. Bermúdez, H. Calcutt, N. Marcelino, S. Viti, B.J. Drouin, I. R. Medvedev, C. F. Neese, L. Pszczólkowski, J. L. Alonso, and J. Cernicharo\\ | A. López, B. Tercero, Z. Kisiel, A. M. Daly, C. Bermúdez, H. Calcutt, N. Marcelino, S. Viti, B.J. Drouin, I. R. Medvedev, C. F. Neese, L. Pszczólkowski, J. L. Alonso, and J. Cernicharo\\ |
reported on\\ | reported on\\ |
**[[http://dx.doi.org/10.1051/0004-6361/201423622|Laboratory Characterization and Astrophysical Detection of Vibrationally Excited States of Vinyl Cyanide in Orion-KL]]**\\ | **[[https://doi.org/10.1051/0004-6361/201423622|Laboratory Characterization and Astrophysical Detection of Vibrationally Excited States of Vinyl Cyanide in Orion-KL]]**\\ |
//Astron. Astrophys.// **572**, (2014), Art. No. A44.\\ | //Astron. Astrophys.// **572**, (2014), Art. No. A44.\\ |
The authors detect one further state newly, //v//<sub>10</sub> = 1, which interacts strongly with //v//<sub>11</sub> = //v//<sub>15</sub> = 1. | The authors detect one further state newly, //v//<sub>10</sub> = 1, which interacts strongly with //v//<sub>11</sub> = //v//<sub>15</sub> = 1. |
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Contributor(s): H. S. P. Müller, 12, 2003; 06, 2008; 03, 2012; 11, 2014 | Contributor(s): H. S. P. Müller, 12, 2003; 06, 2008; 03, 2012; 11, 2014 |
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