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| molecules:ism:h2cco [2019/02/27 12:26] – external edit 127.0.0.1 | molecules:ism:h2cco [2019/10/23 17:11] (current) – mueller |
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| Ethenone, H<sub>2</sub>CCO, aka ketene, had been identified first in spectra recorded toward Sgr B2(OH) by\\ | Ethenone, H<sub>2</sub>CCO, aka ketene, had been identified first in spectra recorded toward Sgr B2(OH) by\\ |
| B. E. Turner,\\ | B. E. Turner,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1977ApJ...213L..75T|Microwave Detection of Interstellar Ketene]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1977ApJ...213L..75T|Microwave Detection of Interstellar Ketene]]**\\ |
| //Astrophys. J.// **213**, L75–L79 (1977).\\ | //Astrophys. J.// **213**, L75–L79 (1977).\\ |
| The NRAO 11 m telecope was employed to identify three //K<sub>a</sub>// = 1 transitions with //J'// = 4 and 5. The fourth transition and the two //K<sub>a</sub>// = 0 transitions were detected tentatively around 81 and 101 GHz. | The NRAO 11 m telecope was employed to identify three //K<sub>a</sub>// = 1 transitions with //J'// = 4 and 5. The fourth transition and the two //K<sub>a</sub>// = 0 transitions were detected tentatively around 81 and 101 GHz. |
| Evidence for the //J'// = 4, //K<sub>a</sub>// = 0 and 1 transitions were found in Orion A by:\\ | Evidence for the //J'// = 4, //K<sub>a</sub>// = 0 and 1 transitions were found in Orion A by:\\ |
| L. E. B. Johansson, C. Andersson, J. Eldér, P. Friberg, Å. Hjalmarson, B. Höglund, W. M. Irvine, H. Olofsson, and G. Rydbeck,\\ | L. E. B. Johansson, C. Andersson, J. Eldér, P. Friberg, Å. Hjalmarson, B. Höglund, W. M. Irvine, H. Olofsson, and G. Rydbeck,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1984A%26A...130..227J|Spectral Scan of Orion A and IRC +10216 from 72 to 91 GHz]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1984A%26A...130..227J|Spectral Scan of Orion A and IRC +10216 from 72 to 91 GHz]]**\\ |
| //Astron. Astrophys.// **130**, 227–256 (1984). | //Astron. Astrophys.// **130**, 227–256 (1984). |
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| It is also fairly abundant in dark clouds:\\ | It is also fairly abundant in dark clouds:\\ |
| M. Ohishi, K. Kawaguchi, N. Kaifu, W. M. Irvine, Y. C. Minh, S. Yamamoto, S. Saito,\\ | M. Ohishi, K. Kawaguchi, N. Kaifu, W. M. Irvine, Y. C. Minh, S. Yamamoto, S. Saito,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/1991ASPC...16..387O|The Ortho to Para Ratio for Ketene in TMC-1]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1991ASPC...16..387O|The Ortho to Para Ratio for Ketene in TMC-1]]**\\ |
| //ASP Conf. Ser.// **16**, 387–391 (1991). | //ASP Conf. Ser.// **16**, 387–391 (1991). |
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| It was also found in three translucent clouds (CB 17 CB 24, and CB 228):\\ | It was also found in three translucent clouds (CB 17 CB 24, and CB 228):\\ |
| 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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| J. K. Jørgensen, H. S. P. Müller, H. Calcutt, A. Coutens, M. N. Drozdovskaya, K. I. Öberg, M. V. Persson, V. Taquet, E. F. van Dishoeck, and S. F. Wampfler\\ | J. K. Jørgensen, H. S. P. Müller, H. Calcutt, A. Coutens, M. N. Drozdovskaya, K. I. Öberg, M. V. Persson, V. Taquet, E. F. van Dishoeck, and S. F. Wampfler\\ |
| reported on\\ | reported on\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201731667|The ALMA-PILS Survey: Isotopic Composition of Oxygen-containing Complex Organic Molecules toward IRAS 16293–2422B]]**\\ | **[[https://doi.org/10.1051/0004-6361/201731667|The ALMA-PILS Survey: Isotopic Composition of Oxygen-containing Complex Organic Molecules toward IRAS 16293–2422B]]**\\ |
| //Astron. Astrophys.// **620**, Art. No. A170 (2018).\\ | //Astron. Astrophys.// **620**, Art. No. A170 (2018).\\ |
| The results were obtained in the course of a line survey of the solar-type protostellar binary IRAS 16293–2422 with ALMA covering the frequency range 329.1–362.9 GHz. The authors only investigated source B. They detected for the first time both <sup>13</sup>C isotopomers as well as the mono-deuterated isotopolog. The D/H ratio per H atom is about 0.02 (the HDCCO/H<sub>2</sub>CCO ratio is about 0.04). Many lines of the main isotopic species were optically thick; the local ISM <sup>12</sup>C/<sup>13</sup>C ratio of 68 was assumed. The <sup>18</sup>O and the doubly deuterated isotopologs were near the detection limit and not identified with certainty. Ketene is among the molecules with colder rotational temperatures of around 125 K in that hot corino. | The results were obtained in the course of a line survey of the solar-type protostellar binary IRAS 16293–2422 with ALMA covering the frequency range 329.1–362.9 GHz. The authors only investigated source B. They detected for the first time both <sup>13</sup>C isotopomers as well as the mono-deuterated isotopolog. The D/H ratio per H atom is about 0.02 (the HDCCO/H<sub>2</sub>CCO ratio is about 0.04). Many lines of the main isotopic species were optically thick; the local ISM <sup>12</sup>C/<sup>13</sup>C ratio of 68 was assumed. The <sup>18</sup>O and the doubly deuterated isotopologs were near the detection limit and not identified with certainty. Ketene is among the molecules with colder rotational temperatures of around 125 K in that hot corino. |
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| Contributor(s): H. S. P. Müller; 06, 2006; 03, 2012; 01, 2019 | Contributor(s): H. S. P. Müller; 06, 2006; 03, 2012; 01, 2019 |
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