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| molecules:ism:hoco-plus [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:hoco-plus [2019/10/22 16:42] (current) – mueller |
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| Oxohydroxymethylium, aka protonated carbon dioxide, HOCO<sup>+</sup>, was among the molecules that had been identified in space (toward the star-forming region Sgr B2(OH)) before they had been characterized in the laboratory. Three transitions //J//+1<sub>0,//J//+1</sub> – //J//<sub>0,//J//</sub> with //J// = 3 – 5 were reported by\\ | Oxohydroxymethylium, aka protonated carbon dioxide, HOCO<sup>+</sup>, was among the molecules that had been identified in space (toward the star-forming region Sgr B2(OH)) before they had been characterized in the laboratory. Three transitions //J//+1<sub>0,//J//+1</sub> – //J//<sub>0,//J//</sub> with //J// = 3 – 5 were reported by\\ |
| P. Thaddeus, M. Guélin, and R. A. Linke,\\ | P. Thaddeus, M. Guélin, and R. A. Linke,\\ |
| **[[http://adsabs.harvard.edu/abs/1981ApJ...246L..41T|Three new 'nonterrestrial' molecules]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1981ApJ...246L..41T|Three new 'nonterrestrial' molecules]]**\\ |
| //Astrophys. J.// **246**, L41–L45 (1981). HOCO<sup>+</sup> or HOCN were seen as possible carriers of these lines. Subsequent laboratory spectroscopic investigations proved the carrier to be HOCO<sup>+</sup>:\\ | //Astrophys. J.// **246**, L41–L45 (1981). HOCO<sup>+</sup> or HOCN were seen as possible carriers of these lines. Subsequent laboratory spectroscopic investigations proved the carrier to be HOCO<sup>+</sup>:\\ |
| M. Bogey, C. Demuynck, and J. L. Destombes,\\ | M. Bogey, C. Demuynck, and J. L. Destombes,\\ |
| **[[http://adsabs.harvard.edu/abs/1984A%26A...138L..11B|Laboratory Detection of the Protonated Carbon Dioxide by Submillimeter Wave Spectroscopy]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1984A%26A...138L..11B|Laboratory Detection of the Protonated Carbon Dioxide by Submillimeter Wave Spectroscopy]]**\\ |
| //Astron. Astrophys.// **138**, L11–L12 (1984). | //Astron. Astrophys.// **138**, L11–L12 (1984). |
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| The molecular ion was also detected toward Sgr A:\\ | The molecular ion was also detected toward Sgr A:\\ |
| Y. C. Mihn, W. M. Irvine, and L. M. Ziurys,\\ | Y. C. Mihn, W. M. Irvine, and L. M. Ziurys,\\ |
| **[[http://adsabs.harvard.edu/abs/1988ApJ...334..175M|Observations of Interstellar HOCO<sup>+</sup> – Abundance Enhancements toward the Galactic Center]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1988ApJ...334..175M|Observations of Interstellar HOCO<sup>+</sup> – Abundance Enhancements toward the Galactic Center]]**\\ |
| //Astrophys. J.// **334**, 175–181 (1988). | //Astrophys. J.// **334**, 175–181 (1988). |
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| It is also present in dark clouds, such as TMC-1 and L183, as well as in two out of three translucent clouds (CB 17 and CB 228):\\ | It is also present in dark clouds, such as TMC-1 and L183, as well as in two out of three translucent clouds (CB 17 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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| More recently, it was shown that the ion is not confined to massive star-forming regions:\\ | More recently, it was shown that the ion is not confined to massive star-forming regions:\\ |
| N. Sakai, T. Sakai, Y. Aikawa, and S. Yamamoto,\\ | N. Sakai, T. Sakai, Y. Aikawa, and S. Yamamoto,\\ |
| **[[http://dx.doi.org/10.1086/533463|Detection of HCO<sub>2</sub><sup>+</sup> toward the Low-Mass Protostar IRAS 04368+2557 in L1527]]**\\ | **[[https://doi.org/10.1086/533463|Detection of HCO<sub>2</sub><sup>+</sup> toward the Low-Mass Protostar IRAS 04368+2557 in L1527]]**\\ |
| //Astrophys. J.// **675**, L89–L92 (2008). | //Astrophys. J.// **675**, L89–L92 (2008). |
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| C. Vastel, C. Ceccarelli, B. Lefloch, and R. Bachiller,\\ | C. Vastel, C. Ceccarelli, B. Lefloch, and R. Bachiller,\\ |
| reported on the\\ | reported on the\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201628427|Abundance of HOCO<sup>+</sup> and CO<sub>2</sub> in the Outer Layers of the L1544 Prestellar Core]]**\\ | **[[https://doi.org/10.1051/0004-6361/201628427|Abundance of HOCO<sup>+</sup> and CO<sub>2</sub> in the Outer Layers of the L1544 Prestellar Core]]**\\ |
| //Astron. Astrophys.// **691**, Art. No. L2 (2016).\\ | //Astron. Astrophys.// **691**, Art. No. L2 (2016).\\ |
| They report the detection of the 5<sub>05</sub> – 4<sub>04</sub> transition of DOCO<sup>+</sup> near 100.4 GHz in emission with the IRAM 30 m telescope. They viewed the detection as somewhat tentative because of issues in the laboratory rest frequencies which have been resolved in the meantime.\\ | They report the detection of the 5<sub>05</sub> – 4<sub>04</sub> transition of DOCO<sup>+</sup> near 100.4 GHz in emission with the IRAM 30 m telescope. They viewed the detection as somewhat tentative because of issues in the laboratory rest frequencies which have been resolved in the meantime.\\ |
| A. Fuente, J. Cernicharo, E. Roueff, M. Gerin, J. Pety, N. Marcelino, R. Bachiller, B. Lefloch, O. Roncero, and A. Aguado,\\ | A. Fuente, J. Cernicharo, E. Roueff, M. Gerin, J. Pety, N. Marcelino, R. Bachiller, B. Lefloch, O. Roncero, and A. Aguado,\\ |
| identified the same transition in B1b in the report on the\\ | identified the same transition in B1b in the report on the\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201628285|Ionization Fraction and the Enhanced Sulfur Chemistry in Barnard 1]]**\\ | **[[https://doi.org/10.1051/0004-6361/201628285|Ionization Fraction and the Enhanced Sulfur Chemistry in Barnard 1]]**\\ |
| //Astron. Astrophys.//****, in press (2016),\\ | //Astron. Astrophys.//****, in press (2016),\\ |
| using the same telescope in an extensive molecular line survey. | using the same telescope in an extensive molecular line survey. |
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| Contributor(s): H. S. P. Müller; 03, 2008; 03, 2012; 08, 2016 | Contributor(s): H. S. P. Müller; 03, 2008; 03, 2012; 08, 2016 |
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