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| molecules:extragalactic:ch-plus_extragalactic [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:extragalactic:ch-plus_extragalactic [2019/10/22 13:28] (current) – mueller |
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| P. Magain and D. Gillet\\ | P. Magain and D. Gillet\\ |
| reported on the\\ | reported on the\\ |
| **[[http://adsabs.harvard.edu/abs/1987A%26A...184L...5M|Detection of interstellar CH and CH<sup>+</sup> towards SN 1987a]]**,\\ | **[[https://ui.adsabs.harvard.edu/abs/1987A%26A...184L...5M|Detection of interstellar CH and CH<sup>+</sup> towards SN 1987a]]**,\\ |
| //Astron. Astrophys.// **184**, L5–L6 (1987).\\ | //Astron. Astrophys.// **184**, L5–L6 (1987).\\ |
| Lowest-//J// optical transitions were observed in absorption with the ESO 1.4 m telescope at La Silla. The velocities correspond to interstellar matter within the Large Magellanic Cloud. | Lowest-//J// optical transitions were observed in absorption with the ESO 1.4 m telescope at La Silla. The velocities correspond to interstellar matter within the Large Magellanic Cloud. |
| E. Falgarone, M. A. Zwaan, B. Godard, E. Bergin, R. J. Ivison, P. M. Andreani, F. Bournaud, R. S. Bussmann, D. Elbaz, A. Omont, I. Oteo, and F. Walter\\ | E. Falgarone, M. A. Zwaan, B. Godard, E. Bergin, R. J. Ivison, P. M. Andreani, F. Bournaud, R. S. Bussmann, D. Elbaz, A. Omont, I. Oteo, and F. Walter\\ |
| reported on the\\ | reported on the\\ |
| **[[http://dx.doi.org/10.1038/nature23298|Large Turbulent Reservoirs of Cold Molecular Gas around High-redshift Starburst Galaxies]]**,\\ | **[[https://doi.org/10.1038/nature23298|Large Turbulent Reservoirs of Cold Molecular Gas around High-redshift Starburst Galaxies]]**,\\ |
| //Nature// **548**, (1987) 430–433.\\ | //Nature// **548**, (1987) 430–433.\\ |
| The //J// = 1 – 0 transitions of CH<sup>+</sup> was detected in emission and/or absorption toward six galaxies at red-shifts of 2.0 to 2.6 with ALMA. | The //J// = 1 – 0 transitions of CH<sup>+</sup> was detected in emission and/or absorption toward six galaxies at red-shifts of 2.0 to 2.6 with ALMA. |
| S. Muller, H. S. P. Müller, J. H. Black, M. Gérin, F. Combes, S. Curran, E. Falgarone, M. Guélin, C. Henkel, S. Martín, K. M. Menten, E. Roueff, S. Aalto, A. Beelen, T. Wiklind, and M. A. Zwaan,\\ | S. Muller, H. S. P. Müller, J. H. Black, M. Gérin, F. Combes, S. Curran, E. Falgarone, M. Guélin, C. Henkel, S. Martín, K. M. Menten, E. Roueff, S. Aalto, A. Beelen, T. Wiklind, and M. A. Zwaan,\\ |
| reported on the\\ | reported on the\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201731405|Detection of CH<sup>+</sup>, SH<sup>+</sup>, and Their <sup>13</sup>C- and <sup>34</sup>S-isotopologues toward PKS 1830–211]]**\\ | **[[https://doi.org/10.1051/0004-6361/201731405|Detection of CH<sup>+</sup>, SH<sup>+</sup>, and Their <sup>13</sup>C- and <sup>34</sup>S-isotopologues toward PKS 1830–211]]**\\ |
| //Astron. Astrophys.// **606**, (2017) Art. No. A109.\\ | //Astron. Astrophys.// **606**, (2017) Art. No. A109.\\ |
| The //J// = 1 – 0 transitions of CH<sup>+</sup> and <sup>13</sup>CH<sup>+</sup> were observed with ALMA redshifted from about 835.1 and 830.2 GHz to about 442.85 and 440.24 GHz. The molecular cations were detected toward both SW and NE images. The intensity ratio appears to suggest the molecular cation resides in gas with at least slightly higher molecular fraction than H<sub>2</sub>O<sup>+</sup> or H<sub>2</sub>Cl<sup>+</sup>. The <sup>12</sup>C/<sup>13</sup>C isotopic ratio is about 100, possibly higher. This is, to the best of our knowledge, the first account on extragalactic <sup>13</sup>CH<sup>+</sup>. | The //J// = 1 – 0 transitions of CH<sup>+</sup> and <sup>13</sup>CH<sup>+</sup> were observed with ALMA redshifted from about 835.1 and 830.2 GHz to about 442.85 and 440.24 GHz. The molecular cations were detected toward both SW and NE images. The intensity ratio appears to suggest the molecular cation resides in gas with at least slightly higher molecular fraction than H<sub>2</sub>O<sup>+</sup> or H<sub>2</sub>Cl<sup>+</sup>. The <sup>12</sup>C/<sup>13</sup>C isotopic ratio is about 100, possibly higher. This is, to the best of our knowledge, the first account on extragalactic <sup>13</sup>CH<sup>+</sup>. |
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| Contributor(s): H. S. P. Müller; 11, 2017 | Contributor(s): H. S. P. Müller; 11, 2017 |
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