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| molecules:extragalactic:h2o-plus_extragalactic [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:extragalactic:h2o-plus_extragalactic [2019/10/22 13:49] (current) – mueller |
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| The first substantiated detection of Extragalactic H<sub>2</sub>O<sup>+</sup> involves the //J// = 1.5 – 0.5 fine structure component of the 1<sub>11</sub> – 0<sub>00</sub> transition of //ortho//-oxidaniumyl near 1115 GHz, which has been detected in absorption with the HIFI instrument on board of the //Herschel// satellite toward M 82:\\ | The first substantiated detection of Extragalactic H<sub>2</sub>O<sup>+</sup> involves the //J// = 1.5 – 0.5 fine structure component of the 1<sub>11</sub> – 0<sub>00</sub> transition of //ortho//-oxidaniumyl near 1115 GHz, which has been detected in absorption with the HIFI instrument on board of the //Herschel// satellite toward M 82:\\ |
| A. Weiß, M. A. Requena-Torres, R. Güsten, et al.\\ | A. Weiß, M. A. Requena-Torres, R. Güsten, et al.\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201015078|HIFI Spectroscopy of Low-Level Water Transitions in M 82]]**\\ | **[[https://doi.org/10.1051/0004-6361/201015078|HIFI Spectroscopy of Low-Level Water Transitions in M 82]]**\\ |
| //Astron. Astrophys.// **521**, (2010) Art. No. L1.\\ | //Astron. Astrophys.// **521**, (2010) Art. No. L1.\\ |
| As may be interpreted from the title, H<sub>2</sub>O<sup>+</sup> was observed by accident because of the proximity of that fine structure component to the 1<sub>11</sub> – 0<sub>00</sub> transition of //para//-H<sub>2</sub>O. However, a detailed analysis of this feature has been presented. | As may be interpreted from the title, H<sub>2</sub>O<sup>+</sup> was observed by accident because of the proximity of that fine structure component to the 1<sub>11</sub> – 0<sub>00</sub> transition of //para//-H<sub>2</sub>O. However, a detailed analysis of this feature has been presented. |
| It is worthwhile mentioning that only the weaker //J// = 0.5 – 0.5 fine structure component of the 1<sub>11</sub> – 0<sub>00</sub> transition was reportedly detected with SPIRE///Herschel// in **emission** toward the ultraluminous infrared galaxy Mrk 231:\\ | It is worthwhile mentioning that only the weaker //J// = 0.5 – 0.5 fine structure component of the 1<sub>11</sub> – 0<sub>00</sub> transition was reportedly detected with SPIRE///Herschel// in **emission** toward the ultraluminous infrared galaxy Mrk 231:\\ |
| P. P. van der Werf, K. G. Isaak, R. Meijerink, et al.,\\ | P. P. van der Werf, K. G. Isaak, R. Meijerink, et al.,\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201014682|Black Hole Accretion and Star-Formation as Drivers of Gas Excitation and Chemistry in Markarian 231]]**\\ | **[[https://doi.org/10.1051/0004-6361/201014682|Black Hole Accretion and Star-Formation as Drivers of Gas Excitation and Chemistry in Markarian 231]]**\\ |
| //Astron. Astrophys.// **518**, (2010) Art. No. L42.\\ | //Astron. Astrophys.// **518**, (2010) Art. No. L42.\\ |
| The account is somewhat sketchy, the report should therefore be viewed with some caution. On the other hand, the title seems to indicate why the line, provided the identification is correct, is seen in emission, in contrast to all presently known Galactic observations and also in contrast to the Extragalactic detection mentioned above. | The account is somewhat sketchy, the report should therefore be viewed with some caution. On the other hand, the title seems to indicate why the line, provided the identification is correct, is seen in emission, in contrast to all presently known Galactic observations and also in contrast to the Extragalactic detection mentioned above. |
| E. González-Alfons1 , J. Fischer, S. Bruderer, et al.\\ | E. González-Alfons1 , J. Fischer, S. Bruderer, et al.\\ |
| reported on\\ | reported on\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201220466|Excited OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup>, and H<sub>3</sub>O<sup>+</sup> in NGC 4418 and Arp 220]]**,\\ | **[[https://doi.org/10.1051/0004-6361/201220466|Excited OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup>, and H<sub>3</sub>O<sup>+</sup> in NGC 4418 and Arp 220]]**,\\ |
| //Astron. Astrophys.// **550**, Art. No. A25 (2013);\\ | //Astron. Astrophys.// **550**, Art. No. A25 (2013);\\ |
| using PACS on board of the //Herschel// satellite. Transitions 4<sub>04</sub> – 3<sub>13</sub> and 3<sub>22</sub> – 2<sub>11</sub> with upper state energies of about 300 K were detected in both sources with no or negligible overlap. Additional transitions with //E//<sub>up</sub> beyond 400 K have also been observed, but are at least partially overlapped. | using PACS on board of the //Herschel// satellite. Transitions 4<sub>04</sub> – 3<sub>13</sub> and 3<sub>22</sub> – 2<sub>11</sub> with upper state energies of about 300 K were detected in both sources with no or negligible overlap. Additional transitions with //E//<sub>up</sub> beyond 400 K have also been observed, but are at least partially overlapped. |
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| Contributor(s): H. S. P. Müller; 10, 2010; 04, 2013. | Contributor(s): H. S. P. Müller; 10, 2010; 04, 2013. |
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