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| molecules:extragalactic:oh-plus_extragalactic [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:extragalactic:oh-plus_extragalactic [2019/10/22 13:33] (current) – mueller |
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| The first firm detection of of oxidaniumylidene or hydroxylium, OH<sup>+</sup>, was reported by\\ | The first firm detection of of oxidaniumylidene or hydroxylium, OH<sup>+</sup>, was reported by\\ |
| 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, no rest frequencies are given and no references for these. An abundance has been derived, but no details are given. Only a broad overview spectrum is shown. Thus, one may be inclined to view this detection with some caution. On the other hand, all three fine structure components of the //N// = 1 – 0 transition seem to have been observed in emission toward the ultraluminous infrared galaxy Mrk 231with correct relative intensities employing the SPIRE instrument on board of the //Herschel// satellite. Given the ubiquity and high abundance of OH<sup>+</sup> in Galactic sources, the identification is probably correct. | The account is somewhat sketchy, no rest frequencies are given and no references for these. An abundance has been derived, but no details are given. Only a broad overview spectrum is shown. Thus, one may be inclined to view this detection with some caution. On the other hand, all three fine structure components of the //N// = 1 – 0 transition seem to have been observed in emission toward the ultraluminous infrared galaxy Mrk 231with correct relative intensities employing the SPIRE instrument on board of the //Herschel// satellite. Given the ubiquity and high abundance of OH<sup>+</sup> in Galactic sources, the identification is probably correct. |
| There have been prior reports on the tentative detection of OH<sup>+</sup>:\\ | There have been prior reports on the tentative detection of OH<sup>+</sup>:\\ |
| E. González-Alfonso, H, A. Smith, J. Fischer, and J. Cernicharo,\\ | E. González-Alfonso, H, A. Smith, J. Fischer, and J. Cernicharo,\\ |
| **[[http://dx.doi.org/10.1086/422868|The Far-Infrared Spectrum of Arp 220]]**\\ | **[[https://doi.org/10.1086/422868|The Far-Infrared Spectrum of Arp 220]]**\\ |
| //Astrophys. J.// **613**, (2004) 247–261\\ | //Astrophys. J.// **613**, (2004) 247–261\\ |
| discuss the possibility that absorption features of NH observed with //ISO// LWS at 100 and 150 μm may be affected by the //N// = 3 – 2 and 2 – 1 transitions, respectively, of OH<sup>+</sup>. However, they refrain from suggesting that there is strong evidence for OH<sup>+</sup> to be present.\\ | discuss the possibility that absorption features of NH observed with //ISO// LWS at 100 and 150 μm may be affected by the //N// = 3 – 2 and 2 – 1 transitions, respectively, of OH<sup>+</sup>. However, they refrain from suggesting that there is strong evidence for OH<sup>+</sup> to be present.\\ |
| E. González-Alfonso, H. A. Smith, M. L. N. Ashby, J. Fischer, L. Spinoglio, and T. W. Grundy,\\ | E. González-Alfonso, H. A. Smith, M. L. N. Ashby, J. Fischer, L. Spinoglio, and T. W. Grundy,\\ |
| **[[http://dx.doi.org/10.1086/527292|High-excitation OH and H<sub>2</sub>O Lines in Markarian 231: The Molecular Signatures of Compact Far-infrared Continuum Sources]]**\\ | **[[https://doi.org/10.1086/527292|High-excitation OH and H<sub>2</sub>O Lines in Markarian 231: The Molecular Signatures of Compact Far-infrared Continuum Sources]]**\\ |
| //Astrophys. J.// **675**, (2008) 303–315\\ | //Astrophys. J.// **675**, (2008) 303–315\\ |
| assigned two barely detected (about 2.5 σ) absorption features detected near 150 μm with //ISO// LWS to the two strongest fine structure components of the //N// = 2 – 1 transition.\\ | assigned two barely detected (about 2.5 σ) absorption features detected near 150 μm with //ISO// LWS to the two strongest fine structure components of the //N// = 2 – 1 transition.\\ |
| E. González-Alfonso, J. Fischer, S. Bruderer, et al.\\ | E. González-Alfonso, 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 up to //N// = 4 – 3 with upper state energy of almost 500 K were detected in both sources. There may be even evidence for the 5 – 4 components (//E//<sub>up</sub> ≈ 700 K) in NGC 4418, but the intensities do not fit the model. | using PACS on board of the //Herschel// satellite. Transitions up to //N// = 4 – 3 with upper state energy of almost 500 K were detected in both sources. There may be even evidence for the 5 – 4 components (//E//<sub>up</sub> ≈ 700 K) in NGC 4418, but the intensities do not fit the model. |
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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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