The first substantiated detection of Extragalactic H₂O⁺ involves the J = 1.5 – 0.5 fine structure component of the 1₁₁ – 0₀₀ 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.
HIFI Spectroscopy of Low-Level Water Transitions in M 82
Astron. Astrophys. 521, (2010) Art. No. L1.
As may be interpreted from the title, H₂O⁺ was observed by accident because of the proximity of that fine structure component to the 1₁₁ – 0₀₀ transition of para-H₂O. 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 1₁₁ – 0₀₀ 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.,
Black Hole Accretion and Star-Formation as Drivers of Gas Excitation and Chemistry in Markarian 231
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.

E. González-Alfons1 , J. Fischer, S. Bruderer, et al.
reported on
Excited OH⁺, H₂O⁺, and H₃O⁺ in NGC 4418 and Arp 220,
Astron. Astrophys. 550, Art. No. A25 (2013);
using PACS on board of the Herschel satellite. Transitions 4₀₄ – 3₁₃ and 3₂₂ – 2₁₁ with upper state energies of about 300 K were detected in both sources with no or negligible overlap. Additional transitions with E_up 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.

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