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tokens: [CII] redshift ( Carilli et al. 2013 ). The rest-frame frequencies of HF J = 1–0 and H 2 O (2 20 –2 11 ) are 1232.476 and 1228.789 GHz respectively. In contrast, the line width of the H 2 O (2 20 –2 11 ) in the QSO is, within the uncertainties, exactly the same as for the other lines. Neither the QSO or the SMG show clear evidence for an outflow in the H 2 O line, although there is a possible excess in the line profile of the QSO seen ∼400 km s −1 blueward of the systemic H 2 O redshift, consistent with the velocities of the weak [CII] outflow ( Carilli et al. 2013 ). 4. Discussion 4.1. HF: Molecular gas irradiated by AGN and young stars The detection of HF emission in the QSO is unusual. In most of the sources observed thus far, the HF J = 1–0 line is observed as an absorption line with little or no emission ( van der Werf et al. 2010 ). Only a handful of sources are known to have HF purely in emission, without any obvious associated absorption. These sources are the Orion Bar ( van der Tak et al. 2012 ; Kavak et al. 2019 ), Mrk 231 ( van der Werf et al. 2010 ), and a few nearby galaxies ( Pereira-Santaella et al. 2013 ; Lu et al. 2017b ). To increase the number of galaxies observed with HF in emission, we extracted the HF emission line fluxes from local galaxies observed with Herschel in the sample of Yang et al. (2013) , which all host AGN. We find that the galaxies that host AGN and the QSO in BR 1202-0725 have an approximately constant ratio of L HF / L IR irrespective of L IR (Fig. 3 ). We note, however, that the exact slope of the relation only considering the local AGN and QSO is dependent on the far-infrared luminosity used. Other estimates of the infrared luminosity of the QSO in the literature would lower L IR / L HF (cf. Salomé et al. 2012 ; Wagg et al. 2014 ; Lu et al. 2017a ). Fig. 3. Relationship between the infrared luminosity and the ratio of the HF luminosity and infrared luminosity of BR 1202-0725, a sample of local AGN ( Yang et al. 2013 ), and the Orion Bar ( Salgado et al. 2016 ; Nagy et al. 2017 ). All sources are labeled. We show a least-squares fit to the local AGN, QSO, and the Orion Bar (black line with the dotted line extension to the Orion Bar), which implies the ratio is constant. We note that fitting the AGN and QSO only yields a similar fit but with a slightly steeper slope. For comparison, we show the ratio L HF / L IR for the entire IR luminosity of the Orion Bar and the luminosity if only 2% of the total IR luminosity is within the Herschel beam used to measure the HF flux (see text for details). The Orion Bar is the only known galactic source or sight-line where HF appears purely in emission (although we note that the absorption of HF and the nearby H 2 O (2 20 –2 11 ) could mask any emission in other galactic and extra-galactic sources; see e.g., Monje et al. 2014 ; Neufeld et al. 2010 ; Sonnentrucker et al. 2015 ). If we compare L HF / L IR and L IR for the Orion Bar ( Salgado et al. 2016 ; Nagy et al.