tokens: arise from a broad range of temperatures at a given density (spanning up to ∼0.5 − 1 dex) as they are coming to the end of the rapid cooling phase, and they have not yet reached thermal equilibrium. Emission from molecules and low-ionization states such as [O i ] and [C ii ] that trace the 100 phase also cover a broad range of temperatures at each density, rather than simply tracking the thermal equilibrium temperature as a function of density. This is likely due to turbulent shock heating. We find that, in our simulations, the dense () gas clouds that condense within the outflowing shell after it cools typically have velocity dispersions up to a few tens of km s −1 . The shocks resulting from this turbulence can heat the gas up to a few thousand K. The photoionization models also assume that the ions and molecules are in chemical equilibrium. To test this assumption in our simulations, we computed the equilibrium abundances of each gas particle at fixed density and temperature, and then repeated the radiative transfer calculations using the equilibrium abundances. The most notable difference is in the [O iii ] line, which is ≈7 − 8 times higher when we set the abundances to equilibrium than when we use non-equilibrium abundances. Other emission lines also show modest deviations when we assume equilibrium abundances, in particular [Ne v ] (up to 80 per cent), [N ii ] (up to 62 per cent), [O iv ] (up to 60 per cent), [N iii ] (up to 44 per cent), [S iii ] (up to 39 per cent), [N ii ] (up to 35 per cent), H (up to 31 per cent), H (up to 29 per cent), and CO (up to 26 per cent). The remaining lines differ by 20 per cent when we use equilibrium abundances. 3.3 Comparison with observations We now compare the predictions from our simulations to observations of outflows in AGN host galaxies. Fig. 7 compares the line luminosity ( L line ) divided by the bolometric AGN luminosity ( L AGN ) plotted against L AGN for a subset of the infrared lines (the full sample can be found in Appendix A ). We divide by L AGN on the y -axis to reduce the dynamic range; a simple linear scaling between L line and L AGN would thus manifest itself as a horizontal trend in these plots. For the simulations ( RFG18 ; grey symbols), our radiative transfer calculations include only one quadrant of the spherical outflow (see Section 2.2 ). We therefore multiply the resulting luminosities by four to obtain the luminosity of the whole outflow. Figure 7. Line luminosity ( L line ) divided by bolometric AGN luminosity ( L AGN ) plotted against L AGN . Our simulations from RFG18 are shown by the grey symbols. In the left column, showing a subset of mid-infrared (IR) lines, we compare to the observations in Veilleux et al. ( 2009 ; V09 ; squares), which we divide according to the AGN classification as PG QSO, ULIRG Sy1, ULIRG Sy2, and ULIRG LINER, as indicated by the colour. In the right column, showing a subset of far-IR lines, we compare to the observations in Herrera-Camus et al.
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