Constraining the dynamical importance of hot gas and radiation pressure in quasar outflows using emission line ratios

Understand

Quasar feedback models often predict an expanding hot gas bubble which drives a galaxy-scale outflow.

• In many circumstances this hot gas radiates inefficiently and is therefore difficult to observe directly.
• We present an indirect method to detect the presence of a hot bubble using hydrostatic photoionization calculations of the cold (~10^4 K) line-emitting gas.
• We compare our calculations with observations of the broad line region, the inner face of the torus, the narrow line region (NLR), and the extended NLR, and thus constrain the hot gas pressure at distances 0.1 pc -- 10 kpc from the center.