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Quasar feedback is suspected to play a key role in the evolution of massivegalaxies, by removing or reheating gas in quasar host galaxies and thuslimiting the amount of star formation. In this paper we continue ourinvestigation of quasar-driven winds on galaxy-wide scales. We conduct GeminiIntegral Field Unit spectroscopy of a sample of luminous unobscured (type 1)quasars, to determine the morphology and kinematics of ionized gas around theseobjects, predominantly via observations of the [O III]5007 emission line. Wefind that ionized gas nebulae extend out to ~13 kpc from the quasar, that theyare smooth and round, and that their kinematics are inconsistent with gas indynamical equilibrium with the host galaxy. The observed morphological andkinematic properties are strikingly similar to those of ionized gas aroundobscured (type 2) quasars with matched [O III] luminosity, with marginalevidence that nebulae around unobscured quasars are slightly more compact.Therefore in samples of obscured and unobscured quasars carefully matched in [OIII] luminosity we find support for the standard geometry-based unificationmodel of active galactic nuclei, in that the intrinsic properties of quasars,of their hosts and of their ionized gas appear to be very similar. Given theapparent ubiquity of extended ionized regions, we are forced to conclude thateither the quasar is at least partially illuminating pre-existing gas or thatboth samples of quasars are seen during advanced stages of quasar feedback. Inthe latter case, we may be biased by our [O III]-based selection againstquasars in the early "blow-out" phase, for example due to dust obscuration.

Similarity of ionized gas nebulae around unobscured and obscured quasars