The Close AGN Reference Survey (CARS): Locating the [O III] wing
  component in luminous local Type 1 AGN
  [Abridged]The strong asymmetry in the optical [O III]$\lambda$5007 emission
line is one of the best signatures of AGN-driven warm (~10$^4$ K) ionized gas
outflows on host galaxy scales. While large spectroscopic surveys like SDSS
have characterized the kinematics of [O III] for large samples of AGN,
estimating the associated energetics requires spatially resolving these
outflows with, for example, IFU studies. As part of CARS we obtained
spatially-resolved IFU spectroscopy for a representative sample of 39 luminous
type 1 AGN at 0.01<z<0.06 with MUSE and VIMOS IFUs at the VLT to infer the
spatial location of the ionized gas outflows. We compare the light
distributions of the [O III] wing to that of the H$\beta$ broad emission line
region, a classical point source (PSF). We then use the PSF to distinguish
between the unresolved and resolved [O III] wing emission. We further determine
its location using spectro-astrometry for the point-like sources. The [O III]
wing is spatially unresolved in 23 out of the 36 AGN with >80 % of the flux
associated with a point-like source. We measure <100 pc offsets in the spatial
location of the outflow from the AGN nucleus using the spectro-astrometry
technique for these sources. For the other 13 AGN, the [O III] wing emission is
resolved and possibly extended on kpc scale. We conclude that [O III] wing
emission can be compact or extended in an unbiased luminous AGN sample, where
both cases are likely to appear. Electron density in the compact [O III] wing
regions (median $n_e$~1900 cm$^{-3}$) is nearly a magnitude higher than in the
extended ones (median $n_e$~500 cm$^{-3}$). The presence of spatially extended
and compact [O III] wing emission is unrelated to the AGN bolometric luminosity
and to inclination effects, which means other features such as time delays, or
mechanical feedback/radio jets may shape the ionized gas outflow properties.
