Observational Signatures of Galactic Winds Powered by Active Galactic
  Nuclei
  We predict the observational signatures of galaxy scale outflows powered by
active galactic nuclei (AGN). Most of the emission is produced by the forward
shock driven into the ambient interstellar medium (ISM) rather than by the
reverse shock. AGN powered galactic winds with energetics suggested by
phenomenological feedback arguments should produce spatially extended 1-10 keV
X-ray emission of 10^(41-44) erg/s, significantly in excess of the spatially
extended X-ray emission associated with normal star forming galaxies. The
presence of such emission is a direct test of whether AGN outflows
significantly interact with the ISM of their host galaxy. We further show that
even radio quiet quasars should have a radio luminosity comparable to or in
excess of the far infrared-radio correlation of normal star forming galaxies.
This radio emission directly constrains the total kinetic energy flux in
AGN-powered galactic winds. Radio emission from AGN wind shocks can also
explain the recently highlighted correlations between radio luminosity and the
kinematics of AGN narrow-line regions in radio quiet quasars.
