Direct evidence of AGN-feedback: a post starburst galaxy stripped of its
  gas by AGN-driven winds
  Post starburst E+A galaxies show indications of a powerful starburst that was
quenched abruptly. Their disturbed, bulge-dominated morphologies suggest that
they are merger remnants. The more massive E+A galaxies are suggested to be
quenched by AGN feedback, yet little is known about AGN-driven winds in this
short-lived phase. We present spatially-resolved IFU spectroscopy by the Keck
Cosmic Web Imager of SDSS J003443.68+251020.9, at z=0.118. The system consists
of two galaxies, the larger of which is a post starburst E+A galaxy hosting an
AGN. Our modelling suggests a 400 Myrs starburst, with a peak star formation
rate of 120 Msun/yr. The observations reveal stationary and outflowing gas,
photoionized by the central AGN. We detect gas outflows to a distance of 17 kpc
from the central galaxy, far beyond the region of the stars (about 3 kpc),
inside a conic structure with an opening angle of 70 degrees. We construct
self-consistent photoionization and dynamical models for the different gas
components and show that the gas outside the galaxy forms a continuous flow,
with a mass outflow rate of about 24 Msun/yr. The gas mass in the flow, roughly
$10^9$ Msun, is larger than the total gas mass within the galaxy, some of which
is outflowing too. The continuity of the flow puts a lower limit of 60 Myrs on
the duration of the AGN feedback. Such AGN are capable of removing, in a single
episode, most of the gas from their host galaxies and expelling enriched
material into the surrounding CGM.
