Feedback from Mass Outflows in Nearby Active Galactic Nuclei I. UV and
  X-ray Absorbers
  We present an investigation into the impact of feedback from outflowing UV
and X-ray absorbers in nearby z < 0.04 AGN. From studies of the kinematics,
physical conditions, and variability of the absorbers in the literature, we
calculate the possible ranges in total mass outflow rate and kinetic luminosity
for each AGN, summed over all of its absorbers. These calculations make use of
values (or limits) for the radial locations of the absorbers determined from
variability, excited-state absorption, and other considerations. From a sample
of 10 Seyfert 1 galaxies with detailed photoionization models for their
absorbers, we find that 7 have sufficient constraints on the absorber locations
to determine feedback parameters. For the low-luminosity AGN NGC 4395, these
values are low, although we do not have sufficient constraints on the X-ray
absorbers to make definitive conclusions. At least 5 of the 6 Seyfert 1s with
moderate bolometric luminosities have mass outflow rates that are 10 - 1000
times the mass accretion rates needed to generate their observed luminosities,
indicating that most of the mass outflow originates from outside the inner
accretion disk. Three of these (NGC 4051, NGC 3516, and NGC 3783) have kinetic
luminosities in the range 0.5 to 5% bolometric, which is the range typically
required by feedback models for efficient self-regulation of black-hole and
galactic bulge growth. At least 2 of the other 3 (NGC 5548, NGC 4151, and NGC
7469) have kinetic luminosities > 0.1% bolometric, although these values may
increase if radial locations can be determined for more of the absorbers. We
conclude that the outflowing UV and X-ray absorbers in moderate-luminosity AGN
have the potential to deliver significant feedback to their environments.
