Fueling AGN-I: How the Global Characteristics of the Central Kiloparsec
  of Seyferts differ from Quiescent Galaxies
  In a matched sample of Seyfert and quiescent galaxies we simultaneously probe
the stellar and molecular gas kinematics from 1 kpc down to 50 pc with the aim
of identifying the dynamical processes dictating black hole accretion rates.
This first paper compares the global characteristics of a sample of ten
galaxies. We find several differences within a radius of 500 pc that are
correlated with Active Galactic Nucleus (AGN) activity. The Seyferts have: (1)
a more centrally concentrated nuclear stellar surface brightness with lower
stellar luminosities beyond a radius of 100 pc, (2) a lower stellar velocity
dispersion within a radius of 200 pc, (3) elevated H2 luminosity out to a
radius of at least 250 pc, and (4) more centrally concentrated H2 surface
brightness profiles. These observed differences can be interpreted as evidence
for Seyfert galaxies having a dynamically cold (in comparison to the bulge)
nuclear structure composed of a significant gas reservoir and a relatively
young stellar population. This structure is undetected (and possibly does not
exist) in quiescent galaxies. The presence of such a nuclear structure in
Seyfert galaxies provides evidence for inflow of the surrounding interstellar
medium since the nuclear stellar population requires a supply of gas from which
to form. The fueling of a Seyfert AGN is thus associated with the formation of
a dynamically cold component of gas and stars on scales of hundreds of parsecs.
