An outflow in the Seyfert ESO 362-G18 revealed by Gemini-GMOS/IFU
  Observations
  We present two-dimensional stellar and gaseous kinematics of the inner 0.7
$\times$ 1.2 kpc$^{2}$ of the Seyfert galaxy ESO 362-G18, derived from optical
spectra obtained with the GMOS/IFU on the Gemini South telescope at a spatial
resolution of $\approx$170 pc and spectral resolution of 36 km s$^{-1}$. ESO
362-G18 is a strongly perturbed galaxy of morphological type Sa or S0/a, with a
minor merger approaching along the NE direction. Previous studies have shown
that the [OIII] emission shows a fan-shaped extension of $\approx$ 10\arcsec\
to the SE. We detect the [OIII] doublet, [NII] and H${\alpha}$ emission lines
throughout our field of view. The stellar kinematics is dominated by circular
motions in the galaxy plane, with a kinematic position angle of
$\approx$137$^{\circ}$. The gas kinematics is also dominated by rotation, with
kinematic position angles ranging from 122$^{\circ}$ to 139$^{\circ}$. A
double-Gaussian fit to the [OIII]$\lambda$5007 and H${\alpha}$ lines, which
have the highest signal to noise ratios of the emission lines, reveal two
kinematic components: (1) a component at lower radial velocities which we
interpret as gas rotating in the galactic disk; and (2) a component with line
of sight velocities 100-250 km s$^{-1}$ higher than the systemic velocity,
interpreted as originating in the outflowing gas within the AGN ionization
cone. We estimate a mass outflow rate of 7.4 $\times$ 10$^{-2}$ M$_{\odot}$
yr$^{-1}$ in the SE ionization cone (this rate doubles if we assume a biconical
configuration), and a mass accretion rate on the supermassive black hole (SMBH)
of 2.2 $\times$ 10$^{-2}$ M$_{\odot}$ yr$^{-1}$. The total ionized gas mass
within $\sim$84 pc of the nucleus is 3.3 $\times$ 10$^{5}$ M$_{\odot}$; infall
velocities of $\sim$34 km s$^{-1}$ in this gas would be required to feed both
the outflow and SMBH accretion.
