Gas inflows towards the nucleus of the Seyfert 2 galaxy NGC1667
  We use optical spectra from the inner 2$\times$3kpc$^2$ of the Seyfert 2
galaxy NGC1667, obtained with the GMOS integral field spectrograph on the
Gemini South telescope at a spatial resolution of $\approx$ 240pc, to assess
the feeding and feedback processes in this nearby AGN. We have identified two
gaseous kinematical components in the emission line profiles: a broader
component ($\sigma\approx$ 400km s$^{-1}$) which is observed in the inner
1-2arcsec and a narrower component ($\sigma\approx$ 200km s$^{-1}$) which is
present over the entire field-of-view. We identify the broader component as due
to an unresolved nuclear outflow. The narrower component velocity field shows
strong isovelocity twists relative to a rotation pattern, implying the presence
of strong non-circular motions. The subtraction of a rotational model reveals
that these twists are caused by outflowing gas in the inner $\approx$ 1arcsec,
and by inflows associated with two spiral arms at larger radii. We calculate an
ionized gas mass outflow rate of $\dot{M}_{out}\approx$
0.16M$_{\odot}$yr$^{-1}$. We calculate the net gas mass flow rate across a
series of concentric rings, obtaining a maximum mass inflow rate in ionized gas
of $\approx$ 2.8M$_{\odot}$year$^{-1}$ at 800pc from the nucleus, which is two
orders of magnitude larger than the accretion rate necessary to power this AGN.
However, as the mass inflow rate decreases at smaller radii, most of the gas
probably will not reach the AGN, but accumulate in the inner few hundred
parsecs. This will create a reservoir of gas that can trigger the formation of
new stars.
