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We use optical spectra from the inner 2$\times$3kpc$^2$ of the Seyfert 2galaxy NGC1667, obtained with the GMOS integral field spectrograph on theGemini South telescope at a spatial resolution of $\approx$ 240pc, to assessthe feeding and feedback processes in this nearby AGN. We have identified twogaseous kinematical components in the emission line profiles: a broadercomponent ($\sigma\approx$ 400km s$^{-1}$) which is observed in the inner1-2arcsec and a narrower component ($\sigma\approx$ 200km s$^{-1}$) which ispresent over the entire field-of-view. We identify the broader component as dueto an unresolved nuclear outflow. The narrower component velocity field showsstrong isovelocity twists relative to a rotation pattern, implying the presenceof strong non-circular motions. The subtraction of a rotational model revealsthat 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 anionized gas mass outflow rate of $\dot{M}_{out}\approx$0.16M$_{\odot}$yr$^{-1}$. We calculate the net gas mass flow rate across aseries of concentric rings, obtaining a maximum mass inflow rate in ionized gasof $\approx$ 2.8M$_{\odot}$year$^{-1}$ at 800pc from the nucleus, which is twoorders 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 gasprobably will not reach the AGN, but accumulate in the inner few hundredparsecs. This will create a reservoir of gas that can trigger the formation ofnew stars.

Gas inflows towards the nucleus of the Seyfert 2 galaxy NGC1667