  We present the first spatially resolved mass outflow rate measurements ($\dot
M_{out}$) of the optical emission line gas in the narrow line region (NLR) of a
Seyfert 2 galaxy, Markarian 573. Using long slit spectra and [O III] imaging
from the Hubble Space Telescope and Apache Point Observatory in conjunction
with emission line diagnostics and Cloudy photoionization models, we find a
peak outflow rate of $\dot M_{out} \approx$ 3.4 $\pm$ 0.5 $M_{\odot}$ yr$^{-1}$
at a distance of 210 pc from the central supermassive black hole (SMBH). The
outflow extends to distances of 600 pc from the nucleus with a total mass and
kinetic energy of $M \approx 2.2 \times 10^6 M_{\odot}$ and $E \approx 5.1
\times 10^{54}$ erg, revealing the outflows to be more energetic than those in
the lower luminosity Seyfert 1 galaxy NGC 4151 (Crenshaw et al. 2015). The peak
outflow rate is an order of magnitude larger than the mass accretion and
nuclear outflow rates, indicating local in-situ acceleration of the
circumnuclear NLR gas. We compare these results to global techniques that
quantify an average outflow rate across the NLR, and find the latter are
subject to larger uncertainties. These results indicate that spatially resolved
observations are critical for probing AGN feedback on scales where
circumnuclear star formation occurs.
