  We map the optical and near-infrared (NIR) emission-line flux distributions
and kinematics of the inner 320$\times$535pc$^2$ of the elliptical galaxy
NGC1052. The integral field spectra were obtained with the Gemini Telescope
using the GMOS-IFU and NIFS instruments, with angular resolutions of 0''88 and
0''1 in the optical and NIR, respectively. We detect five kinematic components:
(1 and 2) Two spatially unresolved components, being a broad line region
visible in H$\alpha$, with a FWHM of $\sim$3200km s$^{-1}$ and an
intermediate-broad component seen in the [OIII]$\lambda \lambda$4959,5007
doublet; (3) an extended intermediate-width component with 280<FWHM<450km
s$^{-1}$ and centroid velocities up to 400km s$^{-1}$, which dominates the flux
in our data, attributed either to a bipolar outflow related to the jets,
rotation in an eccentric disc or a combination of a disc and large-scale gas
bubbles; (4 and 5) two narrow (FWHM<150km s$^{-1}$) components, one visible in
[OIII], and one visible in the other emission lines, extending beyond the
field-of-view of our data, which is attributed to large-scale shocks. Our
results suggest that the ionization within the observed field of view cannot be
explained by a single mechanism, with photoionization being the dominant
mechanism in the nucleus with a combination of shocks and photoionization
responsible for the extended ionization.
