  We used Gemini Multi-Object Spectrograph (GMOS) in the Integral Field Unit
mode to map the stellar population, emission line flux distributions and gas
kinematics in the inner kpc of NGC 5044. From the stellar populations synthesis
we found that the continuum emission is dominated by old high metallicity stars
($\sim$13 Gyr, 2.5Z$\odot$). Also, its nuclear emission is diluted by a non
thermal emission, which we attribute to the presence of a weak active galactic
nuclei (AGN). In addition, we report for the first time a broad component
(FWHM$\sim$ 3000km$s^{-1}$) in the H$\alpha$ emission line in the nuclear
region of NGC 5044. By using emission line ratio diagnostic diagrams we found
that two dominant ionization processes coexist, while the nuclear region (inner
200 pc) is ionized by a low luminosity AGN, the filamentary structures are
consistent with being excited by shocks. The H$\alpha$ velocity field shows
evidence of a rotating disk, which has a velocity amplitude of
$\sim$240kms$^{-1}$ at $\sim$ 136 pc from the nucleus. Assuming a Keplerian
approach we estimated that the mass inside this radius is $1.9\times10^9$
$M_{\odot}$, which is in agreement with the value obtained through the
M-$\sigma$ relation, $ M_{SMBH}=1.8\pm1.6\times10^{9}M_{\odot}$. Modelling the
ionized gas velocity field by a rotating disk component plus inflows towards
the nucleus along filamentary structures, we obtain a mass inflow rate of
$\sim$0.4 M$_\odot$. This inflow rate is enough to power the central AGN in NGC
5044.
