  We observed the nuclear region of the galaxy NGC 1365 with the integral field
unit of the Gemini Multi Object Spectrograph mounted on the GEMINI-South
telescope. The field of view covers $13^{\prime\prime} \times 6^{\prime\prime}$
($1173 \times 541$ pc$^{2}$) centered on the nucleus, at a spatial resolution
of $52$ pc. The spectral coverage extends from $5600$ \AA\ to $7000$ \AA, at a
spectral resolution $R=1918$. NGC 1365 hosts a Seyfert 1.8 nucleus, and
exhibits a prominent bar extending out to $100^{\prime\prime}$ (9 kpc) from the
nucleus. The field of view lies within the inner Lindblad resonance. Within
this region, we found that the kinematics of the ionized gas (as traced by
[OI], [NII], H$\alpha$, and [SII]) is consistent with rotation in the
large-scale plane of the galaxy. While rotation dominates the kinematics, there
is also evidence for a fan-shaped outflow, as found in other studies based on
the [OIII] emission lines. Although evidence for gas inflowing along nuclear
spirals has been found in a few barred galaxies, we find no obvious signs of
such features in the inner kiloparsec of NGC 1365. However, the emission lines
exhibit a puzzling asymmetry that could originate from gas which is slower than
the gas responsible for the bulk of the narrow-line emission. We speculate that
it could be tracing gas which lost angular momentum, and is slowly migrating
from the inner Lindblad resonance towards the nucleus of the galaxy.
