Ionized gas kinematics within the inner kiloparsec of the Seyfert galaxy
  NGC 1365
  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.
