  Infrared interferometry of Seyfert galaxies has revealed that their warm
($300-400\,$K) dust emission originates primarily from polar regions instead of
from an equatorial dust torus as predicted by the classic AGN unification
scheme. We present new data for the type 1.2 object ESO$\,$323-G77 obtained
with the MID-infrared interferometric Instrument (MIDI) and a new detailed
morphological study of its warm dust. The partially resolved emission on scales
between $5$ and $50\,$mas ($1.6-16\,$pc) is decomposed into a resolved and an
unresolved source. Approximately $65\%$ of the correlated flux between $8$ and
$13\,\mu\mathrm{m}$ is unresolved at all available baseline lengths. The
remaining $35\%$ is partially resolved and shows angular structure. From
geometric modelling we find that the emission is elongated along a position
angle of $155^\circ\pm14^\circ$ with an axis ratio (major/minor) of
$2.9\pm0.3$. Because the system axis is oriented in position angle
$174^\circ\pm2^\circ$, we conclude that the dust emission of this object is
also polar extended. A $\textit{CAT3D-WIND}$ radiative transfer model of a
dusty disk and a dusty wind with a half opening angle of $30^\circ$ can
reproduce both the interferometric data and the SED, while a classical torus
model is unable to fit the interferometric data. We interpret this as further
evidence that a polar dust component is required even for low-inclination type
1 sources.
