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 $13,mumathrm{m}$ 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 $155^circpm14^circ$ with an axis ratio (major/minor) of $2.9pm0.3$. Because the system axis is oriented in position angle $174^circpm2^circ$, 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.
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