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We present a 3D radiative transfer model for the Spectral Energy Distribution(SED) of NGC 1365, which is a "changing look" Seyfert 1.8 type AGN. The SEDfrom the ultraviolet (UV) to the infrared (IR) is constructed using archivaldata from the UVIT on-board $AstroSat$, along with IR data from the literature.The SKIRT radiative transfer code is used to model the SED and derive thegeometry and composition of dust in this AGN. Similar to our earlier SED modelof NGC 4151, the nuclear region of NGC 1365 is assumed to contain a ring ordisk-like structure concentric to the accretion disk, composed of large(0.1$\mu$m - 1$\mu$m) graphite grains in addition to the two-phase dusty torusmade up of ISM-type grains (Ring And Torus or RAT model). We also include, forthe first time, an additional component of dusty wind in the form of a bipolarcone. We carry out a detailed analysis and derive the best-fit parameters froma $\chi^2 $ test to be $R_{\rm in,r}$ = 0.03 pc, $\sigma$ = 26$^\circ$ and$\tau$ = 20 for the assumed ring-torus-polar wind geometry. Our results suggestthe presence of hot dust at a temperature T $\sim$ 1216 K at the location ofthe ring which absorbs and scatters the incident UV radiation and emits in thenear-IR (NIR). In the mid-IR (MIR) the major contributors are the polar coneand warm dust with T $\sim$ 916 K at $R_{\rm in,t}$ = 0.1 pc. Not only are ourmodel radii in agreement with IR interferometric observations, our study alsoreiterates the role of high resolution UV observations in constraining the dustgrain size distribution in the nuclear regions of AGN.

Unravelling the Nuclear Dust Morphology of NGC 1365: A Two Phase Polar - RAT Model for the Ultraviolet to Infrared Spectral Energy Distribution