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Abstract

The T Tauri star T Cha is known to have a protoplanetary disk with a dust gap separating the inner and outer disk regions. The mid-IR JWST spectrum of T Cha show multiple prominent aromatic infrared bands (AIBs) around 6.2, 8.1, and 11.3 $\mu$m. AIBs are commonly accepted as the emission stemming from PAH molecules. We aim to characterize the PAHs giving rise to the AIBs observed in the JWST spectrum of T Cha. Our objective is to estimate the PAH abundances, in terms of their sizes, ionization fraction, and mass, in the disk of T Cha. We perform spectral fitting of the observed AIBs to identify the possible underlying PAH emission components. We transfer the stellar radiation through a parametric disk model of T Cha in order to reproduce the mid-IR spectrum, optical photometric fluxes, and mm continuum band fluxes of T Cha. We include stochastically heated PAH dust grains in our model to simulate the AIBs, and hence estimate the PAH abundances from the modelling. We use the results from previous observations and modelling efforts to reduce our model degeneracies. We estimate the PAH abundances in T Cha self-consistently, with other important disk parameters. The overall disk morphology - an inner and an outer disk separated by a dust gap - derived in this work is consistent with the previous results from Spitzer, VLT, and ALMA observations. PAHs are located only in the outer disk in our model. We estimate a population of small PAHs of <30 C atoms, with an ionized PAH fraction of ~0.15. We also obtain a PAH-to-dust mass ratio of ~6.5$\times$10$^{-3}$, which amounts to ~16% of the ISM value. We predict that the outer disk should have a frontal wall with smaller dust grains limited up to $\mu$m-order to fit the slope of the continuum within 14-15 $\mu$m. We propose a possibility of sub-micron dust grains within the gap to justify an observed plateau around ~10 $\mu$m in the JWST spectrum.