  Pluto's atmospheric profiles (temperature and pressure) have been studied for
decades from stellar occultation lightcurves. In this paper, we look at recent
Pluto Global Climate Model (GCM) results (3D temperature, pressure, and density
fields) from Bertrand et al. (2020) and use the results to generate model
observer's plane intensity fields (OPIF) and lightcurves by using a Fourier
optics scheme to model light passing through Pluto's atmosphere (Young, 2012).
This approach can accommodate arbitrary atmospheric structures and 3D
distributions of haze. We compared the GCM model lightcurves with the
lightcurves observed during the 15-AUG-2018 Pluto stellar occultation. We find
that the climate scenario which best reproduces the observed data includes an
N2 ice mid-latitude band in the southern hemisphere. We have also studied
different haze and P/T ratio profiles: the haze effectively reduces the central
flash strength, and a lower P/T ratio both reduces the central flash strength
and incurs anomalies in the shoulders of the central flash.
