Prime Focus Spectrograph (PFS), a next-generation instrument being installed on the 8.2m Subaru Telescope, is a very wide-field, massively multiplexed, optical and near-infrared spectrograph. For its successful science operation, high-quality sky subtraction is of crucial importance to accurately extract weak galaxy signals. To achieve that, we are now developing modeling algorithms to determine the 2D point spread function (PSF) at arbitrary positions on the spectrograph detectors. The light coming into the detectors is affected by various components of the instrument before being observed as the final PSF, such as the telescope pupil illumination, focal ratio degradation in the fibers, and various aberrations of the spectrograph optics. We model the PSF by combining optical models of all these effects. Comparing the model with the data taken in commissioning observations, we determine over a hundred parameters. We present the current status of this PSF modeling.
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