Type: Talk
Session: Modeling the Point Spread Function
Authors: Lucia Paz Garate Nunez

Abstract: The point spread function (PSF) of the telescope plays a crucial role when estimations of low-surface brightness sources are required. This extra flux could be confused with real faint flux, leading to inaccurate measurements. In this work, we use data from the third data release of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP PDR3) to construct extended PSF models. We follow a similar approach to Infante-Sainz et al. 2020, where we construct the different parts of the PSF by the median-clipping stacking of stars within a wide brightness range. By using bright and saturated stars to characterise the PSF wings and fainter and non-saturated stars to construct the inner parts, we obtain the HSC-SSP PDR3 PSFs with a radial extension of R ~ 5.6 arcmin. Due to the similarities in terms of depth, photometric bands and pipeline processing between HSC and LSST, our PSF reconstruction method will be directly applicable and beneficial to the LSST.