A Method to Characterize the Wide-angle Point-Spread Function of Astronomical Images

Abstract Uncertainty in the wide-angle point-spread function (PSF) at large angles (tens of arcseconds and beyond) is one dominant sources error a number important quantities observational astronomy. Examples include stellar mass shape galactic halos maximum extent starlight disks nearby galaxies. However, modeling PSF has long been challenge astronomical imaging. In this paper, we present self-consistent method to model images. Scattered light from multiple bright stars fitted simultaneously with background characterize extended wing using Bayesian framework operating on pixel-by-pixel level. The demonstrated our software elderflower applied data Dragonfly Telephoto Array its out 20′–25′. We compare that other telescopes, including SDSS show that, scales arcminutes, scattered markedly lower than wide-field imaging telescopes. energy wings sufficiently low optical cleanliness plays an role defining PSF. This component can be modeled accurately, highlighting power self-contained approach.