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We describe a rapid and direct method for regularizing, post-facto, the
point-spread function (PSF) of a telescope or other imaging instrument, across
its entire field of view. Imaging instruments in general blur point sources of
light by local convolution with a point-spread function that varies slowly
across the field of view, due to coma, spherical aberration, and similar
effects. It is possible to regularize the PSF in post-processing, producing
data with a homogeneous ``effective PSF'' across the entire field of view. In
turn, the method enables seamless wide-field astronomical mosaics at higher
resolution than would otherwise be achievable, and potentially changes the
design trade space for telescopes, lenses, and other optical systems where data
uniformity is important. For many kinds of optical aberration, simple and rapid
convolution with a locally optimized ``transfer PSF'' produces extremely
uniform imaging properties at low computational cost. PSF regularization} does
not require access to the instrument that obtained the data, and can be
bootstrapped from existing data sets that include starfield images or other
means of estimating the PSF across the field.
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