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Coma Off It: Removing Variable Point Spread Functions from Astronomical Images
Instrumentation and Methods for Astrophysics · Submitted 5 Dec 2022
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim 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.
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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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | 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. | contribution 0.99 | 0.88 | 0.35 | asserted 1.00 |
| s1 | 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. | background 1.00 | 0.07 | 0.04 | asserted 1.00 |
| s2 | It is possible to regularize the PSF in post-processing, producing data with a homogeneous ``effective PSF'' across the entire field of view. | contribution 0.51 | 0.28 | 0.39 | hedged possibility 0.81 |
| s3 | 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. | interpretation 0.97 | 0.26 | 0.40 | hedged possibility 0.72 |
| s4 | 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. | method 0.80 | 0.58 | 0.17 | asserted 0.98 |
| s5 | 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. | method 0.79 | 0.39 | 0.10 | asserted 0.97 |
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Original abstract
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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