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If the optical system of a telescope is perturbed from rotational symmetry,the Zernike wavefront aberration coefficients describing that system can beexpressed as a function of position in the focal plane using spin-weightedZernike polynomials. Methodologies are presented to derive these polynomials toarbitrary order. This methodology is applied to aberration patterns produced bya misaligned Ritchey Chretian telescope and to distortion patterns at the focalplane of the DESI optical corrector, where it is shown to provide a moreefficient description of distortion than conventional expansions.

Non-axisymmetric aberration patterns from wide-field telescopes using spin-weighted Zernike Polynomials