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

Abstract

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

19 pages, 5 figures

References in corpus (3)

• The Dark Energy Camera
• Astrometric calibration and performance of the Dark Energy Camera
• ProtoDESI: First On-Sky Technology Demonstration for the Dark Energy Spectroscopic Instrument

Cited by in corpus (2)

• Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument
• Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane