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Title: 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.

Authors:
 [1]
  1. Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
Publication Date:
Research Org.:
Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
Contributing Org.:
DESI
OSTI Identifier:
1409339
Report Number(s):
FERMILAB-PUB-17-508-AE-CD; arXiv:1711.03916
Journal ID: ISSN 0004-6280; 1637059
Grant/Contract Number:  
AC02-07CH11359
Resource Type:
Accepted Manuscript
Journal Name:
Publications of the Astronomical Society of the Pacific
Additional Journal Information:
Journal Volume: 130; Journal Issue: 986; Journal ID: ISSN 0004-6280
Publisher:
Astronomical Society of the Pacific
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; methods analytical; telescopes

Citation Formats

Kent, Stephen M. Non-axisymmetric Aberration Patterns from Wide-field Telescopes Using Spin-weighted Zernike Polynomials. United States: N. p., 2018. Web. doi:10.1088/1538-3873/aaa6b8.
Kent, Stephen M. Non-axisymmetric Aberration Patterns from Wide-field Telescopes Using Spin-weighted Zernike Polynomials. United States. doi:10.1088/1538-3873/aaa6b8.
Kent, Stephen M. Thu . "Non-axisymmetric Aberration Patterns from Wide-field Telescopes Using Spin-weighted Zernike Polynomials". United States. doi:10.1088/1538-3873/aaa6b8. https://www.osti.gov/servlets/purl/1409339.
@article{osti_1409339,
title = {Non-axisymmetric Aberration Patterns from Wide-field Telescopes Using Spin-weighted Zernike Polynomials},
author = {Kent, Stephen M.},
abstractNote = {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.},
doi = {10.1088/1538-3873/aaa6b8},
journal = {Publications of the Astronomical Society of the Pacific},
number = 986,
volume = 130,
place = {United States},
year = {2018},
month = {2}
}

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Figures / Tables:

Figure 1 Figure 1: (a) Schematic diagram showing the orientation and coordinate system definitions of the pupil plane ($ρ, ψ$) and focal plane ($r, \phi$). Each point in the focal plane (e.g., at radius vector $\bar{r}$) sees an image of the exit pupil. A global Cartesian ($x, y$) system is illustrated. (b)more » Another diagram of the pupil plane, this time showing the projection of the radius vector r onto the pupil plane. One can define local pupil axes ($r, t$) that are aligned parallel and perpendicular to the projected radius vector and that are rotated by phgr relative to the global ($x, y$) axes. Pupil coordinates in this system are given by $ρ$ and $ψ$$\prime$= ψ − $\phi$.« less

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