Asymmetries in adaptive optics point spread functions
- Stanford Univ., CA (United States)
- Univ. of Notre Dame, IN (United States)
- Space Telescope Science Institute, Baltimore, MD (United States)
- Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
- California Institute of Technology (CalTech), Pasadena, CA (United States)
- Univ. of Arizona, Tucson, AZ (United States)
- National Astronomical Observatory of Japan (NAOJ), Hilo, HI (United States)
- Univ. of Georgia, Athens, GA (United States)
- Univ. of Montreal, QC (Canada)
- Univ. of California, Berkeley, CA (United States)
- Univ. of California, Los Angeles, CA (United States)
- Amherst College, MA (United States)
- Univ. of Victoria, BC (Canada)
- Gemini Observatory, Hilo, HI (United States)
- Univ. of Michigan, Ann Arbor, MI (United States)
- European Southern Observatory, Vitacura, Santiago (Chile)
- US National Park Service (NPS), Fort Collins, CO (United States). Natural Sounds and Night Skies Division
- Large Synoptic Survey Telescope, Tucson, AZ (United States)
- Univ. of California, San Diego, La Jolla, CA (United States)
- SETI Institute, Mountain View, CA (United States)
- NASA Ames Research Center (ARC), Moffett Field, Mountain View, CA (United States)
- National Research Council of Canada Herzberg, Victoria, BC (Canada)
- Univ. of Western Ontario, London, ON (Canada)
- American Museum of Natural History (AMNH), New York, NY (United States)
- Arizona State Univ., Tempe, AZ (United States)
- Gemini Observatory, La Serena (Chile)
- Cornell Univ., Ithaca, NY (United States)
- Leiden Univ. (Netherlands)
An explanation for the origin of asymmetry along the preferential axis of the point spread function (PSF) of an AO system is developed. When phase errors from high-altitude turbulence scintillate due to Fresnel propagation, wavefront amplitude errors may be spatially offset from residual phase errors. These correlated errors appear as asymmetry in the image plane under the Fraunhofer condition. In an analytic model with an open-loop AO system, the strength of the asymmetry is calculated for a single mode of phase aberration, which generalizes to two dimensions under a Fourier decomposition of the complex illumination. Other parameters included are the spatial offset of the AO correction, which is the wind velocity in the frozen flow regime multiplied by the effective AO time delay and propagation distance or altitude of the turbulent layer. In this model, the asymmetry is strongest when the wind is slow and nearest to the coronagraphic mask when the turbulent layer is far away, such as when the telescope is pointing low toward the horizon. A great emphasis is made about the fact that the brighter asymmetric lobe of the PSF points in the opposite direction as the wind, which is consistent analytically with the clarification that the image plane electric field distribution is actually the inverse Fourier transform of the aperture plane. Validation of this understanding is made with observations taken from the Gemini Planet Imager, as well as being reproducible in end-to-end AO simulations.
- Research Organization:
- Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)
- Sponsoring Organization:
- USDOE National Nuclear Security Administration (NNSA); National Science Foundation (NSF); National Aeronautics and Space Administration (NASA)
- Grant/Contract Number:
- AC52-07NA27344; AST-1411868; NNX14AJ80G; NNX15AC89G; NNX15AD95G
- OSTI ID:
- 1844073
- Report Number(s):
- LLNL-JRNL-831471; 1048339; TRN: US2302327
- Journal Information:
- Journal of Astronomical Telescopes, Instruments, and Systems, Vol. 5, Issue 04; ISSN 2329-4124
- Publisher:
- SPIECopyright Statement
- Country of Publication:
- United States
- Language:
- English
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