Ground-based coronagraphy with high-order adaptive optics
Abstract
We simulate the actions of a coronagraph matched to diffraction-limited adaptive optics (AO) systems on the Calypso 1.2 m, Palomar Hale 5 m and Gemini 8.1 m telescopes, and identify useful parameter ranges for AO coronagraphy on these systems. We model the action of adaptive wavefront correction with a tapered, high-pass filter in spatial frequency rather than a hard low frequency cutoff, and estimate the minimum number of AO channels required to produce sufficient image quality for coronagraphic suppression within a few diffraction widths of a central bright object (as is relevant to e.g., brown dwarf searches near late-type dwarf stars). We explore the effect of varying the occulting image- plane stop size and shape, and examine the trade-off between throughput and suppression of the image halo and Airy rings. We discuss our simulations in the context of results from the 241-channel Palomar Hale AO coronagraph system, and suggest approaches for future AO coronagraphic instruments on large telescopes.
Additional Information
© 2000 Society of Photo-Optical Instrumentation Engineers (SPIE). We thank T. Nakajima and S. R. Kulkarni for stimulating discussion, and B. R. Oppenheimer for pre-publication results and insightful comments. We also thank J. R. P. Angel for bringing high order AO to our attention as an important component of the next step in coronagraphy. Thanks are also due to R. L. White and E. P. Nelan for encouraging this study. We acknowledge the STScI Director's Discretionary Research Fund for support of RBM and travel support for AS, and the STScI Visitors' Program for travel support for CDK.Attached Files
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Additional details
- Eprint ID
- 91465
- Resolver ID
- CaltechAUTHORS:20181204-132723759
- Space Telescope Science Institute
- Created
-
2018-12-06Created from EPrint's datestamp field
- Updated
-
2021-11-16Created from EPrint's last_modified field
- Series Name
- Proceedings of SPIE
- Series Volume or Issue Number
- 4007