High-resolution imaging with a tip-tilt Cassegrain secondary

Details High-resolution imaging with a tip-tilt Cassegrain secondary High-resolution imaging with a tip-tilt Cassegrain secondary

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasp..106...77c&link_type=abstract

Publications of the Astronomical Society of the Pacific, vol. 106, no. 695, p. 77-86

Physics

Optics

24

Adaptive Optics, Cameras, Cassegrain Optics, Image Motion Compensation, Imaging Techniques, Infrared Spectrometers, Infrared Telescopes, Mirrors, Reflecting Telescopes, Spectroscopic Telescopes, Astronomical Photography, Astronomical Spectroscopy, Infrared Astronomy, Infrared Photography

Scientific paper

A prototype adaptive secondary mirror has been developed on a 2.3-m telescope to stabilize rapid motion caused by atmospheric turbulence. The instantaneous position of an image's centroid, or brightest speckle, is measured by a near-infrared camera system which enables the tip-tilt mirror to recenter the image. Correction is accomplished at closed-loop frequencies of less than or = 100 Hz on guide stars with K (2.2 micrometers) magnitudes less than or = 8. Image motion is reduced to less than 0.1 sec rms, removing over 90% of low-frequency (f less than or = 5 Hz) tilt power, leaving less than or = 1 rad exp 2 mean square wave front tilt phase error. In seeing conditions where D/ro approximately = 4, long exposures in the H band (1.6 micrometers) exhibit a nearly diffraction-limited resolution of 0.19 sec full width at half maximum (FWHM) (Strehl ratio aprroximately = 0.14)-a factor of 4 improvement over uncorrected images. Reduction of the present static optical errors will improve the Strehl ratio another factor of 2, leading to approximately 70% of the maximum possible Strehl ratio.

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