Image Processing Reference
large kuiper belt object 2003 EL61,” Astrophysical Journal ,
632 , L45-L48
Wizinowich, P.L., et al., “Adaptive optics developments at Keck observatory,”
Proceedings of SPIE , 4839 , 9-20 (2003).
The WIYN Observatory is located on Kitt Peak in Arizona and has the 3.5-m
WIYN telescope. The observatory is operated by a consortium of three universities,
Wisconsin, Indiana, and Yale, as well as the National Optical Astronomy Observa-
tory. This telescope has also been used to evaluate orthogonal transfer cameras for
correction of image motion. An active optics system is presently being developed
for use on the telescope to enhance image quality.
Claver, C.F., C. Corson, R.R. Gomez, P.N. Daly, D.M. Dryden, B. Abareshi,
“WIYN tip-tilt module performance,” Proceedings of SPIE ,
4837 , 438-447
Vieira, K., W.F. van Altena, T.M. Girard, “Astrometry with OPTIC at WIYN,”
Astrometry in the Age of the Next Generation of Large Telescopes, ASP Con-
ference Series , edited by P. Kenneth Seidelmann and Alice K.B. Monet. Vol.
338, Lowell Observatory, Flagstaff, Ariz., USA. Astronomical Society of the
Pacific, San Francisco (2005).
7.4 Beam Steering for Interferometers
Long-baseline interferometers use many small-aperture telescopes to provide im-
age resolution equivalent to that of full-aperture telescopes several hundred meters
in diameter. Today's technology does not fully support full-aperture telescopes of
this size, making long-baseline interferometers the highest resolution instruments
available. Moving light from the individual telescopes hundreds of meters and
maintaining the phase relationship of the original wavefront requires beam stabili-
zation to operate at very high precision.
The first long-baseline interferometer was developed by Pease and Michelson
using the 100-in. telescope at Mount Wilson. This 20-ft interferometer is known as
the Michelson Stellar Interferometer; it positioned two auxiliary mirrors above the
100-in telescope mirror. The result was the first high-resolution measurement of
stars and the determination of their diameters. This instrument was the forerunner
of a 50-ft interferometer on Mount Wilson, also developed by Pease.
Modern long-baseline interferometers use meter class and larger telescopes to
collect the light over extremely long baselines and provide resolutions far beyond
the early instruments. A partial list of interferometers that makes use of image sta-
bilization is given in the next section.