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Phased array optical telescope
| Details |
Inventors: Stuhlinger, Tilman W.;
Assignee: Talandic Research Corporation (Azusa, CA)
Primary Examiner: Hannaher; Constantine
Assistant Examiner: Glick; Edward J.
Attorney, Agent or Firm: Brunell; Norman E.
A phased array telescope in which the output field angle of each afocal subtelescope is equal to the arcsin of the product of the magnification and the sine of the input field angle. The resultant subtelescope distortion reduces piston error at the input to the beam combining telescope to increase resolution by reducing piston error otherwise caused by distortion-free subtelescopes. The phased array telescope uses only reflecting surfaces in order to operate over a wide spectral band. Optically powered primary, secondary and tertiary reflecting surfaces are combined with an aspheric folding mirror before the image that would have been formed by the secondary mirror to control the distortion of each subtelescope to exactly follow the arcsin rule provided. |
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DETAILED DESCRIPTION OF THE PREFERRED EMBODIMENT(S) FIG.
1 is a simplified phased array telescope design, shown in a fictional two-aperture configuration, for the purpose of describing conventional design requirements and practice.
In FIG.
1, phased array telescope 10 includes subtelescopes 12 and 14 coupled to beam combining telescope 16 by outer and inner fold mirror pairs 18 and 20, and 22 and 24, respectively.
Although phased array telescope 10 is shown in a two aperture configuration for convenience, a three or four aperture configuration is more likely to be used as a practical minimum aperture configuration.
During operation of phased array telescope 10, a wavefront of diameter D enters from the left and is broken by subtelescopes 12 and 14 into subaperture wavefronts of diameter s.
Subtelescopes 12 and 14 convert these subaperture wavefronts, known as the entrance pupil array, into output wavefronts of diameter .
sigma.
.
Outer and inner fold mirror pairs 18 and 20, and 22 and 24, convert the array of exiting subtelescope wavefronts, known as the exit pupil array, into an array of diameter d applied to beam combining telescope 16.
As noted herein above, the golden rule of separated telescopes requires that the array of exit pupils be an exact, demagnified replica of the entrance pupil array.
A mathematical expression of this requirement, based on the configuration of phased array telescope 10 may be presented as follows: d=D/m.
sub.
c .
sigma.
=s/m.
sub.
c (1) where m.
sub.
c is the subtelescope linear magnification, that is, the ratio of input to output marginal ray heights, D is the overall or global array diameter, d is the entrance pupil diameter of beam combining telescope 16, s is the entrance pupil diameter of subtelescopes 12 and 14 and .
sigma.
is the output beam diameter of subtelescopes 12 and 24.
The golden rule of separated telescopes also implies that the Lagrange invariant, H, must be satisfied by the configuration of phased array telescope 10, as follows: 0H=.
gamma.
D/2=(.
gamma
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