Abstract

To correct for the spherical aberration in the Hubble Space Telescope primary mirror, five anamorphic aspheric mirrors representing correction for three scientific instruments have been fabricated as part of the development of the corrective-optics space telescope axial-replacement instrument (COSTAR). During the acceptance tests of these mirrors at the vendor, a quick and simple method for verifying the asphere surface figure was developed. The technique has been used on three of the aspheres relating to the three instrument prescriptions. Results indicate that the three aspheres are correct to the limited accuracy expected of this test.

© 1993 Optical Society of America

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References

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  1. D. Malacara, Optical Shop Testing (Wiley, New York, 1978), Chap. 12.
  2. M. Born, E. Wolf, Principles of Optics (Pergamon, New York, 1975).
  3. Code V Reference Manual, Version 7.2 (Optical Research Associates, Pasadena, Calif., 1988).
  4. P. Glenn, “Surface telescope performance prediction using the optical surface analysis code (OSAC),” Opt. Eng. 23, 1026 (1986).

1986 (1)

P. Glenn, “Surface telescope performance prediction using the optical surface analysis code (OSAC),” Opt. Eng. 23, 1026 (1986).

Born, M.

M. Born, E. Wolf, Principles of Optics (Pergamon, New York, 1975).

Glenn, P.

P. Glenn, “Surface telescope performance prediction using the optical surface analysis code (OSAC),” Opt. Eng. 23, 1026 (1986).

Malacara, D.

D. Malacara, Optical Shop Testing (Wiley, New York, 1978), Chap. 12.

Wolf, E.

M. Born, E. Wolf, Principles of Optics (Pergamon, New York, 1975).

Opt. Eng. (1)

P. Glenn, “Surface telescope performance prediction using the optical surface analysis code (OSAC),” Opt. Eng. 23, 1026 (1986).

Other (3)

D. Malacara, Optical Shop Testing (Wiley, New York, 1978), Chap. 12.

M. Born, E. Wolf, Principles of Optics (Pergamon, New York, 1975).

Code V Reference Manual, Version 7.2 (Optical Research Associates, Pasadena, Calif., 1988).

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Figures (2)

Fig. 1
Fig. 1

Schematic drawing of the COSTAR CGH interferometer. The diffraction grating replaces CGH in the CGH stage. DMI, distance measuring interferometer.

Fig. 2
Fig. 2

(a) Goddard-high-resolution spectrograph, (b) faint-object spectrograph, (c) faint-object camera.

Tables (3)

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Table 1 Faint-Object-Spectrograph Zernike Comparison In p–v Waves

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Table 2 Goddard High-Resolution-Spectrograph Zernike Comparison in p–v Waves

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Table 3 Faint-Object-Camera Zernike Comparison in p–v Waves

Equations (1)

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Z = Z plane ( R ref { [ R ref ( X 2 + Y 2 ) ] } 1 / 2 ) ,

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