Abstract

A systematic performance analysis of aplanatic Cassegrainian telescopes has been accomplished by means of a ray trace program. The results indicate that the available field angle for a given geometric spot size is, to a very close approximation, a function of the relative back focal distance only. Image curvatures, as computed by third-order theory and by the ray trace program, were found to be in very close agreement. Image curvature is plotted as a function of the ray height ratio for a wide range of secondary magnification.

© 1974 Optical Society of America

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References

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  1. D. Korsch, J. Opt. Soc. Am. 63, 667 (1973).
    [CrossRef]
  2. D. Korsch, J. Opt. Soc. Am. 63, 497 (1973).
    [CrossRef]
  3. H. Köhler, Astron. Nachr. 278, 1 (1949).
    [CrossRef]
  4. H. Theissing, O. Zinke, Optik 3, 451 (1948).
  5. H. Slevogt, Z. Instrumentenkd. 62, 312 (1942).
  6. LST Project Guidelines and Requirements Document. George C. Marshall Space Flight Center, 21 September 1973.

1973 (2)

D. Korsch, J. Opt. Soc. Am. 63, 497 (1973).
[CrossRef]

D. Korsch, J. Opt. Soc. Am. 63, 667 (1973).
[CrossRef]

1949 (1)

H. Köhler, Astron. Nachr. 278, 1 (1949).
[CrossRef]

1948 (1)

H. Theissing, O. Zinke, Optik 3, 451 (1948).

1942 (1)

H. Slevogt, Z. Instrumentenkd. 62, 312 (1942).

Köhler, H.

H. Köhler, Astron. Nachr. 278, 1 (1949).
[CrossRef]

Korsch, D.

D. Korsch, J. Opt. Soc. Am. 63, 497 (1973).
[CrossRef]

D. Korsch, J. Opt. Soc. Am. 63, 667 (1973).
[CrossRef]

Slevogt, H.

H. Slevogt, Z. Instrumentenkd. 62, 312 (1942).

Theissing, H.

H. Theissing, O. Zinke, Optik 3, 451 (1948).

Zinke, O.

H. Theissing, O. Zinke, Optik 3, 451 (1948).

Astron. Nachr. (1)

H. Köhler, Astron. Nachr. 278, 1 (1949).
[CrossRef]

J. Opt. Soc. Am. (2)

D. Korsch, J. Opt. Soc. Am. 63, 497 (1973).
[CrossRef]

D. Korsch, J. Opt. Soc. Am. 63, 667 (1973).
[CrossRef]

Optik (1)

H. Theissing, O. Zinke, Optik 3, 451 (1948).

Z. Instrumentenkd. (1)

H. Slevogt, Z. Instrumentenkd. 62, 312 (1942).

Other (1)

LST Project Guidelines and Requirements Document. George C. Marshall Space Flight Center, 21 September 1973.

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Figures (5)

Fig. 1
Fig. 1

Geometry for the aplanatic Cassegrainian telescope = −D2/D1.

Fig. 2
Fig. 2

Field angle radius in milliradians as a function of the ray height, ratio , for a 1-μrad spot size.

Fig. 3
Fig. 3

Field angle radius in milliradians as a function of relative back focal distance b/D1 for a 1-μ rad spot size.

Fig. 4
Fig. 4

An example of LST class telescopes. Field angle radius in milliradians as a function of B for a 150 nrad spot size.

Fig. 5
Fig. 5

Image curvature (cm−1) as a function of the ray height ratio for f = −1000 cm.

Equations (7)

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δ 1 = 1 + { 2 / [ m 2 2 ( 1 + ) ] } ,
δ 2 = { 2 m 2 / [ ( 1 + ) ( m 2 + 1 ) ] 3 } [ ( m 2 1 ) / ( m 2 + 1 ) ] 2 .
r 1 = 2 f / m 2
r 2 = 2 f / ( m 2 + 1 )
d = ( f / m 2 ) ( 1 + )
b = f
1 R i = 1 f ( m 2 m 2 + 1 + m 2 + 1 2 m 2 2 · { [ m 2 ( + 1 ) + + 1 ] 2 δ 2 + [ m 2 ( 1 ) 1 ] 2 } ) .

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