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desired degree of accuracy by the incorporation of an aspheric element in the null corrector This method is limited to cases in which the gure of the aspheric element can be ascertained with an accuracy better than that desired for the aspheric mirror Primary mirrors that are to be incorporated into diffraction-limited space-borne optical systems are now required to have RMS gure errors as small as onehundredth of the wavelength of visible light It is therefore desirable that the components of a null corrector for these mirrors be spherical or at so that their gure errors can be measured to the required accuracy In the design of his null corrector, Ross found that the farther he put the lens from the center of curvature of the mirror, the less residual aberration there was when the compensation was exactly at the center and the edge.

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This is so because, although the longitudinal spherical aberration S of the normals to the paraboloid follows the simple law S y2=2R, where y is the distance of the normal from the axis of the paraboloid and R is its radius, additional terms of a power series would be required to describe the same spherical aberration distribution in a coordinate system with its origin at the null corrector For a null corrector in contact with the paraboloid, the compensating spherical aberration would be described by the same simple law Unfortunately, this null corrector would be as large as the paraboloid 1281.

Given the following functio ns F (s), find f(I).

Refractive Offner Compensator Offner (1963) pointed out that a small lens that forms a real image of a point source at the center of curvature of a paraboloid, in combination with a eld lens at the center of curvature that images the small lens at the paraboloid, is optically equivalent to a large lens at the paraboloid The use of a eld lens in this way was rst suggested by Schupmann to control secondary spectrum (Schupmann, 1899; Offner, 1969) This kind of compensator has been widely used to test astronomical optics of many different characteristics (Sasian, 1988) With a eld lens that images the compensating lens c at the paraboloid in Offner s arrangement, the spherical aberration of the compensating lens must follow the same law for aperture as do the normals to the paraboloid This restriction on the compensating lens is not necessary.

All that is required is that lens c provide suf cient third-order spherical aberration to compensate for that of the normals of the paraboloid The power of the eld lens (and thus the location of the image of lens c) is then varied to minimize the high-order aberration To balance the third-order aberration of the normals to a conicoidal mirror with conic constant K and base radius R, a planoconvex lens of focal length f and index of refraction n must satisfy the relation " # 2 2 KR 3n 1 1 m m 3n 2 m2 2 n 1 m 1 m 12:20 f n 1 n n 1 2 where m is the ratio l0=l (Fig 1233) (The conicoid must have K < 0 if the aberration of its normals are to be balanced by the spherical aberration of a planoconvex lens.

The sign convention is such that m < 0).

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