three-mirror anastigmat

A telescope with only one curved mirror, such as a Newtonian telescope, will always have aberrations. If the mirror is spherical, it will suffer from spherical aberration. If the mirror is made parabolic, to correct the spherical aberration, then it must necessarily suffer from coma and off-axis astigmatism. This allows a larger useful field of view, and the remaining astigmatism is symmetrical around the distorted objects, allowing astrometry across the wide field of view. However, the astigmatism can be reduced by including a third curved optical element. When this element is a mirror, the result is a three-mirror anastigmat. In practice, the design may also include any number of flat fold mirrors, used to bend the optical path into more convenient configurations.

Many combinations of three mirror figures can be used to cancel all third-order aberrations. In general these involve solving a relatively complicated set of equations. A few configurations are simple enough, however, that they could be designed starting from a few intuitive concepts.

The first were proposed in 1935 by Maurice Paul. The basic idea behind Paul's solution is that spherical mirrors, with an aperture stop at the centre of curvature, have only spherical aberration – no coma or astigmatism (but they do produce an image on a curved surface of half the radius of curvature of the spherical mirror). So if the spherical aberration can be corrected, a very wide field of view can be obtained. This is similar to the conventional Schmidt design, but the Schmidt does this with a refractive corrector plate instead of a third mirror. Paul's idea was to start with a Mersenne beam compressor, which looks like a Cassegrain made from two (confocal) paraboloids, with both the input and output beams collimated. The compressed input beam is then directed to a spherical tertiary mirror, which results in traditional spherical aberration. Paul's key insight is that the secondary can then be converted back to a spherical mirror. One way to look at this is to imagine the tertiary mirror, which suffers from spherical aberration, being replaced by a Schmidt telescope, with a correcting plate at its centre of curvature. If the radii of the secondary and tertiary are of the same magnitude, but opposite sign, and if the centre of curvature of the tertiary is placed directly at the vertex of the secondary mirror, then the Schmidt plate would lie on top of the paraboloid secondary mirror. Therefore, the Schmidt plate required to make the tertiary mirror a Schmidt telescope is eliminated by the paraboloid figuring on the convex secondary of the Mersenne system, as each corrects the same magnitude of spherical aberration, but the opposite sign. Also, as the system of Mersenne + Schmidt is the sum of two anastigmats (the Mersenne system is an anastigmat, and so is the Schmidt system), the resultant system is also an anastigmat, as third-order aberrations are purely additive. In addition the secondary is now easier to fabricate, as it is spherical rather than parabolic. This design is also called a Mersenne–Schmidt, since it uses a Mersenne configuration as the corrector for a Schmidt telescope.

Paul's solution had a curved focal plane, but this was corrected in the Paul–Baker design, introduced in 1969 by James Gilbert Baker. The Paul–Baker design adds extra spacing and reshapes the secondary to elliptical, which corrects field curvature to flatten the focal plane.

A more general set of solutions was developed by Dietrich Korsch in 1972. A Korsch telescope is corrected for spherical aberration, coma, astigmatism, and field curvature and can have a wide field of view while ensuring that there is little stray light in the focal plane.

• Illustration — Eisenberg–Pearson two-mirror three-surface • Illustration — Eisenberg solid three-mirror anastigmat A variation of the Korsch design is the two-mirror three-surface telescope introduced by Shai Eisenberg and Earl T. Pearson in 1987. Employing the Korsch equations with minimal modifications, the number of mirrors is reduced from three to two by combining the primary surface and the tertiary surface on the same mirror. In one option the tertiary is identical to the primary, whereas the second option shows the tertiary as polished into the primary mirror. The Eisenberg–Pearson telescope does not require a flat fold mirror to allow access to the image plane, since the focal plane is located behind the secondary mirror. A compact illustration of the Korsch telescope published in 1995 by Shai Eisenberg is the solid version of the design with the use of total internal reflection (TIR) to integrate the fourth fold mirror without introducing vignetting.

• The James Webb Space Telescope is a three-mirror anastigmat featuring an ellipsoidal primary, hyperboloidal secondary, and ellipsoidal tertiary. • The Euclid mission uses a Korsch telescope. • The project includes a 100 mm working model built in 1985 and a 500 mm prototype built in 1986. • The Vera C. Rubin Observatory's telescope (formerly known as Large Synoptic Survey Telescope) is an Eisenberg-Pearson design with an additional refractive corrector. • The KH-11 Kennen (or perhaps the now cancelled Future Imagery Architecture) telescopes may be a three-mirror anastigmat, since the spare telescopes given to NASA by the National Reconnaissance Office are of this form. • One of these spare telescopes, the Nancy Grace Roman Space Telescope, formerly named the Wide Field Infrared Survey Telescope (WFIRST), employs a folded three-mirror anastigmat featuring an ellipsoidal primary, hyperboloidal secondary, and ellipsoidal tertiary. An earlier design used an off-axis three-mirror anastigmat. • The Extremely Large Telescope will be a three-mirror anastigmat design, with two additional flat fold mirrors. • The Deimos2 and DubaiSat2 Earth observation satellites both carry a three-mirror anastigmat Korsch design telescope. • Ralph imaging spectrometer on New Horizons spacecraft