10.1.2. Sub-aperture corrector examples: Two-mirror systems
The most common two-mirror candidates for sub-aperture corrector are classical Cassegrain, Dall-Kirkham and Ritchey-Chretien. In addition, the simplest two-mirror arrangement, consisting of a pair of spherical mirrors, also can be made (very) useable with the addition of sub-aperture corrector. The two examples are Field's two-mirror telescope, using a single meniscus corrector, and Klevtsov, using two-element corrector to offset the aberrations of a pair of spherical mirrors.
Sub-aperture corrector with two-mirror systems usually fills one of these two roles: it either serves as field corrector in systems that have good axial correction, or comes as an integral part of a system that cannot function without it. The former is usually referred to as field corrector, and the latter, somewhat informally, will be referred to as integrated (sub-aperture) corrector.
The advantage of sub-aperture vs. full-aperture corrector is in much less glass required, also resulting in less added weight. The disadvantage is that they generally have more stringent tolerances for both, fabrication and alignment. The chromatism of a corrector is typically very low, and usually not a factor.
Sub-aperture correctors for classical Cassegrain
In general, correcting field aberrations in classical Cassegrain, often with field curvature included, requires more or less simple two-element sub-aperture corrector. Depending on corrector's design, it can be either add-on field corrector, or integrated system corrector. Follow examples of both types. All four systems below are fast, or very fast for a Cassegrain, but have flat, well corrected fields. System A, published by Charles Rydel (SPECS), features two BK7 lenses, one plano-concave and the other bi-convex. System B, designed by Mike I. Jones (SPECS), uses two meniscus elements (FK5/BK7). Both these systems are classical Cassegrains that can function without field corrector. Unlike them, the last two systems with paraboloidal primary and spherical secondary, are useless without their integrated correctors. System C (SPECS) uses a Harmer-Wynne type corrector. System D (SPECS) uses three simple plano-convex/concave lenses in a very fast, well corrected arrangement.
For comparison, at 0.5° off-axis, coma blur in an f/10 classical Cassegrain w/o corrector would be three times the Airy disc diameter, and in an f/5.9 as much as 14 times larger than the Airy disc (0.82 and 3.7 waves P-V, respectively).
Sub-aperture correctors for Dall-Kirkham telescope
Due to its spherical secondary and less aspherised primary, Dall-Kirkham (DK) telescope is easier to fabricate than any other all-reflecting two-mirror system. However, its relatively strong coma severely limits quality field already at medium focal ratios. A simple two-element sub-aperture corrector can effectively eliminate both, coma and field curvature. However, since such corrector induce under-correction, the primary is somewhat more strongly aspherised (still prolate ellipsoid). Thus these are integrated correctors. Also, DK with sub-aperture corrector is significantly more sensitive to misalignment.
The DK correctors can come in various forms, but the three general configurations are: (1) a pair of plano-concave/convex lenses of identical reversed radii, (2) two meniscus lenses in () configuration, and (3) two meniscus lenses in )( configuration. Degree of correction is similar for all (meniscus correctors are likely to show smaller ray spots, but at that high level of correction it has little or no practical consequences).
Design A (SPECS) uses corrector made of two thin PCV/PCX BK7 lenses, for near-perfect overall correction. Corrector in the design B (SPECS) has advantage of being closer to the focal plane, thus using smaller lenses. On the other hand, lenses are more difficult to make. Designs C (SPECS) and D (SPECS) illustrate the influence of primary's focal ratio on corrector's performance. In general, the faster primary, the more aberrations generated at the secondary, and the harder it is to achieve high level of correction. The last design uses 3 easy to make lenses, with the role of the separated negative lens being to cancel lateral color.
The A sub-correctors for classical Cassegrain and DK are the simplest type, only requiring two plane surfaces and two identical reversed radii. Despite their apparent simplicity, needed calculation is quite complex. The focus is on coma, which requires establishing coma mirrors' aberration coefficient for the two mirrors - given by Eq. 82 as coma aberration coefficient, which determines the peak aberration coefficient as given by Eq. 13 - and find at which corrector location it can be can be cancelled by the opposite coma induced by corrector, calculated from Eq. 98, with the effective aperture stop separation T for the corrector's front lens being the distance to the exit pupil formed by the secondary (measured from the pupil to the surface).
With proper choice of lens radii and corrector location both, lower-order coma and astigmatism can be corrected. As mentioned, primary conic is made somewhat stronger, to correct for under-correction induced by the lens corrector. The raytrace showed the presence of higher-order aberrations, which required additional radii/location adjustment, in order to have it minimized by balancing it with the lower-order form. Corrector's final parameters are the result of a lengthy series of iterations.
The result is a modified Dall-Kirkham telescope with integrated sub-aperture lens corrector, and significantly improved field quality. Diffraction limited field in the green light typically approaches 1° in diameter on flat field, up to a dozen times, or more, greater than in a comparable all-reflecting Dall-Kirkham. Quality field is also up to several times greater than in a comparable all-reflecting classical Cassegrain, and significantly greater than in a comparable all-reflecting Ritchey-Chretien. Beyond 1° off-axis, or so, image often quickly deteriorates - more so than in all-reflecting Dall-Kirkham, classical Cassegrain and Ritchey-Chretien - as a result of higher-order astigmatism and coma. That, however, has little importance since the field size is typically limited to about 1°, or less.
Sub-aperture corrector for the Ritchey-Chretien
The two remaining aberration in the Ritchey-Chretien (RC) are astigmatism and field curvature. Astigmatism alone significantly limits quality field even over best (curved) image surface. Over flat field, it is further reduced by defocus resulting from field curvature. Neither aberration is significant in visual use. However, considering that the usual purpose of RC systems is imaging, some form of corrective action is necessary to improve quality of the outer field. Bending detector's surface to conform to best image curvature cancels out field curvature, but astigmatism still remains. Fortunately, correcting both aberrations is possible with relatively simple sub-aperture correctors. Since generating astigmatism by a lens corrector does not necessarily generate spherical aberration as well - such as the case with coma correctors - RC systems can use add-on field correctors for that purpose. Two examples are shown below.
System at left (SPECS) uses a pair of plano-concave and plano-convex lens of the same glass (BK7), designed by Richard from U.K. Lens elements have somewhat different surface radii, which is compensated for by widening the separation. Field correction is excellent, with the error in e-line being still only 0.068 wave RMS at the edge of 0.4-degree field radius. Color error is literally non-existent: as little as 0.01 wave RMS axially at 404nm and nearly half as much at 830nm. System at right (SPECS) uses two meniscus lenses, also BK7, for just as good, near-perfect correction: the e-line RMS wavefront error ranges from 0.017 on axis to 0.031 at 0.4° off-axis; axial color error is 0.068 wave RMS at 404nm, and 0.026 at 830nm, not changing appreciably over the entire field.
Particular form of a corrector, placed at the secondary mirror, was published as a complete analysis by Argunov in Russia, 1962 (about a decade later, similar arrangement was described in the U.S. by Richter, known as "Acme" telescope). It consists of an achromatized contact doublet whose rear surface is made reflective, serving as the secondary. Its limitation is relatively significant axial chromatism and, according to Klevtsov, hard to eradicate light scatter/ghosting. There is no published prescription, but a detailed analysis of the system is given in the articles by Argunov (USSR patent# 158697), which is the base of the Argunov-like system shown below (it uses LZOS glasses, OF3 and K2). It is a quite fast system, with the secondary spectrum more than 3 times smaller than in the comparable doublet achromat.
In 1966, Argunov came up with an advanced single-glass double-meniscus "isochromatic" (literally, "all colors equal") corrector. According to Klevtsov, it also has light scatter problem, and correcting the small residual coma requires corrector somewhat separated from the secondary. There is also no prescription available, so the system shown is to illustrate main characteristics of this arrangement; it uses LZOS glass, but replacing it with BK7 would not affect performance. Due to its strong radii, this corrector type requires meeting very tight tolerances.
In 1966, Popov found solution for an aplanatic catadioptric telescope using a single thick meniscus in front of the secondary. System of this type is shown below. It has very good axial correction, good control of astigmatism, but strong field curvature and some lateral color.
Other sub-aperture correctors for two-mirror system: Field-Maksutov, Klevtsov, Celestron Edge, Vixen VC200L
A simple corrector for all-spherical two-mirror system would be the ultimate in convenience, since it would make aspherizing the mirrors unnecessary. Such correctors exist, but are less in use than full-aperture correctors for all-spherical systems. The reason is that, in general, they don't offer as good overall level of correction, and/or that their fabrication and alignment tolerances are significantly more stringent. It is particularly pronounced here, due to this particular corrector type having to correct an enormous amount of aberrations. Two examples of all-spherical two-mirror systems with integrated sub-aperture corrector are shown below (obviously, the corrector here must by integrated, since spherical mirrors alone would be entirely useless as a telescope).
Field-Maksutov (SPECS) mainly corrects for spherical aberration. The corrector offsets only a small fraction of primary's coma; with the secondary offsetting nearly half of it, the system as a whole has approximately half of the primary's coma, as angular wavefront aberration. Since the final linear field for given field angle is larger than that of the primary by the factor of secondary magnification m, the final linear diffraction-limited field radius is, from Eq. 70.2, approximated by mF13/45, or FF12/45 in mm, with F1 and F being the focal ratio of the primary and system, respectively. In this particular system, with F1=3, m=3.3 and F=10, diffraction limited field radius is little over 2mm. In that, an f/10 Field-Maksutov is nearly identical to a commercial f/2/10 SCT (SCT with an f/3 primary would, of course, have significantly less coma).
Field-Maksutov coma is somewhat dependant on the meniscus thickness. In general, thicker meniscus offsets more of primary's coma, and vice versa, but the difference is not significant. In the above system, reducing meniscus thickness by 25% increases coma by about 10%. Placing aperture stop at the tube opening (as indicated above) nearly halves the astigmatism; however, since the coma is by far the dominant aberration, and not affected by stop position (the change in coma contribution by the spherical primary is nearly entirely offset by the opposite change at the corrector and secondary) the effect is relatively small: only about 4% reduction in the RMS wavefront error at 0.5° off-axis).
Addition of the second lens in the Klevtsov design (SPECS) enables correction of both, coma and spherical aberration (f/3/10 system is rescaled version from Busack's PointSpread). However, corrector adds astigmatism, rising the total system astigmatism near to double that of the primary mirror. Still, field correction is significantly better than Field's, with the RMS wavefront error of astigmatism at 0.5° off axis being about 1/3 smaller (considering that astigmatism changes with the square of field radius, vs. coma changing with field radius, Klevtsov's field quality advantage is considerably greater than what the edge error implies).
In addition, visual field in the Klevtsov should be further improved due to partial offset of its astigmatism with eyepiece astigmatism (in other words, visual field quality in the Klevtsov is limited by somewhat reduced astigmatism of the eyepiece).
Relatively recent use for sub-aperture corrector has been found in the commercial SCT telescope as well. While coma of this compact arrangement can be corrected by aspherizing the secondary, field curvature still remains, and can only be corrected by adding a field flattener. Since a pair of lenses can do both, correct for coma and field curvature, aspherizing the secondary becomes unnecessary. Two examples below are based on the Celestron's published data (EdgeHD White Paper - Final). Since no specific prescription has been given in the paper, the systems shown are not the exact replica, but the performance level should be practically identical.
Coma and field curvature can be corrected with a similar corrector consisting of a pair of BK7 lenses, but the astigmatism is nearly twice greater. It implies that better correction might be possible with some other, more expensive glass combination, As mentioned, off axis error of these systems is already practically negligible, and added expense for the further improvement - if possible - probably wouldn't be justified.
Vixen's VC200L VISAC, a 200mm f/9 system advertised as having primary with 6th order figure, uses 3-element sub-aperture corrector to achieve a highly corrected flat-field design. While its image contrast is somewhat compromised due to its 40% (linear) obstruction, correction level achievable with this design is exquisite. Technial drawing of the design can be found online, and suffice for reconstructing what is not strictly the actual design, but one that doesn't differ significantly in its level of correction.
The violet g-line error is below 1/40 wave P-V, and the rest of lines have at least twice smaller error. Axial e-line Strehl 1.000000 is a rare sight indeed, and the polychromatic Strehl is 0.999+. The effect of central obstruction is analyzed in detail elsewhere. Of course, it is not to expect that the actual units offer this level of correction, but the design certainly does offer a realistic possibility to deliver "sensibly perfect" performance, as long as the aberrations are concerned. And so is unrealistic to expect the "6th order curve" on the primary, which in this case would require surface correction by 1/23 wave on its deepest point, at the edge (if corrected for 6th order spherical at its paraxial focus, from the product of the A6 coefficient and ρd6, with 0<ρ<1 and d the aperture radius; if corrected at its best focus, the curve added to the surface is described with ρ6-0.9ρ2 instead of ρ, and the deepest point is at the 77% zone, 1/50 wave P-V). Just by optimizing the 4th order curve by adding a tiny amount of overcorrection to minimize the higher-order component - which in this case translates into -0.69 conic, since the conic K relates to the 4th power coefficient as A4=Kd4/8R3 - the central line correction is still as good as 1/170 wave P-V, and the off axis correction remains practically identical.
Ceravolo's all-spherical Gregorian
The original design is for 1m aperture with a very fast f/1.5 primary mirror. Design here is downscaled both, in aperture size and primary's
(and final) focal ratio, to make it more suitable for the amateurs' environment, and to make it comparable to other telescope types here
(it is, however, better suited to larger apertures, for better field quality, and for keeping central obstruction smaller). It consists of two
spherical mirrors and four small single lenses, yet its performance is comparable to that of the Celestron Edge systems, which in addition uses
a full aperture Schmidt corrector. The ray spot plots and diffraction images speak for themselves.
The disadvantage vs. SCT systems with as fast primary is its longer tube, although most of the extra length could be limited to some form of extended secondary housing/baffle, making the O.T.A. less balky. There would be, however, little diffrence in this respect vs. Cassegrain-Maksutov systems.
Unusual sub-aperture corrector...
interesting idea from amateurs' circles can be used for larger and
faster systems. It places sub-aperture Schmidt corrector at the focus of
the primary, in the converging cone from the secondary. Therefore, it is
Gregorian arrangement with Schmidt corrector between two concave
mirrors. It allows for
spherical primary, but corrected coma still requires aspherizing the
secondary, although considerably less than in a comparable SCT. The corrector is
significantly stronger than the full-aperture version, but it is also
significantly smaller. Corrector's depth and amount of spherochromatism
induced are similar for both. The spherochromatism is nearly doubled
versus comparable SCT; since it changes inversely to the third power of
the primary's F-number, an ~f/2.4 primary would be necessary to reduce
spherochromatism in this system to the level of a commercial SCT of
similar aperture. Another option is making achromatic corrector, which
practically eliminates spherochromatism.
As shown to the left, chromatism is not
intrusive in 8" aperture SGT with single-glass sub-aperture corrector
It is at the level of 4" f/70 doublet achromat. Achromatizing it with a
crown/flint combination with three identical Schmidt surfaces (the one
on the flint element is inverse Schmidt surface) reduces
spherochromatism several times, and may be desirable for larger
Further reduction of spherochromatism is possible with separated, much
more strongly aspherised Schmidt elements. Since more strongly curved
Schmidt surface also induces more of coma, a compact aplanatic Gregorian
with both mirrors spherical can be achieved. As this
advanced design by Mike I. Jones shows, the chromatism also has
nearly vanished. The downside is over 50% greater astigmatism, and fabrication difficulty
of very strong double Schmidt corrector: in that
respect, its stronger element is comparable to a
corrector for ~f/0.5 standard Schmidt system.
Obviously, the aberration calculation is, in
general, considerably more complex for sub-aperture lens corrector, as
opposed to a full-aperture lens corrector, mainly as a result of
displaced aperture stop, especially when more than a single element
(e.g. single sub-aperture meniscus lens) is required.
In principle, sub-aperture corrector is capable of
correcting any single aberration. The difficulty arises from it tending
to generate significant multiple aberrations, which may be difficult to
match with the aberrations of the rest of the system. Often times,
strongly curved surfaces are required, generating significant
higher-order aberrations, and/or setting very tight fabrication/collimation
tolerances. This is generally less of a problem with more relaxed
full-aperture correctors, which also can be used to
manipulate main mirror's off-axis aberrations by varying the stop location. For that reason, most of quality catadioptric
telescopes are made with full-aperture correctors, despite their often
higher cost. To those most common in amateur telescopes
will be given consideration in the following pages.
Obviously, the aberration calculation is, in general, considerably more complex for sub-aperture lens corrector, as opposed to a full-aperture lens corrector, mainly as a result of displaced aperture stop, especially when more than a single element (e.g. single sub-aperture meniscus lens) is required.
In principle, sub-aperture corrector is capable of correcting any single aberration. The difficulty arises from it tending to generate significant multiple aberrations, which may be difficult to match with the aberrations of the rest of the system. Often times, strongly curved surfaces are required, generating significant higher-order aberrations, and/or setting very tight fabrication/collimation tolerances. This is generally less of a problem with more relaxed radii-wise full-aperture correctors, which also can be used to manipulate main mirror's off-axis aberrations by varying the stop location. For that reason, most of quality catadioptric telescopes are made with full-aperture correctors, despite their often higher cost. To those most common in amateur telescopes will be given consideration in the following pages.