telescopeѲptics.net
▪
▪
▪
▪
▪▪▪▪
▪
▪
▪
▪
▪
▪
▪
▪
▪ CONTENTS
◄
10.2.2.3. SchmidtNewton telescope
▐
10.2.2.4.1. SCT offaxis
aberrations
► 10.2.2.4. SchmidtCassegrain telescope (SCT)Among the most popular commercial designs, the SchmidtCassegrain telescope (or SCT, FIG. 174) owes its success mostly to the possibility of relatively inexpensive commercial production of a wellperforming Schmidt corrector, particularly in combination with two spherical mirrors. The road for the SCT commercial production was paved by Celestron's Tom Johnson who, back in the '60ties, pioneered the method for corrector's massproduction.
FIGURE 174: SchmidtCassegrain telescope is a Cassegrainlike twomirror system combined with a fullaperture Schmidt corrector. Various combinations of corrector separation and mirror conics are possible, with somewhat different image field properties. Prevailing commercial arrangement is a compact design with fast spherical primary and usually also spherical secondary mirror, resulting in ~ƒ/10 system. Allspherical SCT is corrected only for spherical aberration, with low astigmatism, as well as relatively strong field curvature and coma remaining. The corrector also induces low level spherochromatism, undetectable visually and negligible for most photographic applications. Optical effect of the corrector on the system parameters is small, but not negligible. It slightly increases the marginal ray height on the primary, as determined by its refraction angle δ (Eq. 107), with this ray being then directed toward a different focus focus point, as a result of corrector's interference. With, say, 200mm ƒ/2 spherical primary, combined with a 0.707 neutral zone corrector at σ1=0.4R1 (primary's radius of curvature) in front of it, marginal ray on the primary will be only ~0.23mm higher (for ~0.71 corrector power in an allspherical arrangement). The two, corrector and primary, "act" as a prolate ellipsoid (K~0.71), nearly 200.5 mm in diameter, with only slightly extended marginal focus. Since it still retains ~29% of the original D(mm)/32F longitudinal spherical aberration, in order to find out secondary magnification we need to trace the 0.707 zone ray, the only one whose height and orientation after passing the corrector and primary didn't change, and to whose focus the rest of rays will be directed after reflection from the secondary. Taking the 0.707 ray as marginal, the primary becomes 141.4mm diameter ƒ/2.79 mirror (the 0.707 ray focuses at the mid point of the original longitudinal defocus, 1.56mm inside the primary's paraxial focus). Slightly shorter focal length  and the corresponding radius of curvature  increase the effective secondarytoprimary radius of curvature ratio ρ from 0.3125 (in an ƒ/2/10 mirrorsonly system with paraboloidal primary) to 0.3137, with the relative ray height at the secondary in units of the aperture radius k reduced from 0.25 to 0.2471, and the resulting secondary magnification m reduced to ~4.7. Applying this magnification value to the effective 200mm ƒ/1.992 primary results in a final ƒ/9.38 system. So, if the two mirrors without corrector would form an ƒ/10 system, optical effect of the corrector changes it into ~ƒ/9.4. In order to have an ƒ/10 system with an ƒ/2 primary, the secondary needs to be slightly more (~1.5%) strongly curved, thus with the R2/R1 radii ratio ρ~0.308, for the secondary magnification m=~5.05. The relative back focal distance in units of the primary focal length is only slightly reduced, from 0.5 to η~0.49.
Aberrationwise, there are two
significant differences between the SCT and allreflecting Cassegrain
varieties. One is that the SCT can be made free from both, coma and
astigmatism, while an allreflecting arrangement can only correct for
one. On the other hand, the Schmidt corrector induces some spherochromatism.
Follows overview of SCT axial aberrations, spherical (as a sum of
spherical aberration contributions
of its three elements) and spherochromatism. SCT spherical aberration The only significant monochromatic aberration introduced by the Schmidt corrector in collimated light is spherical. Its purpose is to offset spherical aberration on the two mirrors, resulting in a sphericalaberrationfree system. Thus, the PV wavefront errors for lowerorder spherical aberration at the best focus for an SCT system can be written as:
with scr being the corrector spherical aberration coefficient, d the pupil (aperture) radius and the mirror aberration coefficient sM being the sum of the individual mirror spherical aberration coefficients, sM=s1+s2. The individual mirror coefficients for object at infinity are same as for a twomirror system alone (Eq. 9.2 and Eq. 9 for the primary and secondary, respectively), given by:
for the secondary, with K1 being the primary conic, R1 the primary radius of curvature, k the height of marginal ray at the secondary in units of the aperture radius, m the secondary magnification and ρ=R2/R1, the secondary radius of curvature in units of R1. Note that in order to be able to directly add the two coefficients, the secondary aberration coefficient had to be corrected for the difference in apertures by multiplying it with k4 factor, the relative height of marginal ray at the secondary in units of the ray height at the primary. The two forms for the secondary aberration coefficient have parameters interchangeable through k/ρ=kR1/R2=(m1)/m=1(1/m). Thus, the system PV wavefront error at the best focus can be written as:
with P being the needed corrector power to cancel system spherical aberration, and ss={}/4R13 being the system aberration coefficient. Of course, for zero system spherical aberration, the aberration coefficient for the corrector scr, which is related to the corrector power P as scr=P/4R13, needs to be equal to the sum of mirror aberration coefficients sM, and of the opposite sign. If the primary is spherical, to cancel its aberration alone, the corrector aberration coefficient needs to be scr=b/8 (with the aspheric term b=2/R13, it comes to scr=1/4R13, same as the spherical primary, but of the opposite sign). The corrector with this value of the aspheric term is said to have a unit power P. In such arrangement, for cancelled spherical aberration of the system, the secondary mirror conic needs to be K2=[(m+1)/(m1)]2, same as in the classical Cassegrain. With both, primary and secondary spherical (K1=K2=0), needed power P of the corrector for zero system spherical aberration is (from Eq. 113.1) P=1k(m1)(m+1)2/m3. For the typical ƒ/2/10 SCT with k~0.25 and m~5, P~0.71, i.e. needed corrector strength, or depth, is about 71% of that needed to correct the primary alone. In terms of the Fratio, this corrector has the strength needed to correct some 12% slower primary. In general, for any combination of conics, needed corrector power to cancel spherical aberration of two mirrors is determined by a value of the sum of opposite aberrations contributions of the primary and secondary relative to spherical aberration of the primary alone. Thus, it can be written as P=1(s'2/s'1), with the aberration contribution of the secondary s'2 in proportion to k[K2+(m+1)2/(m1)2](11/m)3, and aberration contribution of the primary s'1 proportional to (K1+1). The prime notation is to differentiate the proportionate relative contributions from the corresponding actual aberration coefficients s1=s'1/4R13 and s2=s'2k4/4R23. Thus, the lowerorder aspheric parameter A1 for the corrector in a SchmidtCassegrain system can be, analogously to the Schmidt camera, written as A1=b/8(n'n), but with the corresponding aspheric coefficient b changed in proportion to the needed corrector's power, as b=2P/R13. Reduction of the 5th order aspheric parameter of the SCT corrector, A2, relative to the value for primary alone, is typically greater than that of A1, due to significant higherorder spherical aberration of opposite sign generated at the secondary as a result of relatively close object (i.e. image of the primary) distance, as well as due to reduction in the higherorder aberration resulting from reduced corrector separation (i.e. height of marginal ray at mirror surface). For spherical secondary and typical 8" ƒ/2/10 SCT configuration with σ~0.4, the parameter, given by A2=b'/16(n'n), with the higherorder aspheric coefficient b' approximately 1/6 of that needed for primary alone (with the stop at the center of curvature), or b'~[1(k6/ρ5)]/R15. Thus, the higherorder corrector's power in the typical commercial unit is only ~0.16 of that needed to correct higherorder spherical aberration of a comparable ƒ/2 Schmidt system. The parameter changes for different values of σ1 approximately in proportion to σ1/0.4, thus the generalized approximation for b' can be written as b'~2.5σ1[1(k6/ρ5)]/R15. For closer objects, spherical aberration coefficients for all three, corrector, primary and secondary change (it is negligible for the corrector), disturbing presumed nearzero balance for distant objects, and resulting in spherical aberration. The chage of aberration contribution on the two SCT mirrors is similar to that in all reflecting twomirror systems (Eq. 92). Main difference is with SCT systems that focus by moving the primary. Here, the error induced by a relatively small object distance is in part offset by undercorrection induced by refocusing, which requires an increase in mirror separation. More specifically, reduced object distance lowers
undercorrection of the primary, and increases overcorrection of the
secondary. That makes the system overcorrected; the increased
mirror separation needed to bring the focus point to its fixed location
diminishes the
effective diameter of the secondary, reducing overcorrection induced by
it, and by that the overall system overcorrection as well. This
makes a typical commercial SCT better suited for terrestrial
observations than a similar system with fixedmirror focusing. More
details on this subject are given in
11.5.2. SCT focusing errors. SCT spherochromatism Spherochromatism in the SCT originates at the corrector, whose corrective power is optimized for one  usually green/yellow  wavelength. Since shorter wavelengths refract more strongly, and the longer ones refract more weakly, the effective corrector power increases toward the former, and decreases toward the later. With the combined spherical aberration of the two mirrors being undercorrection, this means that shorter wavelengths (blue/violet) will be overcorrected, and the longer ones (red) undercorrected. This wavelengthdependant spherical aberration increasing with the refractive index differential vs. optimized wavelength is the only source of chromatism in a SCT. Given aperture and F#, SCT spherochromatism is proportional to the relative power of the Schmidt corrector P. In other words, to the relative value of the aspheric term b needed to cancel spherical aberration of the system. It can be written as:
with bs being the aspheric factor  or the corrector's spherical aberration coefficient  needed to correct for spherical aberration of the primary alone. As mentioned, b=2/R13, from the general form of the aspheric coefficient b=2n[(m+1)/(m1)]2/R13, for mirror magnification m=0 (object at infinity) and index of incidence n=1. Aspheric coefficient cancelling the aberration of a spherical mirror is bs=b/8=1/4R13, while that for an SCT system, equal to its aberration coefficient scr, is bSCT=P/4R13, where P is the corrector power, positive in sign. The PV wavefront error of spherochromatism for a particular SCT arrangement is obtained by multiplying relative power of its corrector (Eq. 118) with the wavefront error for the unit power corrector (Eq. 106). For the transverse aberration (ray spot diameter), the relative power is to be multiplied with the transverse aberration for the unit power corrector (Eq. 107.1) and the SCT secondary mirror magnification. In general, SCT spherochromatism is low. For a typical commercial ~ƒ/2/10 version, with both mirrors spherical, k~0.25, σ~0.4 and m~5, relative corrector power ~0.72, and 0.866 neutral zone placement, the red (Cline) and blue (Fline) geometric blurs are still within the Airy disc. For the 0.707 radius neutral zone placement (FIG. 175), the blurs are doubled, but the wavefront error halves for the lowest chromatism level achievable with the Schmidt corrector.
Residual spherical aberration in the system will alter spherochromatic error due to the increased error in the optimized wavelength (FIG. 176).
FIGURE 176: Residual
spherical aberration in the optimized wavelength of an SCT
affects correction in all other wavelengths as well. Nonoptimized wavelengths with spherical aberration
at nearperfect correction of
identical sign to the The overall correction level is nearly certain to be worse, not only due to the error in the optimized wavelength, to which (and those relatively close to it ) the eye is most sensitive. As the plot at right shows, the wavelengths with initially the opposite error sign (red), may only switch the sign, without major error decrease. This particular SCT would show noticeably more color in the blue/violet than when optimally corrected. Since an SCT nearperfectly corrected for spherical aberration have blue wavelengths overcorrected, and red wavelengths undercorrected, a residual of, say, 1/4 wave PV wavefront error of overcorrection in the optimized wavelength will increase spherochromatic error in the blue, and reduce it in the red (the plots are for a typical ƒ/2/10 8inch SCT with spherical mirrors). If the residual spherical is relatively significant, spherical correction in the red is likely to be actually better than in the optimized wavelength. Consequently, the instrument will have more or less pronounced chromatic imbalance, with the negatively affected portion of the spectrum (blue/violet wavelengths in this example) possibly showing noticeably inferior chromatic correction in both, visual observing and imaging. Follows an overview of the SCT offaxis aberrations. ◄ 10.2.2.3. SchmidtNewton telescope ▐ 10.2.2.4.1. SCT offaxis aberrations ►
