Reflecting Telescope Optics I: Basic Design Theory and its Historical Development (Astronomy and Astrophysics Library) (Pt. 1)
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Complete compendium on the physics and applications of telescope optics, underlying the original and oldest of astronomical instruments.
Thoroughly scholarly work that provides both the historical perspective and the state-of-the-art technology, such as the 4-lens corrector of Delabre and the LADS corrector.
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At I2 . If the emergent ray r is projected to meet the projection of the incident ray r, parallel to the axis, the plane P where they intersect is the image-side principal plane of the total system, which is no longer at inﬁnity. The eﬀective focal length is f . Since it is measured from P to I2 , it is negative. The focal length f will determine Fig. 2.9. Image principal plane in the defocused telescope of Fig. 2.8, producing a real image at I2 40 2 Basic (Gaussian) optical theory of.
As represented by Eq. (3.11). The theory of § 3.2.4 above is limited to the second term of this equation, known as the third order, or Seidel, approximation. With steep apertures or signiﬁcant ﬁeld sizes, the third order approximation remains of immense value for understanding the basic correction potential of a given design, but is no longer adequate to describe the ﬁnal image quality. Furthermore, departures may be necessary from the strict conic sections deﬁned by (3.11) in order to compensate.
Null-test (RTO II, Chap. 1) in the classical case. The supplement for the secondary amounts to about 14% in the cases of Table 3.2 with m2 = ±4. It increases rapidly for smaller values of m2 . It is important to note that, while the aplanatic forms of the secondaries are still hyperbolae or ellipses to a third order, these conic sections are no longer such that the foci are at the primary and 3.2 Characteristic Function and Seidel (3rd order) aberrations 97 secondary images, as is the case.
Of the three aberrations C1 (longitudinal chromatic aberration), SI (spherical aberration) and SII (coma). It should be borne in mind that, once SI and SII are corrected, the stop-shift formulae (3.22) and (3.213) show that, to the third order approximation, SI , SII and SIII are independent of the stop position. The stop-shift term for C2 , given in brackets in Eqs. (3.223), shows that this is also true of C2 because C1 is corrected. It follows that we can draw a very important conclusion for.
However, for the systems dealt with in § 22.214.171.124 below consisting of an aspheric plate and one or two mirrors (aspheric in the general case), the analytical equations derived in the general theory above provide a simple and powerful basis for complete understanding of their optical properties. A complete treatment of the systems proposed and investigated in the past 50 years would itself require a whole book. The purpose of the account given in this section is to describe the characteristics of.