17:
89:
Another advantage of either the basic Dall-Kirkham or the
Modified Dall-Kirkham design is that collimation of the convex spherical secondary mirror with respect to the optical axis of the primary mirror is almost trivial, because there is no single defined axis of a sphere. Any line that runs
86:. The performances are equal or better than the Ritchey-Chrétien telescope. The spherical secondary can be fringe tested against a spherical concave surface or tested from behind. This is markedly an advantage over the hyperbolic secondary of the Ritchey-Chrétien design.
63:
is slightly different from that for a conventional Dall-Kirkham and must be optimized along with the lenses during design. The usable field is much better than the
79:) if the corrector is made of quartz. (With a corrector, the Ritchey-Chrétien System also has a better and bigger field.)
64:
127:
99:
44:
111:
60:
52:
16:
121:
76:
48:
83:
67:
without corrector, and over very wide spectral bands, typically 380 to 950
68:
36:
28:
32:
40:
47:
configuration, but also includes a lens group (usually two or three
56:
15:
72:
20:
Dall-Kirkham reflecting telescope, built by Horace Edward Dall
82:
Such a telescope was designed by Rosin and Wynne after
90:through the center of the sphere can be an axis.
8:
7:
14:
1:
59:quality. The primary mirror
112:Le télescope de Wynne-Rosin
144:
65:Ritchey-Chrétien telescope
100:List of telescope types
51:elements) ahead of the
43:as in the conventional
21:
26:Modified Dall-Kirkham
19:
55:to improve off-axis
22:
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128:Telescope types
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117:
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11:
5:
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61:conic constant
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77:near infrared
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84:World War II
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45:Dall-Kirkham
35:primary and
31:utilizes an
25:
23:
53:focal point
106:References
71:(edges of
69:nanometres
39:secondary
33:elliptical
37:spherical
29:telescope
122:Category
114:(French)
94:See also
41:mirror
57:image
75:and
73:UV-A
49:lens
24:The
124::
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