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Cassegrain configuration

Figure4.8 shows the collecting telescopes configuration. Each consists of a pair of focal parabolas (primary Ml, secondary M2) used in a Cassegrain configuration, plus a fold flat used for coarse beam steering (M3). The design is based in NASA s SPIRIT proposal (Wilson et al. 2007). After the beam steering mirror the light is... Figure4.8 shows the collecting telescopes configuration. Each consists of a pair of focal parabolas (primary Ml, secondary M2) used in a Cassegrain configuration, plus a fold flat used for coarse beam steering (M3). The design is based in NASA s SPIRIT proposal (Wilson et al. 2007). After the beam steering mirror the light is...
The angular (spatial) resolution of a telescope, or of any optical system, is ultimately limited by diffraction. As an example, we calculate these limitations for an instrument with a Cassegrain telescope however, the theory is directly applicable to other configurations as well. [Pg.166]

See other pages where Cassegrain configuration is mentioned: [Pg.389]    [Pg.483]    [Pg.212]    [Pg.57]    [Pg.163]    [Pg.297]    [Pg.389]    [Pg.483]    [Pg.212]    [Pg.57]    [Pg.163]    [Pg.297]    [Pg.247]    [Pg.8]    [Pg.7]    [Pg.344]    [Pg.142]    [Pg.163]   
See also in sourсe #XX -- [ Pg.483 ]



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Cassegrain

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