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In the applet above, we show only this secondary mirror.
The primary reflection mirror adopts paraboloidal mirror; the secondary mirror adopts hyperboloidal or ellipsoidal mirror.
The collection optics consists of primary mirror, secondary mirror, relay optics, and fiber collection optics.
Significantly, using the aberration-based design method, the secondary mirror only required 15 µm of freeform departure; whereas, the conventional method produced a secondary mirror with 165 µm of departure an increase of more than an order of magnitude.
This eliminates the extra diffraction caused by the secondary mirror and causes an increase in image contrast and sharpness.
The advantages of using CFRP for the secondary mirror support structure of the European overwhelmingly large telescope are discussed.
This dependency and its effect on heat loss and secondary mirror temperatures are analyzed for three different LFC receiver configurations.
Two Cassegrain telescopes of a spherical primary mirror with the Golay3 configuration and with an aspherical secondary mirror were designed.
The remaining heat flux by the edge of focal spot is directed by the secondary mirror for electric generation.
Heat loss prediction models for parabolic trough receivers do not consider the thermal effect of a secondary mirror.
The main mirror will reflect the ancient starlight it detects onto a 4m-wide secondary mirror before it goes on to hit the detectors.
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