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As terrestrial and spaceborne astronomical telescopes advance in multi-functional design sophistication,
incorporating greater spectral resolutions, the utilization of curved focal plane ccd and cmos imaging
detectors, contoured to match the telescope's Petzval field of curvature, provides a fundamental and novel
optical simplicity facilitating new imaging frontiers in astronomical research. For space based telescopes,
curved focal plane detector devices require significantly fewer optics than their flat counterparts, which
require field flattening optics, in achieving maximum imaging resolutions for adjoining spectrometers or
imaging cameras. consequently, with fewer optics comes greater room to place other optics within the same
space to accomplish other tasks, providing much greater diversification of observing functions and techniques
reserved simultaneously for the telescope. Included within this is the operational capability of producing
multi-wavelength spectrometers gathering data concurrently at a multitude of selected wavelengths, with
greater sensitivity, reliability, size reduction, and operational longevity of the restructured optical system.
Specialized applications involving optical interferometry are also achievable with further enhancements when
the curved detectors are applied specifically to refine or maximize detection of fringes, and when employing
occulting mask algorithms for existing light paths. for planetary surface mapping space probes, curved focal
plane detection provides real-time 3D multi-perspective image acquisition for streaming 3D data sets,
replacing onboard or remote computationally intensive 3D reconstructions used for examining terrestrial
surface features performed with corresponding flat detectors. For earth based telescopes, where mass of the
telescope's optics are not so constrained, more degrees of freedom are also part of the benefits introduced by
curved focal plane detector device optimization. Associated with the very large Petzval radii of curvature for
very large and extreme telescopes within this class are wide field spatial distortions which are instantaneously
corrected when arrays of curved CCD's or CMOS devices are joined homogeneously and precisely together
along the converging field of curvature, without field flattening optics, insuring complete full field detection
superior to flat facet detectors which compromise the telescope's imaging field curvature detection abilities.
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