NDLI: Figures of Merit for Light Bucket Mirrors

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Figures of Merit for Light Bucket Mirrors

Content Provider	Semantic Scholar
Author	Holenstein, Bruce Douglas Mitchell, Richard J. Koch, R. H.
Copyright Year	2010
Abstract	Introduction Aberrations of the surface of a mirror have multiple expressions. “Light bucket” mirrors challenge traditional Gaussianand diffraction-oriented aberration theory due to large amplitude, caustic ray-crossing aberrations. Typical light bucket mirrors may be made of metal, epoxy, foam glass, tessellated segments, and other techniques (Genet 2009) and have many waves of aberration. What is needed is a method to characterize the suitability of light bucket mirrors for an intended purpose, whether that be diaphragm-limiting photometry, lunar occultations, intensity interferometry, Cherenkov radiation detection, or other non-astronomical uses such as solar power collection. (Note that we utilize the familiar alternate term “diaphragm” to signify the typically circular isolator located in the focal plane before a photomultiplier cell or photodiode detector. The word “aperture” has too many astronomical uses.) A mirror surface that will satisfy an astronomical observing program will collect photons from the stellar or other program object and deliver them to the detector, yet exclude enough foreground/background photons so as to yield an acceptable signal-to-noise ratio (SNR). Herein several figures of merit are developed for light bucket mirrors dedicated to astronomical use. We intend this chapter to be the theoretical, analytical background for our second chapter that follows in a later section of this book (Holenstein et al. 2010), and also a general contribution which applies to all highly aberrated mirrors.
File Format	PDF HTM / HTML
Alternate Webpage(s)	http://gravic.com/graviclabs/pdf/papers-altz/Alt%20Az%2016%20Holenstein-FigMerit.pdf
Language	English
Access Restriction	Open
Content Type	Text
Resource Type	Article

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