How to convert starlight into knowledge?
Spectroscopy converts any faint light point of the skies into a database
C11 with flip mirror and LHIRES III spectrograph
CAD drawing of LHIRES III
Optical path of the slit spectrograph LHIRES III
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Wide spectrum of sunlight reflected by moon's surface measured from a distance of 8 light minutes
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Wide spectrum of Riegel (Beta Orionis) measured from a distance of 913 light years
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Sirius's spectrum (horizontal line) overlayed with a Neon calibration spectrum - see the broad H-alpha absorption line @ 656.2 nm (right side)
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Spectrum of the sun and its direct and uncalibrated scan - see Mg I Triplett (middle) and H-beta (outer left)
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Medium resolved (R = 15000) telluric lines (O2 band around 689 nm) in the sun's spectrum
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Wide spectrum of Beteigeuze and its direct and uncalibrated scan - see H-alpha & TiO / MgH molecular line bands
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Wide spectrum of Capella and its direct and uncalibrated scan, most prominent: Sodium (Na-D) & H-Alpha
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Jupiter's highly resolved reflected sunlight spectrum (H-alpha region) appears slightly tilted against earth's atmospheric lines due to the rotational speed and hence variing radial velocities along the equatorially oriented slit
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A scanned narrow portion around Na D lines shows the "fingerprint" of the element Sodium in the atmospheres of stars