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If you have special requirements, we are able to develop custom OCR SDK to fit ... Yunmai Technology , a top-ranking global provider of high-end OCR (aka, ... A basic stellar polarimeter comprises a modulator and detector system The units are usually mounted within a box for attachment to the telescope This self-contained polarimetric head may provide observer support devices such as retractable transfer optics for inspection of the telescope image prior to the measurements Instruments using photomultiplier detectors require the use of a eld stop or eld-limiting diaphragm, in similar fashion to a regular photometer According to Pospergelis (1965), the eld stop must have a knife edge of strictly circular shape, with minimal re ecting surface at its edge The aperture should be made with non-metallic material such as ebonite, and the beam must pass through the hole symmetrically If these conditions are not met, spurious linear polarization of up to 01% may arise The simplest form of modulator is a rotatable polarizer prior to a detector As described at the beginning of the chapter, an early polarimeter of this type, used by Hiltner (1951a), was a standard photometer with a Polaroid inserted whose orientation was adjustable to selected positions In a system described by Hall (1951), a continuous rotating Glan Thompson rism was employed With this instrument, the probable error of the measurements was typically 02%, one of the chief problems being atmospheric intensity scintillation noise A pioneering double-beam polarimeter using a Wollaston prism was constructed by Gehrels & Teska (1960) The output signals for the two channels with photomultiplier detectors were simply recorded by DC ampli ers and pen recorder systems An early design of double-beam polarimeter was also used by Serkowski & Chojnacki (1969) The system comprised a Wollaston prism, with further separation of the resolved components by the apex of an aluminized 97 prism The instrument was rotatable in steps of 45 on the telescope mounting plate Signals were obtained from photomultipliers illuminated via Fabry lenses so that the telescope pupil was imaged on them Difference signals were recorded, and detector imbalances were calibrated using a depolarizer Many of the early instruments involving stepped rotation of wave plates or polarizers were controlled by hand As computer control became an eventuality, such operations were performed by using stepper motors An early automated system was described by Kinman & Mahaffey (1974), this being similar to the design of Visvanathan (1972) In order to reduce sky background contamination that is prevalent at high latitude observatories, Piirola (1973, 1975) designed an instrument with built-in compensation Two diaphragms were placed in the focal plane of the telescope and by a mechanical chopping arrangement, the detector was alternatively illuminated by star plus sky background and then just by an equal area of the sky alone; in this way the contaminating signal from the sky was automatically subtracted The same principle was also incorporated by Korhonen, Piirola & Reiz (1984) and Piirola (1988) in a more sophisticated instrument allowing simultaneous ve-band multi-colour observations. epson scan 2 ocr component download: Download OCR Software - SimpleOCR ocr sdk forum ABBYY FineReader - Download
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