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Figure 1: Schematic layout of a White-light Interferometer. A CCD image sensor like those used for digital photography is placed at the point where the two images are superimposed. A broadband “white light” source is used to illuminate the test and reference surfaces. A condenser lens collimates the light from the broadband light source.
Figure 3. White light interferometric microscope. White-light interferometry scanning (WLS) systems capture intensity data at a series of positions along the vertical axis, determining where the surface is located by using the shape of the white-light interferogram, the localized phase of the interferogram, or a combination of both shape and phase.
From an astronomer's point of view, it is a simple matter of installing the ASCOM platform and suitable client software; no programming is required. ASCOM drivers allow computer-based control of devices such as planetarium software to direct a telescope to point at a selected object. Using a combination of mount, focuser and imaging device ...
DHM performs static measurements of 3D surface topography as many other 3D optical profilometers (white light interferometers, confocal, focus variation, ... ). It enables to retrieve, roughness and shape of many surfaces. [32] [33] [34] Use of multiple wavelengths enable to overcome the l/4 limit of traditional phase shifting interferometers ...
Siril is a software application for astrophotography, which allows pre-processing and processing of images from any type of camera (CCD, planetary camera, webcam etc.). The images must be converted to 32-bit FITS format which is the format used natively by Siril.
The signal can be acquired with a camera in wide-field operation (a, b) or by point detection in confocal arrangement (c, d). Interferometric scattering microscopy ( iSCAT ) refers to a class of methods that detect and image a subwavelength object by interfering the light scattered by it with a reference light field.
Kepler Mission space photometer. In astronomy, photometry, from Greek photo-("light") and -metry ("measure"), is a technique used in astronomy that is concerned with measuring the flux or intensity of light radiated by astronomical objects. [1]
This allows the camera to use a longer exposure and/or a longer focal length lens or even be attached to some form of photographic telescope co-axial with the main telescope. Telescope focal plane photography. In this type of photography, the telescope itself is used as the "lens" collecting light for the film or CCD of the camera.