Search results
Results From The WOW.Com Content Network
A simple two-element optical interferometer. Light from two small telescopes (shown as lenses) is combined using beam splitters at detectors 1, 2, 3 and 4.The elements create a 1/4 wave delay in the light, allowing the phase and amplitude of the interference visibility to be measured, thus giving information about the shape of the light source.
An astronomical interferometer or telescope array is a set of separate telescopes, mirror segments, or radio telescope antennas that work together as a single telescope to provide higher resolution images of astronomical objects such as stars, nebulas and galaxies by means of interferometry.
OSLO has been used in a multitude of optical designs including holographic systems, [1] anastigmatic telescopes, [2] gradient index optics, [3] off-axis refractive/diffractive telescopes, [4] the James Webb Space Telescope, [5] aspheric lenses, [6] interferometers, [7] and time-varying designs.
The distance between the radio telescopes is then calculated using the time difference between the arrivals of the radio signal at different telescopes. This allows observations of an object that are made simultaneously by many radio telescopes to be combined, emulating a telescope with a size equal to the maximum separation between the telescopes.
Aperture masking interferometry (or Sparse aperture masking) is a form of speckle interferometry, that allows diffraction limited imaging from ground-based telescopes (like the Keck Telescope and the Very Large Telescope), and is a high contrast imaging mode on the James Webb Space Telescope.
If a phase-shifting element is added to one arm of the interferometer, then the displacement it causes can be determined by simply counting the interference fringes, i.e., the minima. The Jamin interferometer allows very exact measurements of the refractive index and dispersion of gases ; a transparent pressure chamber can be positioned in the ...
Slow motion movie of the image seen at a telescope when looking at a star at high magnification (negative images). The telescope used had a diameter of about 7r 0 (see definition of r 0 below, and example simulated image through a 7r 0 telescope). The star breaks up into multiple blobs (speckles) -- entirely an atmospheric effect.
This technique works by superposing ("interfering") the signal waves from the different telescopes on the principle that waves that coincide with the same phase will add to each other while two waves that have opposite phases will cancel each other out. This creates a combined telescope that is the size of the antennas furthest apart in the array.