The spatial or angular resolution of a telescope is the smallest angle between two point objects that produces distinct images. It depends on both the wavelength at which observations are made and on the diameter, or aperture, of the telescope. This minimum angle can be given by the Rayleigh limit:
When the angular separation of two stars is very small, it might be thought that the use of a large enough aperture or high enough magnification would always resolve the light into two distinct images. Because of diffraction effects however, the image of each star is not a point of light but a disk (see Airy disk). If the two disks substantially overlap then increased aperture or magnification merely gives a larger blur of light, and the telescope has not sufficient resolving power to separate the images. The stars will just be resolved, however, when their Airy disks touch. This gives the Dawes limit. Two stars are at a telescope's Rayleigh limit when the center of the Airy disk of one star falls on the first dark ring of the diffraction pattern of the other. The illustration shows the images of two stars of equal magnitude separated by 0.8 seconds of arc. Viewed under perfect seeing conditions with a 7.5-cm aperture (right) they are not resolved; with 15-cm (center) they are just resolved and with 30-cm (left) they are clearly separated.
The discovery of Pluto's satellite Charon in 1978 shows that the Dawes (or Rayleigh) limit cannot be too strictly applied. Although well above the limiting angle for large telescopes, Charon had not been resolved; it was detected as an elongated photographic image. This is partly because of the difference in brightness and because Pluto is not a point source, but mainly because poor seeing prevented the larger-aperture telescopes from reaching the limiting angle. The distorting effects of the Earth's atmosphere are greatly reduced in telescopes with active or adaptive optics, and are removed in orbiting telescopes. Very high spatial resolution is thus now feasible.
In radio astronomy, where the same formulae for spatial resolution apply but where very much greater wavelengths are studied, apertures maybe 30 times greater than those used in optical telescopes can only give poor resolution. The situation has been greatly improved by the use of aperture synthesis and very long baseline interferometry (VLBI).
Common Screen Resolutions |
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These are some of the resolutions commonly found on monitors. The higher the resolution, the more information (pixels) can be displayed on screen at one time. For a complete list, see screen resolution. |
Common Screen Resolutions |
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These are some of the resolutions commonly found on monitors. The higher the resolution, the more information (pixels) can be displayed on screen at one time. For a complete list, see screen resolution. |
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