You should be able to see objects with an absolute magnitude lower than L m. L m = 2 + 5×log(D o) - Star magnitude limit. Remember, it's only the perceived brightness, not the absolute one. SB = 2 × D ep² - Surface brightness, given as a percentage of the maximum light intensity per unit area. The higher the magnification, the tinier the area you can observe.ĭ ep = D o / M - Diameter of the exit pupil, the light beam which exits the scope via the eyepiece forms the so-called exit pupil. Practically, the smaller the resolving power, the better.įOV s = FOV e / M - Scope field of view, analogical to the FOV e, but this is the overall part of the sky which can be seen as a combination of the objective and the eyepiece. Two adjacent point sources are resolved by the. Because of diffraction even an aberration-free optical system images a point source not as a point but as an Airy pattern, whose central area is called the Airy disk. In other cases, they blur into one, becoming a single object. This calculator computes the diffraction-limited angular resolution of an optical system, such as a telescope or the human eye. We can distinguish two bodies that are separated by an angle greater than P r. You can read more about this topic in our angular resolution calculator. P r = 115.8" / D o - Resolving power (or angular resolution), given in arcsec. Fortunately, this telescope magnification calculator will do the job for you! These are: Out of these basic parameters, we can evaluate several different features which tell us about the quality of the image. The bigger the value, the greater the fraction of the sky you can analyze at once. FOV e - Eyepiece field of view, this is the area described by the angle which is viewable from your point - in this case, using the eyepiece.You can simply make changes to image properties by choosing an eyepiece with another focal length. ![]() ![]() As D o and f r are usually fixed to the scope (as is the focal length of the telescope), the eyepiece is a changeable element.
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