A telescope consists of two main elements, an objective and an eyepiece. The objective is usually a mirror, or a lens, that focuses the incoming light of the observed object. The eyepiece is a set of lenses that corrects the direction of the beam and lets you get closer to the image. Learn more about how the eyepiece affects your skywatching experience with our telescope field of view calculator.

Lm = 2 + 5×log(Do) - Star magnitude limit. You should be able to see objects with an absolute magnitude lower than Lm. Remember that luminosity is a logarithmic function, and lower values mean brighter objects!

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Want to read more? We highly recommend Randy Culp's presentations, where he explains all of the equations and other interesting features in detail.

Our tool is straightforward: just look at your scope and input all the necessary values. Let's take a look at an example:

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The second thing is that the objective collects the light from its whole surface (also known as the aperture) and processes it through the much smaller surface of the eyepiece. The same amount of light enters and exits the telescope, so the image is not only magnified but also has its brightness increases significantly! This effect is amplified in the highest-powered telescopes, which is why they are able to detect exoplanets.

FOVs = FOVe / M - Scope field of view, analogical to the FOVe, but this is the overall part of the sky which can be seen as a combination of the objective and the eyepiece. The higher the magnification, the tinier the area you can observe.

This is the telescope magnification calculator, a great tool that helps you set your scope for both amateur and professional astronomical observations. In the article below, you can find the answer to the question: How does a telescope work? as well as learn about the magnification equation of a scope.

Dep = Do / M - Diameter of the exit pupil, the light beam which exits the scope via the eyepiece forms the so-called exit pupil. The diameter tells about its size.

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However, some of these values are approximations because they relate to the size of the eye's pupil. We assume that it's around 7 mm in a dark environment, but that likely varies from person to person and generally decreases with age. It's also worth noting that atmospheric disturbances, in particular overcast weather, may lower the quality of the images.

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Pr = 115.8" / Do - Resolving power (or angular resolution), given in arcsec. You can read more about this topic in our angular resolution calculator. We can distinguish two bodies that are separated by an angle greater than Pr. In other cases, they blur into one, becoming a single object. Practically, the smaller the resolving power, the better.

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As you can see, the magnification of the telescope gets greater when the focal length of the objective increases or when the eyepiece's focal length decreases.

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We've mentioned the objective and the eyepiece above. Focal lengths or focal diameters can characterize both. The magnification equation of a telescope is then:

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While magnification is an essential feature of a telescope, it isn't the only thing you should consider checking while choosing a device for observations. In general, telescopes may have numerous measures and symbols, but we can distinguish a few which may be handy in determining the possible image properties:

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Out of these basic parameters, we can evaluate several different features which tell us about the quality of the image. Fortunately, this telescope magnification calculator will do the job for you! These are:

What's more, you'll find not only how to calculate magnification but some other interesting image properties to look for. Get ready, and be well prepared for your next stargazing activity!

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As we know the general concept of how a telescope works, we can take a step further and ask: How to calculate magnification?

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You must have seen a lot of beautiful pictures of galaxies, nebulae, and planets taken by both huge, high-powered telescopes and small, home-used ones. Have you wondered how it's possible to see such distant objects and scale up their images to see that much detail smoothly? Here is how it works:

The focal length of the objective usually goes hand in hand with the length of the telescope itself. That's the reason why the highest-powered telescopes are such monsters with huge mirrors. The biggest ones are actually made of several hexagonal tiles.

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SB = 2 × Dep² - Surface brightness, given as a percentage of the maximum light intensity per unit area. Remember, it's only the perceived brightness, not the absolute one.