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To calculate the telescope FOV from focal length divide the eyepiece field stop (mm), or AFOV by the telescope’s focal length (mm), then multiplying by 57.3, as seen in the formula below.

How much you spend on a magnifier should be determined by the application for which it is being used. Buying the least expensive magnifier could lead to unsatisfactory and frustrating results. Any magnifier you buy should be a tool to fit the rigors of the environment in which it will be used. Additionally, it may be unwise to expect the same magnifier to satisfy the requirements of several functions. Below are several factors affecting the quality of the magnifier, as well as the function for which it is best suited.

The simple lens is a single positive lens. Simple lenses are satisfactory for work that requires only low power magnifiers, such as 2X or 3X reading magnifiers. Simple lens magnifiers distort color on the outer fringes of the image and thereby lose sharpness.

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Magnification in a telescope refers to the degree to which the image of an observed object is enlarged compared to the naked eye. It’s a crucial factor in observational astronomy as it affects the level of detail that is seen when observing celestial objects. Higher magnification allows for more detailed observation of smaller and distant objects, while lower magnification is better for larger or closer objects.

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The field of view (FOV) of a telescope is calculated using either the eyepiece field of view and magnification, or the diameter of the field stop and focal length. The most common method to calculate the true field of view (TFOV) is to divide the apparent field of view (AFOV) by magnification, as seen in the formula below.

Due to physical laws, the outer part of the image formed by a simple lens may appear out of focus. This is caused by the curvature of the lens. The greater the magnification - and the greater curvature of the lens - the greater the problem. This can be easily overcome by designing a magnifier that has more than one lens. A triplet has a "flat field" which means the entire area of view is in focus and undistorted.

The magnification in a telescope is determined by the focal length of the telescope and the eyepiece. To calculate the magnification, divide the telescope focal length by the eyepiece focal length. For instance, if a telescope has a focal length of 1000mm and is used with an eyepiece with a focal length of 10mm, the magnification would be 1000 / 10 = 100x. At 100x magnification, the field of view would be smaller than at 50x magnification, because magnifying an image presents a smaller portion of the sky. This allows for more detailed observation of smaller celestial objects.

A single lens is satisfactory for low powers. Higher power magnifiers require two or more lens elements for improved resolution and correction of chromatic or other aberrations.

The doublet lens is two simple lenses used in conjunction with each other but not cemented together. The doublet produces an image of better quality because it corrects some of the outer image color distortion.

Because of physical laws, the lens may produce a prism effect giving the image false color fringes known as chromatic aberration. Simple lenses focus various colors at different points. Achromats with two simple lenses cemented together correct this by causing many colors to focus at the same point.

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The FOV of an eyepiece is calculated using the formula: FOV = (Eyepiece field stop / Eyepiece focal length) x 57.3. The eyepiece field stop is the diameter of the image formed by the eyepiece, and the eyepiece’s focal length is the distance from the eyepiece to the point where it forms an image. The factor of 57.3 is used to convert the result from radians to degrees.

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The apparent field of view (AFOV) refers to the perceived expanse of the sky covered by the eyepiece, while the true field of view (TFOV) represents the actual segment of the sky visible through the telescope. To illustrate, an eyepiece with a broad AFOV will give the impression of a larger sky, but the actual TFOV is smaller due to the magnifying effect of the telescope.

The calculation of the TFOV involves dividing the AFOV by the magnification of the telescope. This calculation helps astronomers optimize their observations based on the specific characteristics of the celestial objects they wish to study.

The value 57.3 is used because there are 2π radians in a full circle of 360 degrees. Dividing 360° by 2π yields about 57.2958° per radian, allowing astronomers to calculate their TFOV in degrees. For example, a telescope with an eyepiece field stop diameter of 35mm, and a focal length of 1000mm will yield a 2.0055-degree TFOV. This equation is expressed as ([35 / 1000] x [57.3] = 2.0055).

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The maximum distance the eye can be from the magnifier and still provide a full field of view. Longer eye reliefs generally provide more comfortable viewing.

The FOV in the eyepiece is determined by its specific AFOV, and the choice of eyepiece thereby plays a vital role in the observational experience. The relationship between FOV and magnification is inversely proportional, such that an increase in magnification results in a narrower field of view, while a decrease in magnification yields a broader view.

The FOV is a crucial aspect of observational astronomy as it determines the range of celestial objects that can be observed. A larger FOV allows for the observation of larger celestial objects, such as nebulae and galaxies, while a smaller FOV is better suited for observing smaller objects, such as planets and stars.

The field of view (FOV) in a telescope defines the extent of the observable universe that is visible through the eyepiece at any given moment. Knowing the FOV allows astronomers to determine the ideal eyepiece for a specific observation. There are two distinct types of FOV: the apparent field of view (AFOV) and the true field of view (TFOV).

Will Kalif is an amateur astronomer at TelescopeNerd.com. Will is an author of the book "See It With A Small Telescope". Will Kalif has been passionate about telescopes and the wonders of the night sky ever since he received his first telescope as a teenager. And for several decades now he has been making and using his own telescopes and helping other people to also enjoy the various things that can be seen on a dark and starry night.

The field of view of a telescope eyepiece is the angular extent of the sky that is observed through the eyepiece. It is influenced by the eyepiece’s design and is typically provided by the manufacturer.

The ideal FOV for a telescope is contingent on the specifics of the observation. For example, a larger FOV will be more desirable for wide-field observations of large celestial bodies, while a smaller FOV will be more effective for detailed observations of smaller entities.

Cementing three lenses together produces a triplet lens. Triplets produce a better quality image, are corrected for three colors, and give little or no image distortion. They are best used for jobs that require a great deal of precision at high magnifying levels.

The magnification of a telescope is determined by the ratio of the telescope’s focal length to the eyepiece’s focal length. Therefore, the choice of the eyepiece significantly affects the magnification and, consequently, the field of view and the types of celestial objects that can be observed effectively.

10" is assumed to be the closest distance the human eye can focus for comfortable vision. An object only 1" from your eye would be 10 times larger, but out of focus. A magnifier's function is to assist your eye in focusing closer. Since a 1" focal length lens brings clear vision down to 1" from the eye, an object at this distance is clearly seen and appears to be 10 times closer than it does when viewed from 10" away. Such a magnifier is commonly called a 10X or 10 power. Using this definition, the magnifying power of a lens can be approximated as follows: MP = 10/FL if the focal length is specified in inches. If the focal length is specified in mm, the formula will be MP=250/FL.

The FOV plays a pivotal role in observational astronomy as it dictates the range of celestial objects that can be observed. For instance, a telescope with a larger FOV enables the viewing of expansive celestial bodies like nebulae and galaxies, whereas a telescope with a smaller FOV is more suitable for observing smaller entities like planets and stars.

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Actual magnifying power will vary slightly, depending upon working distance, eye relief distance and the characteristics of the observer's eye.

The distance from the magnifier to the object viewed is the working distance. This distance is an important consideration with regard to the type of work that must be done under the magnifier. If your work requires the use of tools, a magnifier with a long working distance will allow enough space to both use the tools and comfortably view the object. Small working distance magnifiers with higher powers are preferred for close-up inspection work.

The eyepiece of a telescope magnifies the image formed by the telescope’s objective lens or mirror. The eyepiece is the part of the telescope that observers look through. The eyepiece plays a significant role in determining the magnification, field of view (FOV), and overall viewing experience.

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When calculating FOV, it’s important to distinguish the difference between the apparent field of view (AFOV) and the true field of view (TFOV). The AFOV is the angle of the sky that appears to be covered by the eyepiece, while the TFOV is the actual portion of the sky that is seen through the telescope. For example, a wide AFOV eyepiece will make the sky appear larger, but the actual TFOV is smaller due to the telescope’s magnification.

Knowledge Center/ Application Notes/ Microscopy Application Notes/ Magnifying Lenses: How to Choose a Magnifier

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To choose the correct magnifier for the job, first determine what tools are to be used on the job; then determine the size and the character of the subject; and finally, analyze the object's surface character. Then review the following aspects of magnifiers:

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The optimal FOV for a telescope depends on the type of observations being made. For example, a larger FOV is preferable for wide-field observations of large celestial objects, while a smaller FOV is better for detailed observations of smaller objects. By understanding the relationship between FOV and viewing experience, astronomers are able to select the best eyepiece for their observational goals.

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The distance between the closest and furthest points at which a magnifier in a fixed position stays in focus. The depth of field decreases as power increases.

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For example, if an eyepiece has a field of view, or AFOV, of 50 degrees and a magnification of 25x, the true field of view is 2 degrees. This equation is expressed as (50 / 25 = 2). Knowing the TFOV of a telescope is crucial to selecting the right optics based on specific observational goals, making it a crucial metric for astronomers.

The field of view is the area seen through the magnifier. As power increases, lens diameter and field of view decrease. At 5 power (5X), field of view is about 1.5". At 10 power (10X), it is about 0.5". Usually, it is best to use low power for scanning larger surfaces and high power for small areas.

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Magnification and field of view (FOV) in a telescope share an inverse relationship. This means that as the magnification increases, the FOV decreases, and conversely, as the magnification decreases, the FOV increases. This relationship stems from the fact that as one increases the magnification, the telescope effectively zooms in on a smaller section of the sky, thereby reducing the FOV.

Though dividing AFOV by magnification is a simple and widely used method of calculation, it is not exact. Telescope optics vary in measurement by up to 5%, which skews the accuracy of the calculation. For a more accurate calculation, astronomers use the field stop diameter and focal length to calculate FOV.

A perfect magnifier would be lightweight, have a large diameter, provide a wide viewing area, and offer high, distortion-free magnification. However, incorporating all of these features into one unit is optically impossible. The magnifying power of a lens depends on its focal length (fl). The focal length, in turn, depends on the lens curvature; the greater the curvature, the shorter the focal length and the greater the power. In the design of a simple, inexpensive magnifier, the lens diameter will typically decrease as the curvature increases to provide higher power. Conversely, as the curvature is decreased to lower the power, the diameter generally increases with a resulting increase in viewing area. In addition, distortion generally increases with an increase in curvature. Thus, a magnifier with a large diameter typically offers more viewing area and less power. So, both wide field of view and high magnifying power cannot be incorporated into a single design without elaborate, weighty, high-cost lenses.

The FOV of the eyepiece impacts the overall FOV of the telescope. An eyepiece with a larger FOV will yield a larger overall FOV for the telescope, facilitating the observation of larger celestial objects. On the other hand, an eyepiece with a smaller FOV will result in a smaller overall FOV, which is more suitable for observing smaller celestial bodies.

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The eyepiece field stop refers to the diameter of the image formed by the telescope’s objective, while the telescope focal length is the distance from the objective to the point where it forms an image.

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Astronomers can also use an online field of view calculator to compute the TFOV of a telescope based on the specifications of the telescope and eyepiece.

Calculation of the TFOV is done by dividing the AFOV of the eyepiece by the magnification of the telescope, or through the relationship of the focal lengths of the telescope and the eyepiece. The TFOV is typically expressed in degrees.

The field of view (FOV) in a telescope refers to the extent of the observable sky that can be viewed at a single point in time. It’s quantified in units such as degrees, arcminutes, or arcseconds, and is influenced by the telescope’s optics, encompassing factors like the diameter of the objective lens or mirror and the eyepiece in use.

An achromat is a positive simple lens cemented to a negative simple lens. The primary advantage is that it is corrected for two colors and works well at high powers. Most high quality magnifiers use achromats to eliminate color fringing at the edge of objects.