Telescopes

The Hale telescope is at the Palomar Observatory, located in Mount Palomar, California.

Most mid-level and up telescopes have the capability to externally attach a camera in some way. However, this often takes the form of a connection for an old style 35mm film camera. There are moderately-priced computer cameras available which can be used with older 35mm lenses and hardware, and would thus be able to hook up to your telescope with pretty good clarity. Your other option may be to purchase a purpose-built ccd camera unit such as I have linked below. They can be mounted inside the telescope or on it in lieu of an actual eyepiece. These can be very expensive, but will likely give you better results.

How the telescope works In orbit about 380 miles (610 kilometers) above the earth, the Hubble Space Telescope views the heavens without looking through the earth's atmosphere. The atmosphere bends light due to a phenomenon known as diffraction, and the atmosphere is constantly moving. This combination of diffraction and movement causes starlight to jiggle about as it passes through the air, and so stars appear to twinkle. Twinkling blurs images seen through ground-based telescopes. Because an orbiting telescope is above the atmosphere, it can produce pictures in much finer detail than a ground-based telescope can. This false-color image taken by the Hubble Space Telescope using infrared light shows Uranus's rings and clouds. The different colors in the image represent different atmospheric conditions. Image credit: NASA The Hubble Space Telescope can also observe ultraviolet and infrared light that is blocked by the atmosphere. These forms of light, like visible light, are electromagnetic radiation. The wavelength (distance between successive wave crests) of ultraviolet light is shorter than that of visible light. Infrared light has longer wavelengths than visible light. Ultraviolet light comes from highly energetic processes, such as the formation of disks around black holes and exploding stars. Infrared light provides information about cooler, calmer events, such as the formation of dust clouds around new stars. The United States space agency, the National Aeronautics and Space Administration (NASA), operates the Hubble Space Telescope in cooperation with the European Space Agency (ESA). The telescope is controlled by radio commands relayed from NASA's Goddard Space Flight Center in Greenbelt, Maryland. Astronomers tell the telescope where to point, and computer -- driven instruments aboard the telescope record the resulting observations. The telescope transmits the data by radio to astronomers on the ground. The Hubble Space Telescope has two kinds of instruments: (1) imagers, which take pictures; and (2) spectrographs, which analyze light. Imagers are electronic detectors called charge -- coupled devices (CCD's). The CCD's convert light into electronic signals, which an on -- board computer records and sends to the ground. A spectrograph, like a prism, spreads light into its component colors, much as water droplets spread sunlight into a rainbow. The resulting band of light is called a spectrum (plural spectra). Using spectrographic data from the Hubble Space Telescope, astronomers can determine the composition of stars and galaxies--measuring, for example, the amounts of hydrogen, carbon, and other chemical elements in them How the telescope works In orbit about 380 miles (610 kilometers) above the earth, the Hubble Space Telescope views the heavens without looking through the earth's atmosphere. The atmosphere bends light due to a phenomenon known as diffraction, and the atmosphere is constantly moving. This combination of diffraction and movement causes starlight to jiggle about as it passes through the air, and so stars appear to twinkle. Twinkling blurs images seen through ground-based telescopes. Because an orbiting telescope is above the atmosphere, it can produce pictures in much finer detail than a ground-based telescope can. This false-color image taken by the Hubble Space Telescope using infrared light shows Uranus's rings and clouds. The different colors in the image represent different atmospheric conditions. Image credit: NASA The Hubble Space Telescope can also observe ultraviolet and infrared light that is blocked by the atmosphere. These forms of light, like visible light, are electromagnetic radiation. The wavelength (distance between successive wave crests) of ultraviolet light is shorter than that of visible light. Infrared light has longer wavelengths than visible light. Ultraviolet light comes from highly energetic processes, such as the formation of disks around black holes and exploding stars. Infrared light provides information about cooler, calmer events, such as the formation of dust clouds around new stars. The United States space agency, the National Aeronautics and Space Administration (NASA), operates the Hubble Space Telescope in cooperation with the European Space Agency (ESA). The telescope is controlled by radio commands relayed from NASA's Goddard Space Flight Center in Greenbelt, Maryland. Astronomers tell the telescope where to point, and computer -- driven instruments aboard the telescope record the resulting observations. The telescope transmits the data by radio to astronomers on the ground. The Hubble Space Telescope has two kinds of instruments: (1) imagers, which take pictures; and (2) spectrographs, which analyze light. Imagers are electronic detectors called charge -- coupled devices (CCD's). The CCD's convert light into electronic signals, which an on -- board computer records and sends to the ground. A spectrograph, like a prism, spreads light into its component colors, much as water droplets spread sunlight into a rainbow. The resulting band of light is called a spectrum (plural spectra). Using spectrographic data from the Hubble Space Telescope, astronomers can determine the composition of stars and galaxies--measuring, for example, the amounts of hydrogen, carbon, and other chemical elements in them

While space shuttle Columbia was lifting off, a piece of Styrofoam the size of a briefcase fell on its wing. It made a hole in it. While reentering Earth's atmosphere, heat got inside the wing. It started making engines offline at mission control and the space shuttle disintegrated over Texas. Everyone died on Columbia. (I don't know how they would survive anyway)

I've had this problem with a Skywatcher 120mm refractor and Antares SWA eyepiece. I've heard that there are low-profile 1.25" adapters that you can use with 2" diagonals to give you more inward travel. I'm still searching for one myself. Also some people say aftermarket focusers (ex. Moonlite) may solve this problem.

Chandra X-Ray Observatory Cost: Development ~ $1.65 billion Launch Costs ~ $350 million Operations and Data Analysis (years 1-5) ~ $0.75 billion Operations and Data Analysis (years 6-10) ~ $245 million

Galileo discovered the four largest moons of Jupiter (later named the Galilean moons), mountains and craters on the moon, phases of Venus, and sunspots on the sun. These observations supported the heliocentric model of the solar system and challenged the geocentric view of the universe.

Nearly all modern mirrors are aluminum. An aluminum coating is placed on a sheet of polished glass. In common mirrors we observe this aluminum reflector through the glass layer. But if we turn the mirror around, we can bounce light directly off the aluminum, and this is called a "front surface mirror." (Common mirrors have a coating of hard paint over the thin delicate aluminum coating to prevent scratches.) It's perfectly possible to form a mirror by grinding and polishing a thick aluminum slab. But aluminum is softer than glass, and would collect scratches and dings. Also, aluminum is expensive, so an aluminum mirror costing several dollars might replace a glass mirror costing a few cents.

Four telescopes with 8m diameter each can gather as much light as one with 16m diameter because they can be combined using interferometry techniques to effectively act as a single telescope with the equivalent light-gathering area. By correlating the signals from the individual telescopes, the resolution and sensitivity can be increased as if they were a single larger telescope.

Refracting telescopes have a lens at the front to gather light and focus it, while reflecting telescopes use a curved mirror at the back to collect and focus light. The main components of a refracting telescope are the objective lens, eyepiece, and tube, while the main components of a reflecting telescope are the primary mirror, secondary mirror, and housing.

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The telescope has a large diameter concave main mirror with a hole at it's centre.This is known as a Cassegrain configuration. Light from the stars enters the telescope tube and is reflected from the main mirror back up the tube and is then reflected by a small secondary mirror back down through the hole in the main mirror to a focus point behind it.

An array of cameras and spectroscopes share the light by means of a beam splitter at the main focus. The cameras digitally process the images they recieive using charge couple devices known as CCD's or electronic eyes. The digital signals are labelled and sent to a microwave dish which transmit the images back to Earth.

The telescope is powered by solar cells and has a lens cap that automatically closes whenever the sun is a danger to the sensitive cameras.The telescope is remotely pointed and stabilised using gyroscopes and it is these moving parts that are prone to failure.

Despite early problems the Hubble telescope a shuttle space mission was sent to repair the telescope and fit an optical fix known a 'Costar'. The mirror had been ground with an error in the measurement system and ever since has been a fantastic success. It was given major overhaul earlier this year in one of the last shuttle missions and is to be replaced by the James Webb Space Telescope (JWST)in the next decade.

Focal length is the distance between the optical center of a lens and the image sensor when the lens is focused on a subject at infinity. It determines the magnification and field of view of the lens, with shorter focal lengths providing wider angles of view and longer focal lengths providing narrower angles of view. Focal length is commonly measured in millimeters.

The four main properties of a telescope are its aperture (diameter of the primary lens or mirror), magnification (how much larger the telescope makes distant objects appear), focal length (distance from the lens or mirror to the focal point), and resolution (the ability to distinguish fine details or separate closely spaced objects).

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Around 1284 in Italy, Salvino D'Armate is credited with inventing the first wearable eye glasses. This picture is a reproduction copied from an original pair of eye glasses dating back to the mid-1400's.

The magnification (MA) equals the focal length of the objective lens (fo) divided by the focal length of the eyepiece (fe), which is this: MA = fo / fe = 10 feet / .25 inches = 120 inches / .25 inches = 480 A link to the Wikipedia article on magnification is included.

weaver was the vender but the model was sold as JC Higgins it was a 4 power scope known as JC Higgins marksman both the scope and the mount were unique to the model 31 rifle 583 75 was Made by High Standard manufacturing in 1952 Both the rifle and scope were sold only by Sears & Roebuck and exclusive to them only I see the scope for sale all the time on Ebay they average about 15 to 25 bucks .If you by one make sure it works and that it has it scope mount

The magnification of any reflector telescope is given by the focal length of the mirror divided by the focal length of the eyepiece, so if the mirror's focal length is 1000mm and the eyepiece has a focal length of 10mm, then the magnification is 1000 / 10 or 100 X magnification. So, if you wish to increase the magnification you need to either change the mirror (which is impractical) or change the eyepiece (which is easy) replacing it with an eyepiece with a shorter focal length. So, if the new eyepiece has a focal length of 5mm then the magnification is 1000/5 or 200 X magnification. If you do not wish to buy an expensive complete set of eyepieces, you can buy what is called a Barlow lens which fits between the eyepiece and the telescope. These can increase the magnification by a factor of 2 or 3, but the quality of the image is not so good (as the light has to pass through the Barlow lens as well as the eyepiece). Do not forget that you cannot keep increasing magnification hoping to get better and better images. As you double the magnification, you cut the light entering the telescope by at least a half, so the image is dimmer. Most small telescopes with mirrors between 6 and 8 inches can magnify up to around 100 X effectively but anything more than this will result in the image becoming progressively darker, more grainy and generally not so clear. To get higher magnification you need much bigger mirrors of 10 or 12 inches or more. To add further complications, you will also need a substantial mount for the 'scope as any small vibration at a high magnification will result in a great deal of image shake. Also, you will need a really good motor drive to compensate for the movement of the earth, as, without such a drive at high magnifications, the image will move out of the field of view almost as quickly as you find it due to the earth's motion.

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Depending on optical quality and observing conditions, you can expect to get anywhere from 20x to 50x of useful magnification per inch of aperture. In other words, a 4-inch scope tops out at 200x under ideal conditions, but a 6-inch scope can work well as high as 300x under ideal conditions.

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