The History of Optical Astronomy - eCUIP
... Lyman Strong Spitzer, Jr. was an American theoretical physicist, astronomer and mountaineer. He carried out research into star formation, plasma physics, and in 1946, conceived the idea of telescopes operating in outer space. Spitzer is the namesake of NASA's Spitzer Space Telescope. ...
... Lyman Strong Spitzer, Jr. was an American theoretical physicist, astronomer and mountaineer. He carried out research into star formation, plasma physics, and in 1946, conceived the idea of telescopes operating in outer space. Spitzer is the namesake of NASA's Spitzer Space Telescope. ...
jwhitney - Astronomy at Western Kentucky University
... CCD camera to obtain data for key science projects. Our primary goal is the monitoring of the brightness variations of Active Galactic Nuclei and using these variations to investigate the physics at work in these objects. Working from a control room on WKU's campus, the telescope and camera are cont ...
... CCD camera to obtain data for key science projects. Our primary goal is the monitoring of the brightness variations of Active Galactic Nuclei and using these variations to investigate the physics at work in these objects. Working from a control room on WKU's campus, the telescope and camera are cont ...
The Hubble Space Telescope (HST)
... The Wide Field Camera 3 (WFC3) sees three different kinds of light: nearultraviolet, visible and near-infrared, though not simultaneously. Its resolution and field of view are much greater than that of Hubble's other instruments. WFC3 is one of Hubble's two newest instruments, and will be used to st ...
... The Wide Field Camera 3 (WFC3) sees three different kinds of light: nearultraviolet, visible and near-infrared, though not simultaneously. Its resolution and field of view are much greater than that of Hubble's other instruments. WFC3 is one of Hubble's two newest instruments, and will be used to st ...
slides - Caltech Astronomy
... The ray in the figure has s1 = ∞ intersecting the first surface at y1 and the second at y2 . From two sets of similar right triangles, both sets including either y2 or y1 as one side, y2 / y1 = s2 / s1' = ( s1' - d ) / s1' = s2' / f ' where f ' is the effective focal length of the whole system, and, ...
... The ray in the figure has s1 = ∞ intersecting the first surface at y1 and the second at y2 . From two sets of similar right triangles, both sets including either y2 or y1 as one side, y2 / y1 = s2 / s1' = ( s1' - d ) / s1' = s2' / f ' where f ' is the effective focal length of the whole system, and, ...
Ay 20 - Caltech
... typical 20 cm (8 in) amateur telescope at 550 nm. Express your answer in arcseconds. (b) Using the information in Appendix C, estimate the minimum size of crater on the moon that can be resolved by a 20 cm (8 in) telescope. (c) Is this resolution limit likely to be achieved? Why or why not? PROBLEM ...
... typical 20 cm (8 in) amateur telescope at 550 nm. Express your answer in arcseconds. (b) Using the information in Appendix C, estimate the minimum size of crater on the moon that can be resolved by a 20 cm (8 in) telescope. (c) Is this resolution limit likely to be achieved? Why or why not? PROBLEM ...
Telescope Principles - The Federation of Galaxy Explorers
... in many optical designs, and consist of one or more lenses in combination -- they are almost like mini-telescopes themselves. The purposes of the eyepiece are to: • produce and allow you to change the telescope's magnification • produce a sharp image When we look through a telescope with our eyes we ...
... in many optical designs, and consist of one or more lenses in combination -- they are almost like mini-telescopes themselves. The purposes of the eyepiece are to: • produce and allow you to change the telescope's magnification • produce a sharp image When we look through a telescope with our eyes we ...
Justin Kiehne: Next Generation X-ray Observatory
... X-ray astrophysics and astronomy require increasingly high resolution optics for the study of the most distant stellar objects. As resolution improves, light weight must be maintained for increasing photon collection area. X-ray observations are made from space so limitations imposed by launch must ...
... X-ray astrophysics and astronomy require increasingly high resolution optics for the study of the most distant stellar objects. As resolution improves, light weight must be maintained for increasing photon collection area. X-ray observations are made from space so limitations imposed by launch must ...
The Telescope - Salt Lake Astronomical Society
... the ancient astronomers. The true beginning of telescopes is somewhat foggy in history but the roots of its development started somewhere in the 13th century. An glassmaker noticed that if he looked through a glass disk just right, everything looked a little clearer and the object in view was slight ...
... the ancient astronomers. The true beginning of telescopes is somewhat foggy in history but the roots of its development started somewhere in the 13th century. An glassmaker noticed that if he looked through a glass disk just right, everything looked a little clearer and the object in view was slight ...
astronomical observatories of the canary islands
... Canary Island Telescope by the GTC Team.Treatment: Daniel López/IAC ...
... Canary Island Telescope by the GTC Team.Treatment: Daniel López/IAC ...
Observatory, Domes, and Telescopes
... ascension (RA) axis that lies north-south at an angle of about 30 degrees (the same as the Observatory’s latitude). This telescope axis is parallel with Earth’s rotation axis. HET and mount: The primary mirror is a hexagonal array of 1-meter hexagonal mirrors, primary mirror tetrahedron truss, track ...
... ascension (RA) axis that lies north-south at an angle of about 30 degrees (the same as the Observatory’s latitude). This telescope axis is parallel with Earth’s rotation axis. HET and mount: The primary mirror is a hexagonal array of 1-meter hexagonal mirrors, primary mirror tetrahedron truss, track ...
r 0 - Observatoire de Genève
... • Basic optics, diffraction, Fourier optics, image structure • High contrast AO (VLT SPHERE, E-ELT ) • Sky coverage, Laser guide stars • Wide field AO, Multi-Conjugate Adaptive Optics (Gemini GLAO, VLT MAD, Gemini MCAO) ...
... • Basic optics, diffraction, Fourier optics, image structure • High contrast AO (VLT SPHERE, E-ELT ) • Sky coverage, Laser guide stars • Wide field AO, Multi-Conjugate Adaptive Optics (Gemini GLAO, VLT MAD, Gemini MCAO) ...
All I Want for Christmas Are Astronomy Toys!
... Like the webcam, the lens is removed and replaced with a nosepiece to insert it into the telescope. A video is made and then the best individual frames are selected to stack into a single image. Software is available that will do most of the work automatically. ...
... Like the webcam, the lens is removed and replaced with a nosepiece to insert it into the telescope. A video is made and then the best individual frames are selected to stack into a single image. Software is available that will do most of the work automatically. ...
Document
... 9) Only use paddle control to slew the telescope to center the 2 stars Slewing speed is controlled from the numeric keypad (9 is the fastest, 1 is the slowest) ...
... 9) Only use paddle control to slew the telescope to center the 2 stars Slewing speed is controlled from the numeric keypad (9 is the fastest, 1 is the slowest) ...
Telescopes in History
... mirrors, that are too thin to support their own weight, and segmented mirrors can now be adjusted by computer-controlled servomechanical actuators so that they maintain their optimal shape and position at all times. Small adaptive mirrors may also be inserted in the light path of the telescope to co ...
... mirrors, that are too thin to support their own weight, and segmented mirrors can now be adjusted by computer-controlled servomechanical actuators so that they maintain their optimal shape and position at all times. Small adaptive mirrors may also be inserted in the light path of the telescope to co ...
Toward a revival of Stellar Intensity Interferometry
... high-speed photon-counting instrument. The entrance pupil can be optically sliced into a hundred segments, each feeding a separate detector. Different means of electronically combining the signal in software would yield either a photometric signal of very high time-resolution using the collecting ar ...
... high-speed photon-counting instrument. The entrance pupil can be optically sliced into a hundred segments, each feeding a separate detector. Different means of electronically combining the signal in software would yield either a photometric signal of very high time-resolution using the collecting ar ...
Lenses - singhscience
... creates a real image within a telescope of a distant object. Eyepiece lens – magnifies the image of a distant object. ...
... creates a real image within a telescope of a distant object. Eyepiece lens – magnifies the image of a distant object. ...
PowerPoint - Chandra X
... by the same team. The authors used over 150 separate Chandra observations spread over 13 years to obtain these results. These are stellar-mass black hole candidates, which are formed by the collapse of a massive star and typically have masses between five and 10 times that of the Sun. New techni ...
... by the same team. The authors used over 150 separate Chandra observations spread over 13 years to obtain these results. These are stellar-mass black hole candidates, which are formed by the collapse of a massive star and typically have masses between five and 10 times that of the Sun. New techni ...
3. Telescopes: The Tools of Astronomy
... d) using multiple linked telescopes. Explanation: Shaping a mirror in real time can dramatically improve resolution. © 2017 Pearson Education, Inc. ...
... d) using multiple linked telescopes. Explanation: Shaping a mirror in real time can dramatically improve resolution. © 2017 Pearson Education, Inc. ...
Cosmic Times 1955, 65 PPT
... Advantages Easy to use and construct Excellent for faint deep sky objects (galaxies, nebulae and star clusters) Few optical irregularities, deliver very bright images Reasonably compact and portable Costs less per inch of aperture compared to refractors (mirrors cheaper than lenses) ...
... Advantages Easy to use and construct Excellent for faint deep sky objects (galaxies, nebulae and star clusters) Few optical irregularities, deliver very bright images Reasonably compact and portable Costs less per inch of aperture compared to refractors (mirrors cheaper than lenses) ...
Very Large Telescope
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The Very Large Telescope (VLT) is a telescope operated by the European Southern Observatory on Cerro Paranal in the Atacama Desert of northern Chile. The VLT consists of four individual telescopes, each with a primary mirror 8.2 m across, which are generally used separately but can be used together to achieve very high angular resolution. The four separate optical telescopes are known as Antu, Kueyen, Melipal and Yepun, which are all words for astronomical objects in the Mapuche language. The telescopes form an array which is complemented by four movable Auxiliary Telescopes (ATs) of 1.8 m aperture.The VLT operates at visible and infrared wavelengths. Each individual telescope can detect objects roughly four billion times fainter than can be detected with the naked eye, and when all the telescopes are combined, the facility can achieve an angular resolution of about 0.001 arc-second (This is equivalent to roughly 2 meters resolution at the distance of the Moon).In single telescope mode of operation angular resolution is about 0.05 arc-second.The VLT is the most productive ground-based facility for astronomy, with only the Hubble Space Telescope generating more scientific papers among facilities operating at visible wavelengths. Among the pioneering observations carried out using the VLT are the first direct image of an exoplanet, the tracking of individual stars moving around the supermassive black hole at the centre of the Milky Way, and observations of the afterglow of the furthest known gamma-ray burst.