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Calibration of Non-Spatially-Filtered Data in Optical
Calibration of Non-Spatially-Filtered Data in Optical

... • If we turn our telescopes to overlooked nearby stars with white dwarf companions (like Mira A when it dies), we should be able to find many systems that formed like Mira B. • So… We discovered that around Mira B is a new kind of protoplanetary disk, formed from the wind of a dying star. This is th ...
USING a NEWTONIAN REFLECTOR for DOUBLE STAR WORK
USING a NEWTONIAN REFLECTOR for DOUBLE STAR WORK

... The only answer, if you want to use a Newtonian for double star work, is to build one that is as close to aplanatic as feasible. A Newtonian is only aplanatic when the focal ratio for a given aperture is such that the departure of the paraboloidal primary mirror surface from a spheroidal surface is ...
GM-8 manual-05.cdr
GM-8 manual-05.cdr

... Remove all the parts from their respective boxes and place them on a flat, clear work area. A large floor space is ideal. When setting up your Losmandy GM-8, you must start with the tripod and work from there. To insure proper assembly, each task must be performed in the specific order as defined by ...
History - Astrophysical Research Consortium
History - Astrophysical Research Consortium

... As early as October 1965 the UW Regents authorized construction of a large telescope using external (Vs state) funds. Although Professors Wallerstein and Hodge entered into discussions with many potential partners in the following ten years, including the Jet Propulsion Lab and the University of Wis ...
Light and Telescopes Astronomy 1 — Elementary Astronomy LA Mission College Spring F2015
Light and Telescopes Astronomy 1 — Elementary Astronomy LA Mission College Spring F2015

... A. Largest diameter primary mirror B. Largest diameter secondary mirror C. eyepiece with the largest magnification D. tube with the longest length Astronomy 1 - Elementary Astronomy ...
The last gasps of VY CMa: Aperture synthesis and adaptive optics
The last gasps of VY CMa: Aperture synthesis and adaptive optics

... asymmetries in the circumstellar emission at high spatial resolution, although no such asymmetries had been directly detected until this work. McCarthy (1979) reported asymmetry in the midinfrared emission of the dust shell, interpreting this as evidence for thermal emission from a disklike structur ...
Outline Thesis – so far
Outline Thesis – so far

... star constellation comprises of three beacons forming an equilateral triangle on a circle with a radius of 2 arcminutes. The images of the beacons that have to be reproduced suffer from strong aberrations caused by the large off-axis distance. To match the wavefront of the beacons‟ images to the des ...
On the Parabolic Curve of Primary Mirrors
On the Parabolic Curve of Primary Mirrors

Binocular Performance Index
Binocular Performance Index

The Ages of Astrophotography - Powered by Catchers of the Light
The Ages of Astrophotography - Powered by Catchers of the Light

... features 100 of the most important, iconic and famous of astronomical objects, instruments, surveys, telescopes and cameras. For each ‘object’ two images are depicted side by side, one taken by an early Pioneer of Astrophotography and a second imaged by one of today’s finest Astronomical Photographe ...
V.90-3-James H. Cole, Clay Kirkendall, Anthony Dandridge, Gary
V.90-3-James H. Cole, Clay Kirkendall, Anthony Dandridge, Gary

Using Mirrors to Form Images
Using Mirrors to Form Images

... than the one used in Hubble. You probably know that aluminum is much less dense than iron, which is why aluminum is commonly used in aircraft. Beryllium is a metal that is even less dense than aluminum, and research is under way to make mirrors completely out of this metal. The mirrors on space tele ...
PACS Calibration Status and Plans
PACS Calibration Status and Plans

... orientation angles, both partners with sufficient flux 2) double galaxies (13) with 35” – 150” separation, compact well located and distinguishable emission component 3) asteroid – asteroid, asteroid – planet encounters, moons ...
Principles, Limitations and Performance of Multi
Principles, Limitations and Performance of Multi

...  The very crude analytical approach proposed above seem to describe quite well the amplitude of the generalized tting error, at least for this kind of systems. An arbitrary limit to h when designing a MCAO system is to have both terms of Eq 3 balanced (classical tting and generalized tting erro ...
RPT-O-G0047 Gemini Telescopes f/16 Optical
RPT-O-G0047 Gemini Telescopes f/16 Optical

... desirable. However, a small focal ratio would require a large secondary mirror when keeping the focal plane location constant. And as secondary mirrors increased in size, the problem of maintaining low self-weight deflection in changing gravity orientations became more difficult. The best overall co ...
Martin`s presentation
Martin`s presentation

... No current plans for a Chandra-class sub-arcsec - mission - world-wide No space agency developing high resolution X-ray mirrors Reason: Cannot make a bigger Chandra  mirrors are heavy ...
The secondary and tertiary mirros for the TMT
The secondary and tertiary mirros for the TMT

... The TMT Project gratefully acknowledges the support of the TMT partner institutions. They are the Association of Canadian Universities for Research in Astronomy (ACURA), the California Institute of Technology and the University of California. This work was supported as well by the Gordon and Betty M ...
Optics and Telescopes PowerPoint
Optics and Telescopes PowerPoint

... • Infrared Telescopes – Very similar to visible wavelength telescopes, except for the detector, called a bolometer. – IR scopes detect heat from warm gas or warm objects. “Warm” means not hot enough to glow in visible light. – These scopes must be kept very cold or the heat that the ‘scope itself ra ...
The GMT-Consortium Large Earth Finder (G
The GMT-Consortium Large Earth Finder (G

... Universidade de São Paolo, Rua do Matão 1226, 05508-900, São Paulo, Brazil b ...
Finite number of Guide Star
Finite number of Guide Star

... – PSF variability problem drastically reduced • Cone-effect solved ...
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Galileo Gahilei Aiko Corralz Salt Lake Community
Galileo Gahilei Aiko Corralz Salt Lake Community

... of Saturn, it may have seem that these are the planets that his telescope can observe, but that is not quite true. When he was observing Jupiter, he noticed a bright star near the big red planet. At the time Galileo believed that it was just another star, but as researchers now discovered that Galil ...
Paper 1 (pdf)
Paper 1 (pdf)

... for the incoming X-rays. Sampling at least 3 PAs is required in order to measure three Stokes parameters (I, Q, U) uniquely, so one would require at least three separate detector systems with accompanying multilayer-coated flats. This design is more costly and heavy than the original design by Flana ...
3. Daylight Mapping
3. Daylight Mapping

User Manual for the UofL CDK20 System at Mt Kent...
User Manual for the UofL CDK20 System at Mt Kent...

... The telescope is a Planewave (http://planewave.com ) CDK20 0.5m aperture, f/6.8 corrected DallKirkham design with a 3.454m focal length. This is an innovative design that provides sharp focus over a large field of view, and great temperature stability of focus due to its carbon-fibre truss. The prim ...
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Very Large Telescope



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.
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