How to Buy Your First Telescope
... The world’s best telescope is useless if you can’t find anything with it. Its high magnification limits the field of view. Even with a go-to drive, you’ll need a quality low-power finder scope. Most are tubes you view straight through. They flip the image but let you look toward the object, a positi ...
... The world’s best telescope is useless if you can’t find anything with it. Its high magnification limits the field of view. Even with a go-to drive, you’ll need a quality low-power finder scope. Most are tubes you view straight through. They flip the image but let you look toward the object, a positi ...
Mirror coatings for the Large Synoptic Survey Telescope
... on the Twin Gemini Telescopes [1,2] and the European Southern Observatory Very Large Telescope (VLT) [3]. Both of these observatories were designed with 8m diameter monolithic meniscus mirrors. Large telescopes are usually located on remote elevated sites that are inherently dusty and windy. Because ...
... on the Twin Gemini Telescopes [1,2] and the European Southern Observatory Very Large Telescope (VLT) [3]. Both of these observatories were designed with 8m diameter monolithic meniscus mirrors. Large telescopes are usually located on remote elevated sites that are inherently dusty and windy. Because ...
instruction manual
... useful accessories. When they are correctly aligned with the telescope, objects can be quickly located and brought to the centre of the field. Alignment is best done outdoors in day light when it's easier to locate objects. If it is necessary to refocus your finderscope, sight on an object that is a ...
... useful accessories. When they are correctly aligned with the telescope, objects can be quickly located and brought to the centre of the field. Alignment is best done outdoors in day light when it's easier to locate objects. If it is necessary to refocus your finderscope, sight on an object that is a ...
Construction of a unit power finder
... In order to be able to locate faint objects the intensity of the led can be changed with the potentiometer. For the moment I can see a couple of drawbacks in the design: A double reflection may be visible in the finder window due to the thickness of the glass. By minimizing this thickness, this p ...
... In order to be able to locate faint objects the intensity of the led can be changed with the potentiometer. For the moment I can see a couple of drawbacks in the design: A double reflection may be visible in the finder window due to the thickness of the glass. By minimizing this thickness, this p ...
X-ray tracing using Geant4 ARTICLE IN PRESS Nuclear Instruments
... details of the interaction of X-rays on a surface can be described by scattering models of various complexity, and are also driven by the type of data describing the microscopic surface details. It is therefore not surprising that even within the same model different surfaces may have different X-ra ...
... details of the interaction of X-rays on a surface can be described by scattering models of various complexity, and are also driven by the type of data describing the microscopic surface details. It is therefore not surprising that even within the same model different surfaces may have different X-ra ...
FGS1R: Potentially HST`s Astrometry Science Workhorse
... In order to illustrate the perfomance capabilities of FGS3 and FGS1R, we have generated a series of synthetic S-Curves of binary systems. A simple schematic of a binary orbit and resulting S-Curves are given in Figure 4. The composite S-Curve of a multiple system is a linear superposition of the S-C ...
... In order to illustrate the perfomance capabilities of FGS3 and FGS1R, we have generated a series of synthetic S-Curves of binary systems. A simple schematic of a binary orbit and resulting S-Curves are given in Figure 4. The composite S-Curve of a multiple system is a linear superposition of the S-C ...
Chandra The Role of Modeling in the Calibration of ’s Optics
... The Chandra X-ray observatory, launched in 1999, is the result of more than two decades of design, engineering, and manufacturing effort. At its heart is a set of four Wolter type I optics, fabricated of Zerodur and polished to a surface roughness of 1.3 − 3Å,1 designed to provide better than 100 a ...
... The Chandra X-ray observatory, launched in 1999, is the result of more than two decades of design, engineering, and manufacturing effort. At its heart is a set of four Wolter type I optics, fabricated of Zerodur and polished to a surface roughness of 1.3 − 3Å,1 designed to provide better than 100 a ...
Astrometry: Revealing the Other Two Dimensions of
... hundred stars. At no point in astronomical science is fuller knowledge more desirable, more pressingly urgent, than in the subject of stellar distances.” ...
... hundred stars. At no point in astronomical science is fuller knowledge more desirable, more pressingly urgent, than in the subject of stellar distances.” ...
Document
... • Its near-IR imaging will go far deeper than VISTA or any other ground-based imaging survey because of the reduced background and lack of atmospheric absorption. The IR imaging isn’t at HST resolution – it isn’t for weak lensing, but for photometric redshifts. • It will also take near-IR spectra of ...
... • Its near-IR imaging will go far deeper than VISTA or any other ground-based imaging survey because of the reduced background and lack of atmospheric absorption. The IR imaging isn’t at HST resolution – it isn’t for weak lensing, but for photometric redshifts. • It will also take near-IR spectra of ...
ALMA Newsletter N°5
... Kea, or the four 8-m units of the Very Large Telescope on Paranal: they allow us to investigate very faint optical phenomena whose details cannot be studied with the unaided eye. The evolution of optical instruments also includes detector systems: first the unaided eye, then photographic plates, and ...
... Kea, or the four 8-m units of the Very Large Telescope on Paranal: they allow us to investigate very faint optical phenomena whose details cannot be studied with the unaided eye. The evolution of optical instruments also includes detector systems: first the unaided eye, then photographic plates, and ...
Project_Description2
... of the optical-UV to the near IR (although there is a significant drop in the 700-900nm region), and it develops a native layer that enables it to survive for 2-3 years before recoating is necessary. However, in modern 3-mirror telescopes, a 10% loss at each surface degrades throughput by nearly 30% ...
... of the optical-UV to the near IR (although there is a significant drop in the 700-900nm region), and it develops a native layer that enables it to survive for 2-3 years before recoating is necessary. However, in modern 3-mirror telescopes, a 10% loss at each surface degrades throughput by nearly 30% ...
Boy Scouts of America ASTRONOMY Merit Badge Guide
... or in a guidebook. Prepare an observing log or notebook. Show your plan, charts, and log or notebook to your counselor before making your observations. Review your log or notebook with your counselor afterward. C) Plan and host a star party for your Scout troop or other group such as your class at s ...
... or in a guidebook. Prepare an observing log or notebook. Show your plan, charts, and log or notebook to your counselor before making your observations. Review your log or notebook with your counselor afterward. C) Plan and host a star party for your Scout troop or other group such as your class at s ...
Postgraduate English - Durham University Community
... poems—that the self is not accurately reflected or represented in images. Bishop ends her poem with the quoted sentence, “Half is enough” (11), a hollow statement that not only implies that half is probably not enough, but that another half is missing. That the gentleman did not say it directly—he h ...
... poems—that the self is not accurately reflected or represented in images. Bishop ends her poem with the quoted sentence, “Half is enough” (11), a hollow statement that not only implies that half is probably not enough, but that another half is missing. That the gentleman did not say it directly—he h ...
Pupil Mapping in 2-D for High-Contrast Imaging
... the pupil is tapered to zero at the edges, thereby reducing the sidelobes, but at a loss of light and angular resolution. Another idea is the shaped pupil (Spergel (2000), Vanderbei et al. (2003a,b,c, 2004)), in which the pupil is covered by an opaque mask that has carefully-shaped transmitting cut- ...
... the pupil is tapered to zero at the edges, thereby reducing the sidelobes, but at a loss of light and angular resolution. Another idea is the shaped pupil (Spergel (2000), Vanderbei et al. (2003a,b,c, 2004)), in which the pupil is covered by an opaque mask that has carefully-shaped transmitting cut- ...
Chapter 2.1 - Focusing Fundamentals
... have plenty of light to work with while you focus, and so does the automatic focuser found in most of today’s cameras. Professional film cameras allow you to focus by looking at a ground glass screen that is conveniently located exactly the same distance from the camera lens as the film. The scene i ...
... have plenty of light to work with while you focus, and so does the automatic focuser found in most of today’s cameras. Professional film cameras allow you to focus by looking at a ground glass screen that is conveniently located exactly the same distance from the camera lens as the film. The scene i ...
Mapping the Milky Way: William Herschel`s Star-‐Gages
... The left part of Figure 6 shows the 3D view of the star system. This system is just like the previous one except the stars are highly concentrated near the center of the disk. The plot o ...
... The left part of Figure 6 shows the 3D view of the star system. This system is just like the previous one except the stars are highly concentrated near the center of the disk. The plot o ...
CFRP composite optical telescope assembly for the 1m ULTRA project
... package, however, will be the same as one used on a traditional glass and steel telescope. The ULTRA instrumentation package is expected to be up to 50 Kg. These requirements lead to an OTA design that keeps the weight (and required stiffness) near the declination axis as much as possible. The top e ...
... package, however, will be the same as one used on a traditional glass and steel telescope. The ULTRA instrumentation package is expected to be up to 50 Kg. These requirements lead to an OTA design that keeps the weight (and required stiffness) near the declination axis as much as possible. The top e ...
Engineering Lightweight Dobsonian Telescopes
... reasonably short. You also want to use common eyepiece sizes, so mid f/ ratios are a good fit. If your f/ ratio is too low, the view at the eyepiece will display coma (blurring at the edge of the field). This may require an expensive light robbing coma corrector. Eyepiece diameter, field stop, and ...
... reasonably short. You also want to use common eyepiece sizes, so mid f/ ratios are a good fit. If your f/ ratio is too low, the view at the eyepiece will display coma (blurring at the edge of the field). This may require an expensive light robbing coma corrector. Eyepiece diameter, field stop, and ...
AstroMaster Series Telescopes
... Take time to read through this manual before embarking on your journey through the Universe. It may take a few observing sessions to become familiar with your telescope, so you should keep this manual handy until you have fully mastered your telescope’s operation. The manual gives detailed informati ...
... Take time to read through this manual before embarking on your journey through the Universe. It may take a few observing sessions to become familiar with your telescope, so you should keep this manual handy until you have fully mastered your telescope’s operation. The manual gives detailed informati ...
Atmospheric Gas Phase Reactions
... 1) Slit could be very high (long) if e.g. a detector with 20 x 20 mm size is used 2) Angle of incidence on refracting surface is about: /2 + /2 23o + 30o 53o Fresnel reflection @ 53o is about 6-7% 90% efficiency! 3) Dispersion curve is highly non-linear Needs to be corrected (l ...
... 1) Slit could be very high (long) if e.g. a detector with 20 x 20 mm size is used 2) Angle of incidence on refracting surface is about: /2 + /2 23o + 30o 53o Fresnel reflection @ 53o is about 6-7% 90% efficiency! 3) Dispersion curve is highly non-linear Needs to be corrected (l ...
FISICA: The Florida Image Slicer for Infrared Cosmology
... infrared astronomy. While optical fibers have tended to work rather well in integral field units (IFU) for optical instruments, they can suffer from many drawbacks for infrared work, including low throughput, limited bandwidth, high background (for non-cryogenic IFUs), and other optical drawbacks as ...
... infrared astronomy. While optical fibers have tended to work rather well in integral field units (IFU) for optical instruments, they can suffer from many drawbacks for infrared work, including low throughput, limited bandwidth, high background (for non-cryogenic IFUs), and other optical drawbacks as ...
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.