Performance of the Hobby-Eberly Telescope and facility instruments
... Figure 1 shows an example of EF imaging of the full primary mirror. The images either side of focus reveal some segments to be astigmatic at about 1.0 arcsec. This is not atypical as shown in Figure 2, which is taken at the CoC with the stack burst out into a hexagonal pattern. At first glance, thes ...
... Figure 1 shows an example of EF imaging of the full primary mirror. The images either side of focus reveal some segments to be astigmatic at about 1.0 arcsec. This is not atypical as shown in Figure 2, which is taken at the CoC with the stack burst out into a hexagonal pattern. At first glance, thes ...
Image Formation in the Eye and the Telescope
... Once the polar axis has been properly aligned there needs only to be smooth rotation about this one axis (360 degrees per day, to compensate for the Earth’s rotation) to keep a particular celestial object in view. Because this is relatively easy, particularly if the telescope has a small motor, an e ...
... Once the polar axis has been properly aligned there needs only to be smooth rotation about this one axis (360 degrees per day, to compensate for the Earth’s rotation) to keep a particular celestial object in view. Because this is relatively easy, particularly if the telescope has a small motor, an e ...
Line of sight
... Converting Angular Values Convert a = 390 41’ 54” to radians 2 p radians = 3600 OR p radians = 1800 a = (39 + 41/60 +54/3600) degs / (180/p) ……. radians DMS must usually be converted to D.DD before they can be operated on in a calculator or computer. In some cases (e.g. Excel) angular values must b ...
... Converting Angular Values Convert a = 390 41’ 54” to radians 2 p radians = 3600 OR p radians = 1800 a = (39 + 41/60 +54/3600) degs / (180/p) ……. radians DMS must usually be converted to D.DD before they can be operated on in a calculator or computer. In some cases (e.g. Excel) angular values must b ...
in-field pointing and stray light LISA Symp_final2.pptx
... More difficult telescope design: more optics ...
... More difficult telescope design: more optics ...
Introduction to Adaptive Optics and Deformable
... mirrors to increase depth range, creating truer 3D. In vision applications, adaptive optics are used in robotic vision and surveillance cameras to provide real time or longdistance imaging. In microscopy, adaptive optics correct for aberrations in static lenses. Biomedical applications, including o ...
... mirrors to increase depth range, creating truer 3D. In vision applications, adaptive optics are used in robotic vision and surveillance cameras to provide real time or longdistance imaging. In microscopy, adaptive optics correct for aberrations in static lenses. Biomedical applications, including o ...
Australia-France PhD projects
... o Key questions: what is the beaming angle of GRBs? What is the nature of the progenitors? How are GRBs connected to supernovae? Population studies of GRBs. o Key questions: what is the rate GRBs in the universe? What fraction of GRBs can be detected by gravitational wave detectors? Are afterglows ...
... o Key questions: what is the beaming angle of GRBs? What is the nature of the progenitors? How are GRBs connected to supernovae? Population studies of GRBs. o Key questions: what is the rate GRBs in the universe? What fraction of GRBs can be detected by gravitational wave detectors? Are afterglows ...
Tech Notes Specialized www.ll.mit.edu
... Adaptive optics requires detectors with high fill factor—as an incident light spot shifts, so does the pattern of detector responses. Lincoln Laboratory has demonstrated an array of GM-APDs specifically tailored for adaptive optics uses. ...
... Adaptive optics requires detectors with high fill factor—as an incident light spot shifts, so does the pattern of detector responses. Lincoln Laboratory has demonstrated an array of GM-APDs specifically tailored for adaptive optics uses. ...
Telescope Errors NGAO - Caltech Optical Observatories
... – Move secondary toward primary • 1 cm at secondary, 74 cm at Cassegrain focus • Large spherical aberration (much larger than typical DM stroke) ...
... – Move secondary toward primary • 1 cm at secondary, 74 cm at Cassegrain focus • Large spherical aberration (much larger than typical DM stroke) ...
FIRSTSCOPE 60 - MODELS #21055 and #21055-DX
... The constant, mentioned above, is a relationship between your latitude and the angular distance the celestial pole is above the northern (or southern) horizon; The angular distance from the northern horizon to the north celestial pole is always equal to your latitude. To illustrate this, imagine tha ...
... The constant, mentioned above, is a relationship between your latitude and the angular distance the celestial pole is above the northern (or southern) horizon; The angular distance from the northern horizon to the north celestial pole is always equal to your latitude. To illustrate this, imagine tha ...
Lens defects / Aberration
... Moon is viewed through a telescope with an objective whose focal length is 53 cm and an eyepiece whose focal length is 25 mm. What is the angular size of the Moon as seen through this telescope? ...
... Moon is viewed through a telescope with an objective whose focal length is 53 cm and an eyepiece whose focal length is 25 mm. What is the angular size of the Moon as seen through this telescope? ...
New results on a Cn2 profiler for GeMS
... already complies with several WFSs and several guide sources, the SLODAR implementation was straightforward. Three main modifications to the classical SLODAR approach are however required. First the SLODAR is usually implemented with natural stars while the WFS of GeMS observe LGS at finite distance ...
... already complies with several WFSs and several guide sources, the SLODAR implementation was straightforward. Three main modifications to the classical SLODAR approach are however required. First the SLODAR is usually implemented with natural stars while the WFS of GeMS observe LGS at finite distance ...
Wide-field CCD imager for the 6.5m MMT telescope
... a large collecting area and large area coverage on the sky. Planned projects include redshift and photometric surveys of faint galaxies, searches for high-redshift quasars and searches for objects in the outer solar system. Keywords: CCDs, imaging, astronomy, telescopes, cameras ...
... a large collecting area and large area coverage on the sky. Planned projects include redshift and photometric surveys of faint galaxies, searches for high-redshift quasars and searches for objects in the outer solar system. Keywords: CCDs, imaging, astronomy, telescopes, cameras ...
J.Marque: Mode matching of the Virgo FP cavities
... cavity eigenmodes (radius of curvature of the mirrors of the cavity, length of the cavity). o This action can be performed by adjusting the position of the various optical elements of the telescope. o The input bench telescope has been designed to match the input beam to the FP cavities and minimize ...
... cavity eigenmodes (radius of curvature of the mirrors of the cavity, length of the cavity). o This action can be performed by adjusting the position of the various optical elements of the telescope. o The input bench telescope has been designed to match the input beam to the FP cavities and minimize ...
Word Format - US Scouting Service Project
... b. Describe the similarities and differences of several types of astronomical telescopes. ___________________________ ______________________________________________________________________________________________ _______________________________________________________________________________________ ...
... b. Describe the similarities and differences of several types of astronomical telescopes. ___________________________ ______________________________________________________________________________________________ _______________________________________________________________________________________ ...
astronomy discovery tour to india
... The site has been found to be good (about 150 cloud free nights per year) for astronomical observations. The specifications for surface finish of the telescope mirrors has been one-tenth of 589 nm line of sodium so that the telescope can be effectively used for imaging studies at both optical and in ...
... The site has been found to be good (about 150 cloud free nights per year) for astronomical observations. The specifications for surface finish of the telescope mirrors has been one-tenth of 589 nm line of sodium so that the telescope can be effectively used for imaging studies at both optical and in ...
Parallel-plate MEMS Mirror Design for Large On
... resonance. These characteristics make it suitable for implementation in several application areas such as spectroscopy, optical delay lines, and adaptive optics. There exist other types of movable mirrors with a variety of features. Magnetically actuated mirrors generally have large displacement and ...
... resonance. These characteristics make it suitable for implementation in several application areas such as spectroscopy, optical delay lines, and adaptive optics. There exist other types of movable mirrors with a variety of features. Magnetically actuated mirrors generally have large displacement and ...
User Manual Explore Scientific Truss Tube Dobsonian Telescopes
... Now take a look at the mirror box from above. You will notice threaded rods that are sticking out of the corners of the mirror box. There is a wing nut riding on each of those inward pointing threaded rods. Unscrew the wing nuts until the end of the threaded rods, but take care that they don´t come ...
... Now take a look at the mirror box from above. You will notice threaded rods that are sticking out of the corners of the mirror box. There is a wing nut riding on each of those inward pointing threaded rods. Unscrew the wing nuts until the end of the threaded rods, but take care that they don´t come ...
TAL
... accurately determine position of M2. Useful publishable discovery: when coma is tipped out on-axis, one of the two nodes of binodal astigmatism is also zero for this field point. Determined that A-scope is in need of calibration at around the 2’ level. ...
... accurately determine position of M2. Useful publishable discovery: when coma is tipped out on-axis, one of the two nodes of binodal astigmatism is also zero for this field point. Determined that A-scope is in need of calibration at around the 2’ level. ...
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.