LABORATORY MANUAL (Modern Physics & General Optics) PL – 402 (2013-2014)
... If we assume both grid and anode as plane parallel electrodes, when the temp. is low, the mean free path is large compare to any length scale in this tube and electron’s motion is ballistic. Electrons collected by the grid, then, is proportional to fraction of the area covered by the grid wire. When ...
... If we assume both grid and anode as plane parallel electrodes, when the temp. is low, the mean free path is large compare to any length scale in this tube and electron’s motion is ballistic. Electrons collected by the grid, then, is proportional to fraction of the area covered by the grid wire. When ...
System Level # Requirements Document
... IFU-based spectrometer operating over a wavelength range 0.8-2.5µm. Will use multiple IFUs and access a 5 arcmin diameter field. It is expected to benefit from developments in multi-object adaptive optics (MOAO). Mid-IR High-resolution Echelle Spectrometer (MIRES): Diffraction-limited, 5000 < R < ...
... IFU-based spectrometer operating over a wavelength range 0.8-2.5µm. Will use multiple IFUs and access a 5 arcmin diameter field. It is expected to benefit from developments in multi-object adaptive optics (MOAO). Mid-IR High-resolution Echelle Spectrometer (MIRES): Diffraction-limited, 5000 < R < ...
Optics business segment
... surveillance devices. Located in the Tucson Optics Valley, the facility boasts some of the region’s most advanced clean room, metrology, and process control capabilities all backed by highly skilled engineers and assembly technician staff. ...
... surveillance devices. Located in the Tucson Optics Valley, the facility boasts some of the region’s most advanced clean room, metrology, and process control capabilities all backed by highly skilled engineers and assembly technician staff. ...
Speckle Imaging through the Atmosphere
... this portion of the triple product, the length of the resultant noise phasor can be estimated as n3 / 2 . If M frames are chosen to average out the statistics of the atmosphere, the length of the resultant noise phasor is on the order of M I / 2 • n3 / 2 , and the desired signal vector is of length ...
... this portion of the triple product, the length of the resultant noise phasor can be estimated as n3 / 2 . If M frames are chosen to average out the statistics of the atmosphere, the length of the resultant noise phasor is on the order of M I / 2 • n3 / 2 , and the desired signal vector is of length ...
PPT-Version - EPS 2003, Aachen
... The light weight structure and the low inertia of the structure allows a fast slewing time in such a way that the telescope will be able to perform an early follow-up of a Gamma Ray Burst With the engines at 70% of full power, the telescope was able to move of ...
... The light weight structure and the low inertia of the structure allows a fast slewing time in such a way that the telescope will be able to perform an early follow-up of a Gamma Ray Burst With the engines at 70% of full power, the telescope was able to move of ...
3-DIMENSIONAL SPECTROSCOPIC-TOMOGRAPHY OF BIOLOGICAL MEMBRANE BY THE IMAGING-TYPE 2-D FOURIER SPECTROSCOPY
... becomes vague as if seen through frosted glass. We can observe only blood vessels that are near the skin surface and not greatly affected by diffusion. An image becomes a comparatively simple blood vessel pattern that enables personal identification. So, we decided to focus on a layer close to the s ...
... becomes vague as if seen through frosted glass. We can observe only blood vessels that are near the skin surface and not greatly affected by diffusion. An image becomes a comparatively simple blood vessel pattern that enables personal identification. So, we decided to focus on a layer close to the s ...
Laser guide star adaptive optics at the Keck Observatory
... First corrected images on NIRC2 with laser LGS AO facility operable by AO experts First LGS AO engineering science LGS AO observing strategy decision First shared-risk science First light engineering science paper LGS AO facility operable for science by OA and one expert First queue/non-shared scien ...
... First corrected images on NIRC2 with laser LGS AO facility operable by AO experts First LGS AO engineering science LGS AO observing strategy decision First shared-risk science First light engineering science paper LGS AO facility operable for science by OA and one expert First queue/non-shared scien ...
Optical Fabrication and Testing - National Optical Astronomy
... • Active and adaptive compensation for wind buffeting • Adaptive correction of atmospheric turbulence • Segment co-alignment and phasing • Tip-tilt control of secondary mirror ...
... • Active and adaptive compensation for wind buffeting • Adaptive correction of atmospheric turbulence • Segment co-alignment and phasing • Tip-tilt control of secondary mirror ...
Design, fabrication, and open-loop control of micro deformable mirrors for Contents
... ground-based instrument intended for observation of Jovian exoplanets, with the help of high spatial resolution DMs having thousands of control points. In addition to exoplanet detection, such an ExAO system will be capable of characterizing dust disks around stars and will allow high Strehl ratio i ...
... ground-based instrument intended for observation of Jovian exoplanets, with the help of high spatial resolution DMs having thousands of control points. In addition to exoplanet detection, such an ExAO system will be capable of characterizing dust disks around stars and will allow high Strehl ratio i ...
月面環境評価 - cosmos.ru
... • Size：Reflection Efficiency more than A11 or A15 • Structure： Hard to be affected by gravitational and thermal effects • Optical Performance：Ray tracing simulation • Dihedral Angle Offset：What is the optimal value ? • Adaptive Optics：Option ...
... • Size：Reflection Efficiency more than A11 or A15 • Structure： Hard to be affected by gravitational and thermal effects • Optical Performance：Ray tracing simulation • Dihedral Angle Offset：What is the optimal value ? • Adaptive Optics：Option ...
mach-zehnder wavefront sensor for phasing of segmented
... simulations, showing that with proper settings of the interferometer’s parameters, the technique can be made insensitive to atmospheric turbulence and, more generally, to almost any error source not associated with the segmentation. It also appears that, in a telescope that would include more than o ...
... simulations, showing that with proper settings of the interferometer’s parameters, the technique can be made insensitive to atmospheric turbulence and, more generally, to almost any error source not associated with the segmentation. It also appears that, in a telescope that would include more than o ...
Conventional Mirror Technology - The University of Arizona College
... Concept demonstrated, now being optimized for production Achieves 25 nm resolution at 77K Requires zero hold power 5 mm total travel, F > 100 g ...
... Concept demonstrated, now being optimized for production Achieves 25 nm resolution at 77K Requires zero hold power 5 mm total travel, F > 100 g ...
Experiment 24 - School of Physics
... Figure 24-1 shows the layout of the Michelson interferometer used in this experiment. The mirrors, beamsplitter and compensator plate are mounted on a marble slab for stability. The apparatus is housed in a clear plastic box to exclude drafts and to keep the optics clean. Light from the source is sp ...
... Figure 24-1 shows the layout of the Michelson interferometer used in this experiment. The mirrors, beamsplitter and compensator plate are mounted on a marble slab for stability. The apparatus is housed in a clear plastic box to exclude drafts and to keep the optics clean. Light from the source is sp ...
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... monitoring and controlling the Hale 200” telescope. FACSUM allows users to manage astronomical target lists, visualize the spatial distribution of astronomical targets and send selected target positions directly ...
... monitoring and controlling the Hale 200” telescope. FACSUM allows users to manage astronomical target lists, visualize the spatial distribution of astronomical targets and send selected target positions directly ...
The Four-Quadrant Phase-Mask Coronagraph. I. Principle
... the interferometric coronagraph imagined by Bracewell (1978), where the light from several distant telescopes is combined with a n phase shift applied on half of the beams. Here, we are concerned only with single-aperture telescopes, the angular resolution of which is suited for the detection of out ...
... the interferometric coronagraph imagined by Bracewell (1978), where the light from several distant telescopes is combined with a n phase shift applied on half of the beams. Here, we are concerned only with single-aperture telescopes, the angular resolution of which is suited for the detection of out ...
Modeling the Spectral Energy Distributions and Variability
... Optical afterglow of GRB 990510 (May 10, 1999) Optical afterglows of GRBs are extremely difficult to localize: Very faint (~ 18 – 20 mag.); decaying within a few days. ...
... Optical afterglow of GRB 990510 (May 10, 1999) Optical afterglows of GRBs are extremely difficult to localize: Very faint (~ 18 – 20 mag.); decaying within a few days. ...
Stable Operation of a 300-m Laser Interferometer with Sufficient
... for the stable operation of the interferometer, this system can introduce excess noise to the interferometer [18]. The noise in the alignment control error signal causes displacement noise by coupling with miscentering of the beam on a mirror, and efficiency asymmetries of the coil-magnet actuators ...
... for the stable operation of the interferometer, this system can introduce excess noise to the interferometer [18]. The noise in the alignment control error signal causes displacement noise by coupling with miscentering of the beam on a mirror, and efficiency asymmetries of the coil-magnet actuators ...
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.