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... This document describes the Palomar Observatory DBSP guider control software. The DBSP instrument is a dual channel spectrograph that simultaneously measures spectra in both the blue and red portions of t ...
... This document describes the Palomar Observatory DBSP guider control software. The DBSP instrument is a dual channel spectrograph that simultaneously measures spectra in both the blue and red portions of t ...
LIGO-T0900407-v4 - DCC - LIGO Document Control Center Portal
... cold sate is defined by the bean size and the ROC at the PRM. However, there may be certain scenarios where the mode at the PRM may change due to imperfect TCS or higher than expected thermal lensing in the IFO. For such cases, it will be advantageous to have two control knobs in the IO chain. This ...
... cold sate is defined by the bean size and the ROC at the PRM. However, there may be certain scenarios where the mode at the PRM may change due to imperfect TCS or higher than expected thermal lensing in the IFO. For such cases, it will be advantageous to have two control knobs in the IO chain. This ...
First steps of the development of a fiber optic piston sensor for
... Valeurs des pistons introduits (nm) ----------------------------------------------p1 : -50 p2 : 0 p3 :100 ...
... Valeurs des pistons introduits (nm) ----------------------------------------------p1 : -50 p2 : 0 p3 :100 ...
OBTAINING THE PROPERLY WEIGHTED AVERAGE ALBEDO OF
... to increase with decreasing size; however, this limit does not appear to significantly affect the average albedo. The same cannot be said about those data points below the line. Two of the objects (data points 1.1, 1.2 and 0.21, 4.9) have average albedos just above 80. This suggests that these two o ...
... to increase with decreasing size; however, this limit does not appear to significantly affect the average albedo. The same cannot be said about those data points below the line. Two of the objects (data points 1.1, 1.2 and 0.21, 4.9) have average albedos just above 80. This suggests that these two o ...
Optimal wave-front reconstruction strategies for
... We propose an optimal approach for the phase reconstruction in a large field of view (FOV) for multiconjugate adaptive optics. This optimal approach is based on a minimum-mean-square-error estimator that minimizes the mean residual phase variance in the FOV of interest. It accounts for the C 2n prof ...
... We propose an optimal approach for the phase reconstruction in a large field of view (FOV) for multiconjugate adaptive optics. This optimal approach is based on a minimum-mean-square-error estimator that minimizes the mean residual phase variance in the FOV of interest. It accounts for the C 2n prof ...
A Sixty-Year Timeline of the Air Force Maui Optical and
... (AMOS) has provided the U.S. Department of Defense (DoD) with space situational awareness capabilities from the island of Maui, Hawaii. AMOS is comprised of two separate facilities: the Maui Space Surveillance Complex (MSSC) and the Maui High Performance Computing Center (MHPCC). The MSSC is located ...
... (AMOS) has provided the U.S. Department of Defense (DoD) with space situational awareness capabilities from the island of Maui, Hawaii. AMOS is comprised of two separate facilities: the Maui Space Surveillance Complex (MSSC) and the Maui High Performance Computing Center (MHPCC). The MSSC is located ...
Astronomical seeing conditions as determined by turbulence modelling and optical measurement
... Modern space geodetic techniques are required to provide measurements of millimetrelevel accuracy. A new fundamental space geodetic observatory for South Africa has been proposed. It will house state-of-the-art equipment in a location that guarantees optimal scientific output. Lunar Laser Ranging (L ...
... Modern space geodetic techniques are required to provide measurements of millimetrelevel accuracy. A new fundamental space geodetic observatory for South Africa has been proposed. It will house state-of-the-art equipment in a location that guarantees optimal scientific output. Lunar Laser Ranging (L ...
7. Non-adaptive wavefront control
... The most important disturbance acting on the telescope structure is wind buffeting at different locations in the structure. Due to the large mass and the low resonance frequency of 2.6 Hz of the locked rotor mode only a limited control bandwidth is available. In addition the dynamical behaviour of t ...
... The most important disturbance acting on the telescope structure is wind buffeting at different locations in the structure. Due to the large mass and the low resonance frequency of 2.6 Hz of the locked rotor mode only a limited control bandwidth is available. In addition the dynamical behaviour of t ...
Slides
... MPPC Single pe observation at room temperature with 1.2 μs effective gate Initial Time Resolution Studies 137Cs Source spectrum for MPPC (time permitting) ...
... MPPC Single pe observation at room temperature with 1.2 μs effective gate Initial Time Resolution Studies 137Cs Source spectrum for MPPC (time permitting) ...
9 adaptive optics - Giant Magellan Telescope
... deformable mirror conjugated to the ground turbulence. The target for wavefront correction accuracy from the beacon system is 200 nm RMS under typical seeing conditions. This is chosen to give relatively good Strehl in the H band, 56% for a guide star on axis, degrading to 35% for a tilt star 1′ off ...
... deformable mirror conjugated to the ground turbulence. The target for wavefront correction accuracy from the beacon system is 200 nm RMS under typical seeing conditions. This is chosen to give relatively good Strehl in the H band, 56% for a guide star on axis, degrading to 35% for a tilt star 1′ off ...
T1000311-v7 TMS Hazards Analysis - DCC
... The steering mirrors and periscope mirrors will be adjusted to align the external 1064nm and 532nm reference beams with the ISC Optical Table optical path and the TMS Telescope optical path. The alignment laser presents a laser eye hazard, and an appropriate laser safe operating procedure must be fo ...
... The steering mirrors and periscope mirrors will be adjusted to align the external 1064nm and 532nm reference beams with the ISC Optical Table optical path and the TMS Telescope optical path. The alignment laser presents a laser eye hazard, and an appropriate laser safe operating procedure must be fo ...
D. Kampf
... Point sources at focal plane of top optics. Mask at photometers Field mirror for pupil alignment. Alignment of FOLD 4 and FOLD 5 using scatter plates at secondary mirror ...
... Point sources at focal plane of top optics. Mask at photometers Field mirror for pupil alignment. Alignment of FOLD 4 and FOLD 5 using scatter plates at secondary mirror ...
astronomical eyepieces - Amateur Astronomers Association Delhi
... of what kinds of eyepiece systems are available to the average amateur astronomer I-INTRODUCTION Eyepiece is assembly of lenses placed at focal point of objective of a telescope. They are also known as ocular lens. Eyepiece is used to magnify the image formed by objective lens or mirror of the teles ...
... of what kinds of eyepiece systems are available to the average amateur astronomer I-INTRODUCTION Eyepiece is assembly of lenses placed at focal point of objective of a telescope. They are also known as ocular lens. Eyepiece is used to magnify the image formed by objective lens or mirror of the teles ...
Herschel Observers` Manual
... The Herschel Space Observatory is an ESA cornerstone mission that was be launched on 14 May 2009, alongside the Plank cosmic microwave background mission. Originally known as FIRST (Far InfraRed Submillimetre Telescope) its name was officially changed in the year 2000 in recognition of the 200th ann ...
... The Herschel Space Observatory is an ESA cornerstone mission that was be launched on 14 May 2009, alongside the Plank cosmic microwave background mission. Originally known as FIRST (Far InfraRed Submillimetre Telescope) its name was officially changed in the year 2000 in recognition of the 200th ann ...
2014 - Society for Astronomical Sciences
... system is a challenge even for stars with spectral distributions similar to black bodies. Supernovae with more complex spectra, present additional difficulty ...
... system is a challenge even for stars with spectral distributions similar to black bodies. Supernovae with more complex spectra, present additional difficulty ...
TECHNICAL REPORT
... The Mid-Infrared Instrument (MIRI) on JWST is designed to obtain 5.6 - 25.5 µm images with a plate scale of 110 mas pix-1 and 5 - 14 µm low-resolution spectra of the most distant galaxies in the Universe, to study the formation of the first galaxies. As a result, MIRI is extremely sensitive and satu ...
... The Mid-Infrared Instrument (MIRI) on JWST is designed to obtain 5.6 - 25.5 µm images with a plate scale of 110 mas pix-1 and 5 - 14 µm low-resolution spectra of the most distant galaxies in the Universe, to study the formation of the first galaxies. As a result, MIRI is extremely sensitive and satu ...
THE CASSINI VISUAL AND INFRARED MAPPING SPECTROMETER
... The Cassini VIMS instrument has its roots in a long line of proposed imaging spectrometers, starting with a rudimentary instrument proposed for the Lunar Polar Orbiter in 1974. A more refined concept was proposed for the Mariner Jupiter Uranus (MJU) mission in 1975. This design was accepted for the ...
... The Cassini VIMS instrument has its roots in a long line of proposed imaging spectrometers, starting with a rudimentary instrument proposed for the Lunar Polar Orbiter in 1974. A more refined concept was proposed for the Mariner Jupiter Uranus (MJU) mission in 1975. This design was accepted for the ...
Test cryostat and OGSE
... Two liquid helium reservoirs: 70l for 4.2K and 13l for 1.7K level 90l liquid nitrogen for thermal shielding Optical bench 1060mm diameter, covered by super-insulated 4.2K thermal shield with 900mm available height Service life 10 hours with full PACS operation, 48 hours with PACS off FIR windows for ...
... Two liquid helium reservoirs: 70l for 4.2K and 13l for 1.7K level 90l liquid nitrogen for thermal shielding Optical bench 1060mm diameter, covered by super-insulated 4.2K thermal shield with 900mm available height Service life 10 hours with full PACS operation, 48 hours with PACS off FIR windows for ...
Astronomical Adaptive Optics using Multiple Laser Guide Stars
... University Library to be made available to borrowers under rules of the Library. Brief quotations from this dissertation are allowable without special permission, provided that accurate acknowledgment of source is made. Requests for permission for extended quotation from or reproduction of this manu ...
... University Library to be made available to borrowers under rules of the Library. Brief quotations from this dissertation are allowable without special permission, provided that accurate acknowledgment of source is made. Requests for permission for extended quotation from or reproduction of this manu ...
Design of PIAA Coronagraphs Over Square Apertures
... has been extremely active, and a variety of solutions for space based imaging of earth twins have been proposed and tested. Among these concepts, the Phase Induced Amplitude Apodisation coronagraph, first introduced by Guyon (2003), is a promising solution since it makes most of the photons collected ...
... has been extremely active, and a variety of solutions for space based imaging of earth twins have been proposed and tested. Among these concepts, the Phase Induced Amplitude Apodisation coronagraph, first introduced by Guyon (2003), is a promising solution since it makes most of the photons collected ...
Characterization of adaptive optics point spread function for
... this fundamentally limits the performance of all the deconvolution techniques. We present here a simple and analytical expression of this PSF degradation in the FOV and an application to a posteriori processing of wide FOV images. After a short presentation of the image formation in a wide FOV, a th ...
... this fundamentally limits the performance of all the deconvolution techniques. We present here a simple and analytical expression of this PSF degradation in the FOV and an application to a posteriori processing of wide FOV images. After a short presentation of the image formation in a wide FOV, a th ...
Parallax - Georgia State University
... • Use the baseline of the Earth; measure the angle through which a star moves. ...
... • Use the baseline of the Earth; measure the angle through which a star moves. ...
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.