High-order wavefront sensing system for PALM-3000 Christoph Baranec
... optics system to support observations with the Well-Corrected Subaperture12 project, which will also be supported in the PALM-3000 upgrade. The spatial filter used in PALM-3000 will have a maximum aperture size of 4 arc sec (1.56 mm) for guiding on solar system objects, and a minimum size of 0.48 ar ...
... optics system to support observations with the Well-Corrected Subaperture12 project, which will also be supported in the PALM-3000 upgrade. The spatial filter used in PALM-3000 will have a maximum aperture size of 4 arc sec (1.56 mm) for guiding on solar system objects, and a minimum size of 0.48 ar ...
Sensor Modeling and Demonstration of a Multi-Object Spectrometer for Performance-Driven Sensing
... 3.1 Multi-object spectrometer modeling An adaptive multimodal optical sensor at the heart of a performance-driven sensor system is an imaging device with the capability of interacting with a performance-driven algorithm to detect, identify, and track targets in real-time using multiple modalities. ...
... 3.1 Multi-object spectrometer modeling An adaptive multimodal optical sensor at the heart of a performance-driven sensor system is an imaging device with the capability of interacting with a performance-driven algorithm to detect, identify, and track targets in real-time using multiple modalities. ...
IRMOS: The near-InfraRed Multi-Object
... Meter Telescope (TMT) project (www.tmt.org). This paper presents a status report of the University of Florida (UF) and Herzberg Institute of Astrophysics (HIA) concept for IRMOS, which has recently completed its feasibility study phase. IRMOS is best summarized as a Multi-Object Adaptive Optics (MOA ...
... Meter Telescope (TMT) project (www.tmt.org). This paper presents a status report of the University of Florida (UF) and Herzberg Institute of Astrophysics (HIA) concept for IRMOS, which has recently completed its feasibility study phase. IRMOS is best summarized as a Multi-Object Adaptive Optics (MOA ...
Cvetojevic_PIMMS_11 - School of Physics
... We have successfully demonstrated the first IPS-like device on a telescope, with spectra taken from 3 different types of stars. Currently, redesigning the AWG chips to improve FSR, R, Wavelength ...
... We have successfully demonstrated the first IPS-like device on a telescope, with spectra taken from 3 different types of stars. Currently, redesigning the AWG chips to improve FSR, R, Wavelength ...
5. System Engineering
... reflect constraints and objectives not directly related to scientific objectives but to technical, programmatic, or even legal considerations (e.g. compliance with legal safety standards). At this stage, characteristics covered by OWL Level 1 Requirements are generally given two values (or two set o ...
... reflect constraints and objectives not directly related to scientific objectives but to technical, programmatic, or even legal considerations (e.g. compliance with legal safety standards). At this stage, characteristics covered by OWL Level 1 Requirements are generally given two values (or two set o ...
poster208
... consistent with envelope material recently heated by a central massive (proto)star (see Fig. 3). This suggests that the observed sources may have experienced a prestellar phase with gas temperature similar to those in the nearby low-mass cores (~10 K). ...
... consistent with envelope material recently heated by a central massive (proto)star (see Fig. 3). This suggests that the observed sources may have experienced a prestellar phase with gas temperature similar to those in the nearby low-mass cores (~10 K). ...
A spherical mirror - College of Optical Sciences
... Position a ball at focus of the 0th order diffraction beam after CGH, use it as a reference to position the spherical mirror. Put a few balls at the mirror surface, patches of CGH direct spherical beams toward the ball and the reflection fringes are used to position the balls accurately in lateral d ...
... Position a ball at focus of the 0th order diffraction beam after CGH, use it as a reference to position the spherical mirror. Put a few balls at the mirror surface, patches of CGH direct spherical beams toward the ball and the reflection fringes are used to position the balls accurately in lateral d ...
Problem Statement
... Sometime after launch on 4/24/1990, engineers testing images from the Hubble Space Telescope (HST) noticed that the images were blurry. They were unable to focus the image through normal equipment adjustments. The blurry images were determined through testing to be a form of spherical aberration. Sp ...
... Sometime after launch on 4/24/1990, engineers testing images from the Hubble Space Telescope (HST) noticed that the images were blurry. They were unable to focus the image through normal equipment adjustments. The blurry images were determined through testing to be a form of spherical aberration. Sp ...
Deployment of the Hobby-Eberly Telescope wide
... the telescope correctly aligned. The WFC is a four-mirror design with two concave 1 meter diameter mirrors, one concave 0.9 meter diameter mirror, and one convex 0.23 m diameter mirror. The corrector is designed for feeding optical fibers at f/3.65 to minimize focal ratio degradation, and so the chi ...
... the telescope correctly aligned. The WFC is a four-mirror design with two concave 1 meter diameter mirrors, one concave 0.9 meter diameter mirror, and one convex 0.23 m diameter mirror. The corrector is designed for feeding optical fibers at f/3.65 to minimize focal ratio degradation, and so the chi ...
Homework #2, AST 1002, Fall 2015
... Which of the following is (are) common to all planets? (a) Their orbital planes are near the ecliptic plane. (b) They revolve eastward (counterclockwise) around the Sun. (c) Their axes of rotation lie very near the ecliptic plane. The correct answer(s) is(are) ____________. 13. A 5500 Angstrom sourc ...
... Which of the following is (are) common to all planets? (a) Their orbital planes are near the ecliptic plane. (b) They revolve eastward (counterclockwise) around the Sun. (c) Their axes of rotation lie very near the ecliptic plane. The correct answer(s) is(are) ____________. 13. A 5500 Angstrom sourc ...
collimating an astro-tech AT10RC
... on Page 1, the optical axis of the scope (the primary mirror/baffle tube assembly) will rarely need collimation. If the optical axis does get knocked out of collimation, however, the image through the Cheshire eyepiece will appear to be shifted to one side within the light ring formed by the end of ...
... on Page 1, the optical axis of the scope (the primary mirror/baffle tube assembly) will rarely need collimation. If the optical axis does get knocked out of collimation, however, the image through the Cheshire eyepiece will appear to be shifted to one side within the light ring formed by the end of ...
T1000700-v2 Transmon Telescope Mirror Test Procedure
... aligns with the horizontal cross line on the reference mirror target. Iterate these steps until the autocollimator is aligned perpendicular to reference mirror and is 5.13 in height. This completes the alignment of Autocollimator #1; it must not be moved during the remainder of the telescope ...
... aligns with the horizontal cross line on the reference mirror target. Iterate these steps until the autocollimator is aligned perpendicular to reference mirror and is 5.13 in height. This completes the alignment of Autocollimator #1; it must not be moved during the remainder of the telescope ...
LaPalma_2013_Hook
... • A concave spherical mirror suffers from severe spherical aberration and has limited use without additional optics (more about this later) • A concave paraboloid focuses light to a perfect image on its axis but suffers from coma (~1/F2) and astigmatism off-axis • For long focal ratios (f/4 and grea ...
... • A concave spherical mirror suffers from severe spherical aberration and has limited use without additional optics (more about this later) • A concave paraboloid focuses light to a perfect image on its axis but suffers from coma (~1/F2) and astigmatism off-axis • For long focal ratios (f/4 and grea ...
Astrograph Technical
... ASA Newtonian astrographs all use a fast optical system (hence a small f/#) and are capable of working at multiple focal lengths. This means you can achieve good signal-to-noise ratio with your CCD using short exposure times. The N-series astrographs all have a natural focal ratio of f/3.8, without ...
... ASA Newtonian astrographs all use a fast optical system (hence a small f/#) and are capable of working at multiple focal lengths. This means you can achieve good signal-to-noise ratio with your CCD using short exposure times. The N-series astrographs all have a natural focal ratio of f/3.8, without ...
LaPalma_telescopes_2008
... design, this leads to acceptable image quality and is widely used in smaller telescopes For larger apertures a shorter focal ratio is essential and the field of tolerable aberration becomes very small Large telescopes, if they have a prime focus, need correctors (more later). Hyperbolic primaries ca ...
... design, this leads to acceptable image quality and is widely used in smaller telescopes For larger apertures a shorter focal ratio is essential and the field of tolerable aberration becomes very small Large telescopes, if they have a prime focus, need correctors (more later). Hyperbolic primaries ca ...
Interdisciplinary Evolution of the Hubble Space Telescope
... the physical universe – many believed that our galaxy was the only galaxy. Before WWII most astronomy was conducted by individuals or small groups, and astronomical observatories were funded by private philanthropists (example: Carnegie) or by an individual astronomer (example: Percival Lowell). By ...
... the physical universe – many believed that our galaxy was the only galaxy. Before WWII most astronomy was conducted by individuals or small groups, and astronomical observatories were funded by private philanthropists (example: Carnegie) or by an individual astronomer (example: Percival Lowell). By ...
36x48 vertical poster template
... guide stars, to verify that the pointing control is stable when using a faint guide star. The 10458 observations tested the telescope’s ability to reacquire guide stars across occultation, while program 10459 used the same observing sequence with NGC 2298 as a CVZ object to test the tracking over 90 ...
... guide stars, to verify that the pointing control is stable when using a faint guide star. The 10458 observations tested the telescope’s ability to reacquire guide stars across occultation, while program 10459 used the same observing sequence with NGC 2298 as a CVZ object to test the tracking over 90 ...
031031_St_Wkshop
... – What kind of scientific observations? – Big telescope Big instrument optics – Making good use of your observing time • New Ones – The SALT prime focus – New optics: holography Oct 30, 2003 ...
... – What kind of scientific observations? – Big telescope Big instrument optics – Making good use of your observing time • New Ones – The SALT prime focus – New optics: holography Oct 30, 2003 ...
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.