Optical Techniques for Atmospheric Cross-Wind Profiling
|
|
- Osborn Holmes
- 5 years ago
- Views:
Transcription
1 Optical Techniques for Atmospheric Cross-Wind Profiling Dr. Mikhail A. Vorontsov, Army Research Laboratory, CISD, Intelligent Optics Lab. and University of Maryland, College Park, Intelligent Optics , www://iol.umd.edu Dr. Miao Yu, University of Maryland, College Park, Mechanical Eng. Dep. Single-pass propagation Double-pass propagation
2 Wind-profiling Based on Intensity Scintillation Measurements Light source Phase-distorting layer moving with wind velocity v Fast-framing camera v
3 Phase Distorting Layer Location and Intensity Scintillations Light source Phase-distorting layer moving with wind velocity v f v e d c Fast-framing camera a a b ac b Phase screen ad ae af
4 Intensity Scintillation Correlation Technique: Single Turbulence Layer Correlation function C( x = a, y b, Δt) = I( x, y, t) I( x + x a, y + y b, t + Δt) dxdy I Intensity distribution ( x, y, t) L 1 L R ϕ p ϕ v A in I( x, y, t) Intensity distribution at time t Taylor hypothesis: Moving turbulent layers are frozen Intensity at t Correlation between two images (a,b) coordinate of the correlation peak maximum a = v t b = v t x Δ y Δ Intensity at t+δt (a,b) f s = 1/ Δt Sampling frequency Wind velocity: v x = a Δt v y = b Δt
5 Digital Processing of a Set of Short-Exposure Scintillation Patterns Example 1: Sampling frequency 66 fr/sec. DALSA camera (256x256 pixels) receiver aperture diameter D=15 mm v x (m/s) t (s) v y (m/s) t (s) Wind velocity v x 1.35m/s, v y.81m/s 1 pixel shift corresponds to.27m/s Intensity at pupil plane Wind direction
6 Digital Processing of a Set of Short-Exposure Scintillation Patterns Example 2: Sampling frequency 83 Hz, receiver aperture size.42cm Wind velocity v x m/s, v y m/s 1 pixel shift/step=.42cm 83Hz=.34m/s Intensity at pupil plane Wind velocity v x Wind velocity v y Wind velocity
7 Multiple Turbulent Layers: Numerical Simulations Image of cross-correlation Multiple phase-distorting layers L=.25 ka Finding peaks of the correlation function corresponding to each phase-distorting layer The size of the peak corresponding to the distance of phase-distorting layer Sensitive to wind velocity difference between different phase-distorting layers and strength of turbulence dz 1 =.4 dz 2 =.45 dz 1 =.5 dz 2 =
8 Correlation Peak Enhancement Via Moving Camera Two phase-distorting layers Scanning receiver image plane Enhance peaks of correlation function C s ( x, y) L = C( x, y, z) dz D/r =1 V d = a 1 b D/r =4 2 V d =.1
9 Correlation Peak Enhancement Via Phase-Image Diffraction Two distant phase distorting layers Use pupil-plane intensity as input of the wavefront corrector Propagate beam to the matched distance (.1 and.5) to get output intensity 1 & 2 Perform the same process as single phase-distorting layer case to get wind velocity for both phase screens
10 Correlation Peak Enhancement Via Phase-Image Diffraction Two distant phase-distorting layers Example: simulation results Input wind velocity: v = sin( nδt / 2 ) v 2 = 5 1 π Pupil-plane intensity Wind velocity for phase screen 1 Wind velocity for phase screen 2
11 Wind Profiling Based on Intensity Scintillations Analysis: Atmospheric Experiment Telescope and wind sensor 2.3 km Intelligent Optics Laboratory Water Tower
12 Wind Profiling Based on Intensity Scintillations Analysis: Experimental Results Telescope laser Experimental Parameters: Telescope aperture size:15cm CCD camera sampling rate: 25 Hz t t+δt Correlation Receiver aperture size resolution: Wind sensor located at the pupil plane NovaLynx Corporation Weather Monitoring Instruments and Systems
13 Wind speed (mph) Wind speed(mph) wind speed from intensity scintillations wind sensor data 1:37:55 1:4:48 1:43:41 1:46:34 1:49:26 1:52:19 Time Wind Profiling Based on Intensity Scintillations Analysis: Experimental Results Wind data acquired from 1:38am to 1:52am on July 5 25: Wind data acquired from 11:5am to 12:24pm on July 15 25: wind sensor data wind speed from intensity scintillations 11:48:29 11:55:41 12:2:53 12:1:5 12:17:17 12:24:29 Time Negative wind data corresponding to east wind and positive wind data corresponding to west wind Wind direction: south west to south east Wind direction: east
14 Wind Profiling Using Differential Nonlinear Zernike Filter Correlation of intensity I dif + ( r) = I ( r) I ( r) = 8πF I ( r) I () sin[ ϕ( r) Δ] zer zer F D/r =1 V d =.2 DNZF Visualized screen Visualized screen scanning and visualizing the image plane of each distant phasedistorting layer the dominant correlation peak corresponds to the visualized phase-distorting layer Comparison of correlation function using DNZF and without DNZF for two phase screens
Wavefront errors due to atmospheric turbulence Claire Max
Wavefront errors due to atmospheric turbulence Claire Max Page 1 Kolmogorov turbulence, cartoon solar Outer scale L 0 Inner scale l 0 h Wind shear convection h ground Page Atmospheric Turbulence generally
More informationAperture-Averaging - Theory and Measurements
Aperture-Averaging - Theory and Measurements N. Perlot, D. Fritzsche German Aerospace Center (DLR), D-834 Wessling, Germany ABSTRACT Atmospheric laser communications using direct-detection systems do suffer
More informationSpeckles and adaptive optics
Chapter 9 Speckles and adaptive optics A better understanding of the atmospheric seeing and the properties of speckles is important for finding techniques to reduce the disturbing effects or to correct
More informationOn the possibility to create a prototype of laser system for space debris movement control on the basis of the 3-meter telescope.
OJC «RPC «Precision Systems and Instruments», Moscow, Russia A. Alexandrov, V. Shargorodskiy On the possibility to create a prototype of laser system for space debris movement control on the basis of the
More information1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO?
Astronomy 418/518 final practice exam 1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO? b. Describe the visibility vs. baseline for a two element,
More informationThe IPIE Adaptive Optical System Application For LEO Observations
The IPIE Adaptive Optical System Application For LEO Observations Eu. Grishin (1), V. Shargorodsky (1), P. Inshin (2), V. Vygon (1) and M. Sadovnikov (1) (1) Open Joint Stock Company Research-and-Production
More informationsolar telescopes Solar Physics course lecture 5 Feb Frans Snik BBL 707
Solar Physics course lecture 5 Feb 19 2008 Frans Snik BBL 707 f.snik@astro.uu.nl www.astro.uu.nl/~snik solar vs. nighttime telescopes solar constant: 1.37 kw/m 2 destroys optics creates seeing solar vs.
More informationMcMath-Pierce Adaptive Optics Overview. Christoph Keller National Solar Observatory, Tucson
McMath-Pierce Adaptive Optics Overview Christoph Keller National Solar Observatory, Tucson Small-Scale Structures on the Sun 1 arcsec Important astrophysical scales (pressure scale height in photosphere,
More informationAnalysis of the Sequence Of Phase Correction in Multiconjugate Adaptive Optics
Analysis of the Sequence Of Phase Correction in Multiconjugate Adaptive Optics Luzma Montoya, Iciar Montilla Instituto de Astrofísica de Canarias Edinburgh, 25-26/03/2014 AO Tomography Workshop The EST
More informationSky demonstration of potential for ground layer adaptive optics correction
Sky demonstration of potential for ground layer adaptive optics correction Christoph J. Baranec, Michael Lloyd-Hart, Johanan L. Codona, N. Mark Milton Center for Astronomical Adaptive Optics, Steward Observatory,
More informationPolarization Shearing Interferometer (PSI) Based Wavefront Sensor for Adaptive Optics Application. A.K.Saxena and J.P.Lancelot
Polarization Shearing Interferometer (PSI) Based Wavefront Sensor for Adaptive Optics Application A.K.Saxena and J.P.Lancelot Adaptive Optics A Closed loop Optical system to compensate atmospheric turbulence
More informationDisturbance Feedforward Control for Vibration Suppression in Adaptive Optics of Large Telescopes
Disturbance Feedforward Control for Vibration Suppression in Adaptive Optics of Large Telescopes Martin Glück, Jörg-Uwe Pott, Oliver Sawodny Reaching the Diffraction Limit of Large Telescopes using Adaptive
More informationWavefront Correction of Model-based Sensorless Adaptive Optics System
Wavefront Correction of Model-based Sensorless Adaptive Optics System Huizhen Yang 1*, Jian Wu 2 1. School of Electronic Engineering, Huaihai Institute of Technology, Lianyungang, China 222005; 2. School
More informationAdaptive Optics Lectures
Adaptive Optics Lectures 1. Atmospheric turbulence Andrei Tokovinin 1 Resources CTIO: www.ctio.noao.edu/~atokovin/tutorial/index.html CFHT AO tutorial: http://www.cfht.hawaii.edu/instruments/imaging/aob/other-aosystems.html
More informationAstronomical Optics. Second Edition DANIEL J. SCHROEDER ACADEMIC PRESS
Astronomical Optics Second Edition DANIEL J. SCHROEDER Professor of Physics and Astronomy, Emeritus Department of Physics and Astronomy Beloit College, Beloit, Wisconsin ACADEMIC PRESS A Harcourt Science
More informationGround Layer Laser Seeing Meter
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC, 16:31 318, 014 March 014. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. Ground Layer Laser Seeing Meter S. CAVAZZANI,
More informationTECHNICAL RESEARCH REPORT
TECHNICAL RESEARCH REPORT Advanced Phase-Contrast Techniques for Wavefront Sensing and Adaptive Optics by M.A. Vorontsov, E.W. Justh, and L.A. Beresnev CDCSS TR 1-4 (ISR TR 1-7) C + - D S CENTER FOR DYNAMICS
More informationTechnical Note Turbulence/Optical Quick-Reference Table
Quick Reference Table of Turbulence and Optical Relations and Equivalents Matthew R. Whiteley, Ph.D. MZA Associates Corporation, 36 Technology Court, Suite 937-684-4 x, Matthew.Whiteley@mza.com General
More informationTitle. Statistical behaviour of optical vortex fields. F. Stef Roux. CSIR National Laser Centre, South Africa
. p.1/37 Title Statistical behaviour of optical vortex fields F. Stef Roux CSIR National Laser Centre, South Africa Colloquium presented at School of Physics National University of Ireland Galway, Ireland
More informationWavefront Sensing using Polarization Shearing Interferometer. A report on the work done for my Ph.D. J.P.Lancelot
Wavefront Sensing using Polarization Shearing Interferometer A report on the work done for my Ph.D J.P.Lancelot CONTENTS 1. Introduction 2. Imaging Through Atmospheric turbulence 2.1 The statistics of
More informationA novel laser guide star: Projected Pupil Plane Pattern
A novel laser guide star: Projected Pupil Plane Pattern Huizhe Yang a, Nazim Barmal a, Richard Myers a, David F. Buscher b, Aglae Kellerer c, Tim Morris a, and Alastair Basden a a Department of Physics,
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationAOL Spring Wavefront Sensing. Figure 1: Principle of operation of the Shack-Hartmann wavefront sensor
AOL Spring Wavefront Sensing The Shack Hartmann Wavefront Sensor system provides accurate, high-speed measurements of the wavefront shape and intensity distribution of beams by analyzing the location and
More informationPropagation Channel Characterization: Impact on Optical Systems Performance
Propagation Channel Characterization: Impact on Optical Systems Performance Marie-Thérèse Velluet, Clélia Robert, Nicolas Védrenne ONERA, The French Aerospatial Lab, 92322 Chatillon Cedex FRANCE marie-therese.velluet@onera.fr,
More informationModern Observational/Instrumentation Techniques Astronomy 500
Modern Observational/Instrumentation Techniques Astronomy 500 Andy Sheinis, Sterling 5520,2-0492 sheinis@astro.wisc.edu MW 2:30, 6515 Sterling Office Hours: Tu 11-12 Hardware 1 Telescopes What parameters
More informationABSTRACT 1. INTRODUCTION
FASS: The full aperture seeing sensor A.Guesalaga *,1, J.Osborn 2, M.Sarazin 3, B.Neichel 4, S. Perera 2, R.Wilson 2 1 Pontificia Universidad Católica de Chile, 4860 Vicuña Mackenna, 7820436 Santiago,
More informationAn Introduction to. Adaptive Optics. Presented by. Julian C. Christou Gemini Observatory
An Introduction to Adaptive Optics Presented by Julian C. Christou Gemini Observatory Gemini North in action Turbulence An AO Outline Atmospheric turbulence distorts plane wave from distant object. How
More informationAstronomical Seeing. Northeast Astro-Imaging Conference. Dr. Gaston Baudat Innovations Foresight, LLC. April 7 & 8, Innovations Foresight
Astronomical Seeing Northeast Astro-Imaging Conference April 7 & 8, 2016 Dr. Gaston Baudat, LLC 1 Seeing Astronomical seeing is the blurring of astronomical objects caused by Earth's atmosphere turbulence
More information7. Telescopes: Portals of Discovery Pearson Education Inc., publishing as Addison Wesley
7. Telescopes: Portals of Discovery Parts of the Human Eye pupil allows light to enter the eye lens focuses light to create an image retina detects the light and generates signals which are sent to the
More informationControl of the Keck and CELT Telescopes. Douglas G. MacMartin Control & Dynamical Systems California Institute of Technology
Control of the Keck and CELT Telescopes Douglas G. MacMartin Control & Dynamical Systems California Institute of Technology Telescope Control Problems Light from star Primary mirror active control system
More informationWhat do companies win being a supplier to ESO
What do companies win being a supplier to ESO Arnout Tromp Head of Contracts and Procurement Topics Characteristics of what ESO procures Technology in Astronomy Spin off from the past The future: E-ELT
More informationSPATIO-TEMPORAL PREDICTION FOR ADAPTIVE OPTICS WAVEFRONT RECONSTRUCTORS
SPATIO-TEMPORAL PREDICTION FOR ADAPTIVE OPTICS WAVEFRONT RECONSTRUCTORS Michael Lloyd-Hart and Patrick McGuire Center for Astronomical Adaptive Optics, Steward Observatory, University of Arizona, Tucson,
More informationSky Projected Shack-Hartmann Laser Guide Star
Sky Projected Shack-Hartmann Laser Guide Star T. Butterley a, D.F. Buscher b, G. D. Love a, T.J. Morris a, R. M. Myers a and R. W. Wilson a a University of Durham, Dept. of Physics, Rochester Building,
More informationInterference, Diffraction and Fourier Theory. ATI 2014 Lecture 02! Keller and Kenworthy
Interference, Diffraction and Fourier Theory ATI 2014 Lecture 02! Keller and Kenworthy The three major branches of optics Geometrical Optics Light travels as straight rays Physical Optics Light can be
More informationCHARA Meeting 2017 Pasadena, California
MORE AUTOMATION Laszlo Sturmann M7 ACTUATORS LAB. LASER ALIGNMENT TELESCOPE OPTICAL ALIGNMENT NEW ACTUATORS REMOTELY ACTUATED M7 MOUNT MOTIVATION THE PRECISION OF THE COUDE ALIGNMENT WAS NOT SUFFICIENT
More informationInternational Journal of Scientific & Engineering Research, Volume 4, Issue 7, July ISSN
International Journal of Scientific & Engineering Research, Volume 4, Issue 7, July-2013 96 Performance and Evaluation of Interferometric based Wavefront Sensors M.Mohamed Ismail1, M.Mohamed Sathik2 Research
More informationTechniques for direct imaging of exoplanets
Techniques for direct imaging of exoplanets Aglaé Kellerer Institute for Astronomy, Hawaii 1. Where lies the challenge? 2. Contrasts required for ground observations? 3. Push the contrast limit Recycle!
More informationResponse of DIMM turbulence sensor
Response of DIMM turbulence sensor A. Tokovinin Version 1. December 20, 2006 [tdimm/doc/dimmsensor.tex] 1 Introduction Differential Image Motion Monitor (DIMM) is an instrument destined to measure optical
More informationAn Example of Telescope Resolution
An Example of Telescope Resolution J. Kielkopf September 23, 2012 1 Principles Light leaves a distant source with the properties of a spherical wave. That is, the phase of the wave is constant on the surface
More informationRestoration of atmospherically blurred images according to weather-predicted atmospheric modulation transfer functions
Restoration of atmospherically blurred images according to weather-predicted atmospheric modulation transfer functions Yitzhak Yitzhaky, MEMBER SPIE Itai Dror Norman S. Kopeika, MEMBER SPIE Ben-Gurion
More informationMicro-fluctuations of Fried s parameter (r 0 )
Micro-fluctuations of Fried s parameter ( ) S. K. Saha and L. Yeswanth Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India e-mail: sks@iiap.res.in; sks@iiap.ernet.in The atmospheric
More informationWavefront reconstruction for adaptive optics. Marcos van Dam and Richard Clare W.M. Keck Observatory
Wavefront reconstruction for adaptive optics Marcos van Dam and Richard Clare W.M. Keck Observatory Friendly people We borrowed slides from the following people: Lisa Poyneer Luc Gilles Curt Vogel Corinne
More informationCollaborative Site Testing in West China,
Collaborative Site Testing in West China, comparing with Subaru and Okayama Toshiyuki Sasaki (NAOJ) on behalf of Site Survey Team Prof. Yongqiang Yao (NAOC/China), M. Yoshida(Hiroshima-u), N. Ohshima,
More informationLaboratory Experiments of Laser Tomographic Adaptive Optics at Visible Wavelengths on a 10-meter Telescope
1st AO4ELT conference, 08005 (2010) DOI:10.1051/ao4elt/201008005 Owned by the authors, published by EDP Sciences, 2010 Laboratory Experiments of Laser Tomographic Adaptive Optics at Visible Wavelengths
More informationSeptember 9, Wednesday 3. Tools for Solar Observations-I
September 9, Wednesday 3. Tools for Solar Observations-I Solar telescopes. Resolution, MTF, seeing. High resolution telescopes. Spectrographs. Types of Solar Observations Electro-magnetic observations
More informationA down-to-earth guide to high-resolution solar observations. Kevin Reardon National Solar Observatory
A down-to-earth guide to high-resolution solar observations Kevin Reardon kreardon@nso.edu National Solar Observatory Seeing Adaptive Optics Image Reconstruction Atmospheric Effects Spectral Lines Calibration
More informationA NEW METHOD FOR ADAPTIVE OPTICS POINT SPREAD FUNCTION RECONSTRUCTION
Florence, Italy. May 2013 ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13328 A NEW METHOD FOR ADAPTIVE OPTICS POINT SPREAD FUNCTION RECONSTRUCTION J. Exposito 1a, D. Gratadour 1, G. Rousset 1, Y. Clénet
More informationPHY410 Optics Exam #3
PHY410 Optics Exam #3 NAME: 1 2 Multiple Choice Section - 5 pts each 1. A continuous He-Ne laser beam (632.8 nm) is chopped, using a spinning aperture, into 500 nanosecond pulses. Compute the resultant
More informationField Tests of elongated Sodium LGS wave-front sensing for the E-ELT
Florence, Italy. May 2013 ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13437 Field Tests of elongated Sodium LGS wave-front sensing for the E-ELT Gérard Rousset 1a, Damien Gratadour 1, TIm J. Morris 2,
More informationarxiv:astro-ph/ v1 5 Nov 1999
Rayleigh scattering and laser spot elongation problems at ALFA arxiv:astro-ph/9911086v1 5 Nov 1999 E. Viard (eviard@eso.org), F. Delplancke (fdelplan@eso.org) and N. Hubin (nhubin@eso.org) European Southern
More informationSimple quasi-common path point diffraction interferometer with adjustable fringe contrast and carrier frequency
J. Eur. Opt. Soc.-Rapid, 54 (5) www.jeos.org Simple quasi-common path point diffraction interferometer with adjustable fringe contrast and carrier frequency F. Z. Bai fzbaiim@63.com College of Mechanical
More informationAnalysis of the NOT Primary Mirror Dynamics
Analysis of the NOT Primary Mirror Dynamics Graham C. Cox October 24, 2000 Introduction On the nights of 12th and 13th May 2000 observations were made using the JOSE camera system, borrowed from the ING,
More informationTurbulence-induced edge image waviness: theory and experiment
Turbulence-induced edge image waviness: theory and experiment Mikhail S. Belen kii, John M. Stewart, and Patti Gillespie A theoretical model for the edge image waviness effect is developed for the ground-to-ground
More informationScintillation by Extraterrestrial Refractors
Search for Galactic hidden gas The Optical Scintillation by Extraterrestrial Refractors A&A 412, 105-120 (2003) (astro-ph/0302460) Marc MONIEZ, IN2P3, CNRS Project Tucson 03/19/2010 OSER project: measure
More informationOptics.
Optics www.optics.rochester.edu/classes/opt100/opt100page.html Course outline Light is a Ray (Geometrical Optics) 1. Nature of light 2. Production and measurement of light 3. Geometrical optics 4. Matrix
More informationImaging with SPIRIT Exposure Guide
Imaging with SPIRIT Exposure Guide SPIRIT optical telescopes utilise extremely sensitive cameras to record the light from distant astronomical objects. Even so, exposures of several seconds up to a few
More informationROINN NA FISICE Department of Physics
ROINN NA FISICE Department of 1.1 Astrophysics Telescopes Profs Gabuzda & Callanan 1.2 Astrophysics Faraday Rotation Prof. Gabuzda 1.3 Laser Spectroscopy Cavity Enhanced Absorption Spectroscopy Prof. Ruth
More informationFinal Announcements. Lecture25 Telescopes. The Bending of Light. Parts of the Human Eye. Reading: Chapter 7. Turn in the homework#6 NOW.
Final Announcements Turn in the homework#6 NOW. Homework#5 and Quiz#6 will be returned today. Today is the last lecture. Lecture25 Telescopes Reading: Chapter 7 Final exam on Thursday Be sure to clear
More informationChapter 6 Lecture. The Cosmic Perspective Seventh Edition. Telescopes Portals of Discovery Pearson Education, Inc.
Chapter 6 Lecture The Cosmic Perspective Seventh Edition Telescopes Portals of Discovery Telescopes Portals of Discovery 6.1 Eyes and Cameras: Everyday Light Sensors Our goals for learning: How do eyes
More informationField Rotation in Altitude over Azimuth Mounts and Its Effect on CCD Imaging What is the Maximum Exposure? Bill Keicher.
Field Rotation in Altitude over Azimuth Mounts and Its Effect on CCD Imaging What is the Maximum Exposure? Bill Keicher 12 March 2005 When planning astronomical imaging sessions with a telescope equipped
More informationAstronomy 1 Introductory Astronomy Spring 2014
Astronomy 1 Introductory Astronomy Spring 2014 Lab 5: Observing the Sky pt. 2 Quick overview Meet at 8 p.m. in Science Center Room 187. We will go up to the roof from there, and make several different
More informationOptical interferometry: problems and practice
Outline Optical interferometry: problems and practice Chris Haniff Aims. What is an interferometer? Fundamental differences between optical and radio. Implementation at optical wavelengths. Conclusions.
More informationAgenda Announce: Visions of Science Visions of Science Winner
7. Telescopes: Portals of Discovery All of this has been discovered and observed these last days thanks to the telescope that I have [built], after having been enlightened by divine grace. Galileo Galilei
More informationLecture 11: Introduction to diffraction of light
Lecture 11: Introduction to diffraction of light Diffraction of waves in everyday life and applications Diffraction in everyday life Diffraction in applications Spectroscopy: physics, chemistry, medicine,
More informationLOTUCE: A new monitor for turbulence characterization inside telescope s dome
Florence, Italy. May ISBN: 978-88-98876-- DOI:.89/AOELT.5 LOTUCE: A new monitor for turbulence characterization inside telescope s dome Aziz Ziad a, Wassila Dali Ali, Julien Borgnino, Marc Sarazin, and
More informationPhotographing the Moon and the ISS. By Thierry Legault
Photographing the Moon and the ISS By Thierry Legault Photographing the whole Moon: basics Needs a DSLR at prime focus of the telescope The field of view depends on the telescope FL and the size S of the
More informationPhys102 Lecture Diffraction of Light
Phys102 Lecture 31-33 Diffraction of Light Key Points Diffraction by a Single Slit Diffraction in the Double-Slit Experiment Limits of Resolution Diffraction Grating and Spectroscopy Polarization References
More informationZernike expansions for non-kolmogorov turbulence
.. Boreman and C. ainty Vol. 13, No. 3/March 1996/J. Opt. Soc. Am. A 517 Zernike expansions for non-kolmogorov turbulence lenn. Boreman Center for Research and Education in Optics and Lasers, epartment
More informationAtmospheric Turbulence Effects Removal on Infrared Sequences Degraded by Local Isoplanatism
Atmospheric Turbulence Effects Removal on Infrared Sequences Degraded by Local Isoplanatism Magali Lemaitre 1, Olivier Laligant 1, Jacques Blanc-Talon 2, and Fabrice Mériaudeau 1 1 Le2i Laboratory, University
More informationLecture 12. AO Control Theory
Lecture 12 AO Control Theory Claire Max with many thanks to Don Gavel and Don Wiberg UC Santa Cruz February 18, 2016 Page 1 What are control systems? Control is the process of making a system variable
More informationShack-Hartmann Wavefront Measurements of Supersonic Turbulent Boundary Layers in the TGF
45th AIAA Plasmadynamics and Lasers Conference 16-0 June 014, Atlanta, GA AIAA-014-493 Shack-Hartmann Wavefront Measurements of Supersonic Turbulent Boundary Layers in the TGF Adam E. Smith 1, Stanislav
More informationAdaptive Optics for the Giant Magellan Telescope. Marcos van Dam Flat Wavefronts, Christchurch, New Zealand
Adaptive Optics for the Giant Magellan Telescope Marcos van Dam Flat Wavefronts, Christchurch, New Zealand How big is your telescope? 15-cm refractor at Townsend Observatory. Talk outline Introduction
More informationMeasurement of Atmospheric Turbulence with a Shack Hartmann Wavefront Sensor at the new MMT s Prime Focus
Measurement of Atmospheric Turbulence with a Shack Hartmann Wavefront Sensor at the new MMT s Prime Focus Patrick C. McGuire 1, Maud P. Langlois, Michael Lloyd Hart, Troy A. Rhoadarmer, J. Roger P. Angel
More informationOptical/IR Observational Astronomy Telescopes I: Telescope Basics. David Buckley, SAAO
David Buckley, SAAO 17 Feb 2010 1 Some other Telescope Parameters 1. Plate Scale This defines the scale of an image at the telescopes focal surface For a focal plane, with no distortion, this is just related
More informationThe MAORY Multi-Conjugate Adaptive Optics module Emiliano Diolaiti Istituto Nazionale di Astrofisica
The MAORY Multi-Conjugate Adaptive Optics module Emiliano Diolaiti Istituto Nazionale di Astrofisica On behalf of the MAORY module Consortium Shaping E-ELT Science and Instrumentation workshop, ESO, 25
More information1. INTRODUCTION ABSTRACT
Simulations of E-ELT telescope effects on AO system performance Miska Le Louarn* a, Pierre-Yves Madec a, Enrico Marchetti a, Henri Bonnet a, Michael Esselborn a a ESO, Karl Schwarzschild strasse 2, 85748,
More informationChapter 6 Lecture. The Cosmic Perspective. Telescopes Portals of Discovery Pearson Education, Inc.
Chapter 6 Lecture The Cosmic Perspective Telescopes Portals of Discovery 2014 Pearson Education, Inc. Telescopes Portals of Discovery CofC Observatory 6.1 Eyes and Cameras: Everyday Light Sensors Our goals
More informationOrthonormal vector polynomials in a unit circle, Part I: basis set derived from gradients of Zernike polynomials
Orthonormal vector polynomials in a unit circle, Part I: basis set derived from gradients of ernike polynomials Chunyu hao and James H. Burge College of Optical ciences, the University of Arizona 630 E.
More information대기외란보정을위한단일연속변형거울에관한연구 A Study on a Single Continuous Deformable Mirror for Correction of Atmospheric Disturbance
한국정밀공학회지제 35 권제 10 호 pp. 943-949 October 2018 / 943 J. Korean Soc. Precis. Eng., Vol. 35, No. 10, pp. 943-949 https://doi.org/10.7736/kspe.2018.35.10.943 ISSN 1225-9071 (Print) / 2287-8769 (Online) 특집
More informationMore Optical Telescopes
More Optical Telescopes There are some standard reflecting telescope designs used today All have the common feature of light entering a tube and hitting a primary mirror, from which light is reflected
More informationADVANCED CCD PHOTOMETRY AND EXOPLANET TRANSIT PHOTOMETRY. By : Kenny A. Diaz Eguigure
ADVANCED CCD PHOTOMETRY AND EXOPLANET TRANSIT PHOTOMETRY By : Kenny A. Diaz Eguigure KELT: THE KILODEGREE EXTREMELY LITTLE TELESCOPE Robotic Survey for Transiting Exoplanets KELT-North Deployed 2005 to
More informationHigh-Resolution Imagers
40 Telescopes and Imagers High-Resolution Imagers High-resolution imagers look at very small fields of view with diffraction-limited angular resolution. As the field is small, intrinsic aberrations are
More informationSOLAR ADAPTIVE OPTICS SYSTEM FOR 1-M NEW VACUUM SOLAR TELESCOPE
Florence, Italy. May 2013 ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13295 SOLAR ADAPTIVE OPTICS SYSTEM FOR 1-M NEW VACUUM SOLAR TELESCOPE Changhui Rao 1, Lei Zhu 1, Naiting Gu 1, Xuejun Rao 1, Lanqiang
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationHow to Measure and Record Light Spectrograph. The Photographic plate now obsolete Turbulence
PHYS 1411 Introduction to Astronomy Light and Telescope Chapter 6 Chapter 6 topics we have covered so far Radiation Information from Space Wave properties, light as a wave and particle, Electromagnetic
More informationImaging Geo-synchronous Satellites with the AEOS Telescope
Imaging Geo-synchronous Satellites with the AEOS Telescope Douglas A. Hope 1, Stuart M. Jefferies 1,2 and Cindy Giebink 1 1 Institute for Astronomy, University of Hawaii, Advanced Technology Research Center
More informationNB: from now on we concentrate on seeing, as scintillation for large telescopes is unimportant
b) intensity changes: scintillation!i/i on the ground is proportional to h!", i.e. # h e -h/h this function has maximum at h = H = 8.5 km! scintillation comes mostly from high layers! seeing and scintillation
More informationMonitoring Faint Space Debris with Rotating Drift-Scan CCD
Monitoring Faint Space Debris with Rotating Drift-Scan CCD Zhenghong TANG, Yindun MAO, Yan LI, Xudong ZHANG, Yong YU Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai200030,China
More informationAtmospheric Turbulence and its Influence on Adaptive Optics. Mike Campbell 23rd March 2009
Atmospheric Turbulence and its Influence on Adaptive Optics Mike Campbell 23rd March 2009 i Contents 1 Introduction 1 2 Atmospheric Turbulence 1 Seeing..................................................
More information: Imaging Systems Laboratory II. Laboratory 6: The Polarization of Light April 16 & 18, 2002
151-232: Imaging Systems Laboratory II Laboratory 6: The Polarization of Light April 16 & 18, 22 Abstract. In this lab, we will investigate linear and circular polarization of light. Linearly polarized
More informationUse of computer generated holograms for alignment of complex null correctors
Use of computer generated holograms for alignment of complex null correctors Rene Zehnder, James H. Burge and Chunyu Zhao College of Optical Sciences, the University of Arizona 1630 E. University Blvd,
More informationSpatial Light Modulator for wavefront correction 1. INTRODUCTION
Spatial Light Modulator for wavefront correction A. Vyas 1, 2, M. B. Roopashree 1, Ravinder Kumar Banyal 1, B Raghavendra Prasad 1 1 Indian Institute of Astrophysics, Bangalore-560034, India 2 Indian Institute
More informationGreen Laser propagation in a turbulent water
International Journal of ChemTech Research CODEN (USA): IJCRGG, ISSN: 0974-4290, ISSN(Online):2455-9555 Vol.10 No.1 pp 491-495, 2017 Green Laser propagation in a turbulent water Jassim Mohammed Jassim,
More informationComparison of the Performance of Modal Control Schemes for an Adaptive Optics System and Analysis of the Effect of Actuator Limitations
Comparison of the Performance of Modal Control Schemes for an Adaptive Optics System and Analysis of the Effect of Actuator Limitations Masaki Nagashima, Jae Jun Kim, Brij Agrawal Abstract In this study,
More informationAnalysis of Shane Telescope Aberration and After Collimation
UCRL-ID- 133548 Analysis of Shane Telescope Aberration and After Collimation Before Don Gavel January 26,1999 This is an informal report intended primarily for internal or limited external distribution.
More informationSimultaneous Velocity and Concentration Measurements of a Turbulent Jet Mixing Flow
Simultaneous Velocity and Concentration Measurements of a Turbulent Jet Mixing Flow HUI HU, a TETSUO SAGA, b TOSHIO KOBAYASHI, b AND NOBUYUKI TANIGUCHI b a Department of Mechanical Engineering, Michigan
More informationAstronomy 114. Lecture 26: Telescopes. Martin D. Weinberg. UMass/Astronomy Department
Astronomy 114 Lecture 26: Telescopes Martin D. Weinberg weinberg@astro.umass.edu UMass/Astronomy Department A114: Lecture 26 17 Apr 2007 Read: Ch. 6,26 Astronomy 114 1/17 Announcements Quiz #2: we re aiming
More information5. LIGHT MICROSCOPY Abbe s theory of imaging
5. LIGHT MICROSCOPY. We use Fourier optics to describe coherent image formation, imaging obtained by illuminating the specimen with spatially coherent light. We define resolution, contrast, and phase-sensitive
More informationThe interference of waves
The interference of waves In physics, interference is the addition (superposition) of two or more waves that results in a new wave pattern. The displacements of the waves add algebraically. Consider two
More informationCharacterising daytime atmospheric conditions on La Palma
Adapting to the Atmosphere Conference 214 Journal of Physics: Conference Series 9 (21) 123 doi:1.188/1742-696/9/1/123 Characterising daytime atmospheric conditions on La Palma Matthew J. Townson 1, Aglaé
More information