Optical Alignment with Computer Generated Holograms

Slides:



Advertisements
Similar presentations
TMT.OPT.PRE DRF011 Thirty Meter Telescope Secondary and Tertiary Mirror Systems International Symposium on Photoelectronic Detection and Imaging.
Advertisements

Lab 1 Paraxial Optics Lab in 106A. Look at paraxial optics rules Use a bi-convex singlet at 1:1 conjugates Do it double pass so can see image Lateral.
Nasrin Ghanbari OPTI 521. Introduction Spherical wavefront from interferometer is incident on CGH Reflected light will have an aspheric phase function.
Kawada Industries Inc. has introduced the HRP-2P for Robodex 2002
Topic 11.3 Diffraction.
Optical Testing for Next Generation Optical Telescopes; Terrestrial and Space Robert E. Parks Optical Perspectives Group, LLC Tucson, AZ September, 2002.
Tutorial: Design, Fabrication, and Testing of Aspheric Surfaces
Optical Telescope. Faint Light Astronomical objects are distant and faint. –Effectively at infinity Light collection is more important than magnification.
Announcements. Projection Today’s Readings Nalwa 2.1.
Use of a commercial laser tracker for optical alignment James H. Burge, Peng Su, Chunyu Zhao, Tom Zobrist College of Optical Sciences Steward Observatory.
Wide-field, triple spectrograph with R=5000 for a fast 22 m telescope Roger Angel, Steward Observatory 1 st draft, December 4, 2002 Summary This wide-field,
Thermally Deformable Mirrors: a new Adaptive Optics scheme for Advanced Gravitational Wave Interferometers Marie Kasprzack Laboratoire de l’Accélérateur.
High index glass spherical targets for laser interferometry Miroslav Sulc 1st PACMAN worshop 1.
Pre-alignment solutions applied to girders 1/19 Sylvain GRIFFET, 06/07/2010.
Figuring large off-axis segments to the diffraction limit Hubert Martin Steward Observatory University of Arizona.
Optical Design for an Infrared Multi-Object Spectrometer R. Winsor, J.W. MacKenty, M. Stiavelli Space Telescope Science Institute M. Greenhouse, E. Mentzell,
Advanced Optical and Mechanical Technologies in Telescopes and Instrumentation, SPIE 7018 (2008)1 Buddy Martin a, Jim Burge a,b, Brian Cuerden a, Warren.
NA62 Gigatracker Working Group Meeting 2 February 2010 Massimiliano Fiorini CERN.
The wave nature of light Interference Diffraction Polarization
SAM PDR1 SAM LGS Mechanical Design A. Montane, A. Tokovinin, H. Ochoa SAM LGS Preliminary Design Review September 2007, La Serena.
Optical Design Work for a Laser-Fiber Scanned
Effective lens aperture Deff
Magnifiers, Projectors, CamerasPaul Avery (PHY 3400)1 Magnifiers, Projectors, Cameras Applied Optics Paul Avery University of Florida
HESSI Imaging Capability Pre Environmental Review Brian R. Dennis GSFC Tuesday, February 29, 2000.
Optical Design of Giant Telescopes for Space Jim Burge, Erin Sabatke Optical Sciences Center Roger Angel, Neville Woolf Steward Observatory University.
LASER AND ADVANCES IN METROLOGY
Jim Burge, Bill Anderson, Scott Benjamin,
Understanding typical users for this instrument Graduate studentGraduate student –not an X-ray expert but wants to make a spatially resolved measurement;
1 MADRID Measurement Apparatus to Distinguish Rotational and Irrotational Displacement Rafael Ortiz Graduate student Universidad de Valladolid (Spain)
Optical surface measurements for very large flat mirrors Jim Burge, Peng Su, and Chunyu Zhao College of Optical Sciences University of Arizona Julius Yellowhair.
NORDFORSK Summer School, La Palma, June-July 2006 NOT: Telescope and Instrumentation Michal I. Andersen & Heidi Korhonen Astrophysikalisches Institut Potsdam.
1 1 st Light AO 4 LBT Pyramid WFS Adaptive Secondary MMT Unit.
Modern Optics Lab Lab 6 Part 2: Interference Experiments  Observe interference by plane-parallel plates: Measure the thickness of the plates based on.
The Hobby-Eberly Telescope Mirror Alignment Recovery System Marsha Wolf Graduate Student UT Astronomy Department.
K-D-PR Fabrication and testing of KGMT FSM prototype Oct Ho-Soon Yang, Hak-Yong Kihm, Il-Kwon Moon, Jae-Bong Song, Yun-Woo Lee Korea.
ZTF Optics Design P. Jelinsky ZTF Technical Meeting 1.
3D-Shape GmbH Mail: Albert-Rupp-Straße 2 Tel: +49 (0) 9131 / Erlangen Fax: +49 (0) 9131 /
1 MADRID Measurement Apparatus to Distinguish Rotational and Irrotational Displacement Rafael Ortiz Graduate student Universidad de Valladolid (Spain)
Zero field The 25 ‑ m f /0.7 primary mirror for the Giant Magellan Telescope (GMT) is made of seven 8.4 ‑ m segments in a close packed array. Each of the.
Fabrication and Testing of Large Flats Julius Yellowhair Peng Su, Matt Novak, and Jim Burge College of Optical Sciences University of Arizona August 28,
Absolute Calibration of Null Correctors Using Dual-Computer- Generated Holograms (CGHs) Proteep Mallik, Jim Burge, Rene Zehnder, College of Optical Sciences,
Optical Sciences Center and Steward Observatory University of Arizona
1 Design and analysis for interferometric measurements of the GMT primary mirror segments J. H. Burge a,b, L. B. Kot a, H. M. Martin a, R. Zehnder b, C.
Improved Annular-Field Three-Mirror Anastigmat? M.Lampton UCB SSL Previous AFTMAs have pri-sec separation 2.4m Can pri-sec separation be reduced? –Support.
Image at:
ZTF Optics Design ZTF Technical Meeting 1.
The 25 ‑ m f /0.7 primary mirror for the Giant Magellan Telescope (GMT) is made of seven 8.4 ‑ m segments in a close packed array. Each of the off-axis.
LITHOGRAPHY IN THE TOP-DOWN PROCESS - BASICS
College of Optical Sciences The University of Arizona Study of birefringence effect on Fizeau interferometry: analytical and simulation results Chunyu.
The High Altitude Observatory (HAO) at the National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is sponsored by.
J. H. Burgea,b, W. Davisona, H. M. Martina, C. Zhaob
Optomechanical Technologies for Astronomy, SPIE 6273 (2006)1 Manufacture of a 1.7 m prototype of the GMT primary mirror segments Buddy Martin a, Jim Burge.
다양한 창문을 통한 우주 내용 왜 다양한 창문 ? 왜 다양한 창문 ? 대기의 영향 대기의 영향 망원경의 성능 망원경의 성능 관측에서 얻는 정보 관측에서 얻는 정보 중요 망원경들 중요 망원경들 차세대 망원경들 차세대 망원경들.
Date of download: 6/3/2016 Copyright © 2016 SPIE. All rights reserved. Schematic layout of the interferometer setup. (a) T: test beam; R: reference beam;
Optical Sciences CenterThe University of Arizona ERROR ANALYSIS FOR CGH OPTICAL TESTING Yu-Chun Chang and James Burge Optical Science Center University.
ΜD Series 9 LFB --- CYCLOPS. Provides technical support for sister companies including robotic system design and fabrication, equipment maintenance Founded.
SRI 2007: CLS Optical Metrology Facility- Overview
Lab 2 Alignment.
VERTICAL SCANNING INTERFEROMETRY VSI
Design and Manufacture of a Large Aperture Wavefront Sensor (LAWS)
The GMT Project The Giant Magellan Telescope (GMT)
Lab 1 Paraxial Optics Lab in 106A.
Manuel Marchiò, Raffaele Flaminio, Shunshi Kuroki
Interference Requirements
MultiView 400™ Product Presentation Nanonics MultiView 400™
Paper Synopsis: Lens Centering using the Point Source Microscope Robert E. Parks by Wenrui Cai Opti521.
Digital Holographic Microscopy for Quantitative Visualization
Optics Alan Title, HMI-LMSAL Lead,
Announcements Midterm out today Project 1 demos.
Fig. 1 Experimental setup.
Presentation transcript:

Optical Alignment with Computer Generated Holograms James H. Burge, Rene Zehnder, Chunyu Zhao College of Optical Sciences Steward Observatory University of Arizona

Computer Generated Holograms Use diffraction to create a desired wavefront Modern fabrication provides >100 mm patterns with <0.1 µm pixels. That’s > 1012 pixels! Incredible dynamic range

Accuracy and flexibility CGHs transform wavefronts with very high accuracy Errors are typically < l/100 Any wavefront shape can be created No special solution for spheres Multiple wavefronts can be created from the same CGH The registration between the different wavefronts is also very accurate

CGH for interferometric measurement of aspheric surfaces Interferometers use light to measure to ~1 nm surface errors, for spherical or flat surfaces CGH can change spherical wavefronts to aspheric, allowing the use of interferometers for measuring aspheric surfaces Aspheric surface to be measured aspherical wavefront Spherical wavefront Interferometer CGH

Alignment of CGH Reflect wavefront back into the interferometer Use this to align the CGH to the wavefront Spherical wavefront Interferometer Reflection CGH

CGH for aligning the aspheric mirror Use numerous holograms on a single substrate to provide both wavefront and alignment information. For alignment, the CGH can project bright crosshair patterns

CGH for testing off axis parabola A single substrate provides: - reference for interferometer - null lens for aspheric surface - creates 5 reference marks, 4 around edge, 1 on optical axis

CGH alignment for testing off axis parabola

CGH alignment of a 24-in off axis parabola (600-in ROC, 60 inches off axis) Phase map l/20 rms CGH null lens incorporates alignment marks Easily align axis to 0.020” by eye

Projection of fiducial marks The positions of the crosshairs can be controlled to micron accuracy The patterns are well defined and can be found using a CCD Measured pattern at 15 meters from CGH. Central lobe is about 100 µm FWHM

Use of CGH for optical alignment Aligning the test for a 1.7-m off axis parabola 50 cm spherical mirror aligned within 7m CGH aligned within 7m 1.7m diameter OAP

Projecting alignment marks through other optics Aligning test for a 1.7-m off axis parabola Tilted spherical mirror We need to place the OAP to the right place Projecting a mark onto the OAP gives lateral position Need a second mark to get the clocking right CGH Interferometer Relay Lens Clocking mark Positioning mark

Creating desired alignment features Aligning the OAP

Use of CGHs for optical alignment Aligning the Sphere to within 7m The position of the sphere is known if 3 points on its surface are known

Use of CGHs for optical alignment Aligning the Sphere to within 7m Placing a ball concentric to zero order gives a very good reference Distance between balls can be measured with metering rods Lateral position of the ball defined by light Axial position defined by metering rod CGH Attaching the mirror to three balls defines its position The fourth ball gives redundant information

Alignment of tooling balls to light created by CGH Use tooling balls because they provide good mechanical interface Beam with ball at focus well aligned Very sensitive to lateral motion of the ball but not for axial motion Misaligned ball cases return beam to shift

Ball alignment tool 1. Align a tool to the projected beam 2. Use the tool to laterally align the ball CCD Sensitivity comes from the geometry

Direction of the reference beam Ball Alignment Tool CCD camera Ball at mirror Aperture Beam splitter Direction of the reference beam ~2 µm resolution

Use of CGHs for optical alignment Metering rods in action

Multiple patterns We use multiple patterns of the same substrate Divide the regions on the CGH. Each has a single pattern Derive a single pattern the gives simultaneous wavefronts

Single pattern, creating four 1st order references

Single CGH with multiple references Position sensing detector CGH creating multiple wavefronts

Conclusion CGHs are probably the most accurate and flexible things in optics Whatever your problem is, you can probably solve it with a CGH.