Substrate Aberration and Correction for Meta-Lens Imaging: an Analytical Approach
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Chapter 3 (Aberrations)
Chapter 3 Aberrations 3.1 Introduction In Chap. 2 we discussed the image-forming characteristics of optical systems, but we limited our consideration to an infinitesimal thread- like region about the optical axis called the paraxial region. In this chapter we will consider, in general terms, the behavior of lenses with finite apertures and fields of view. It has been pointed out that well- corrected optical systems behave nearly according to the rules of paraxial imagery given in Chap. 2. This is another way of stating that a lens without aberrations forms an image of the size and in the loca- tion given by the equations for the paraxial or first-order region. We shall measure the aberrations by the amount by which rays miss the paraxial image point. It can be seen that aberrations may be determined by calculating the location of the paraxial image of an object point and then tracing a large number of rays (by the exact trigonometrical ray-tracing equa- tions of Chap. 10) to determine the amounts by which the rays depart from the paraxial image point. Stated this baldly, the mathematical determination of the aberrations of a lens which covered any reason- able field at a real aperture would seem a formidable task, involving an almost infinite amount of labor. However, by classifying the various types of image faults and by understanding the behavior of each type, the work of determining the aberrations of a lens system can be sim- plified greatly, since only a few rays need be traced to evaluate each aberration; thus the problem assumes more manageable proportions. -
Synopsis of Technical Report
Tzu-Yu Wu October 26, 2011 Opti 521 – Fall 2011 Introductory to opto-mechanical engineering Synopsis of Technical Report J.M. Sasian. ”Design, assembly, and testing of an objective lens for a free-space photonic switching system”, Optical Engineering 32(8), 1871-1878 (August 1993) 1. Introduction In this paper, the design, lens tolerancing, assembly and testing of a lens with a high numerical aperture over a small field of view are discussed. Although this object lens is specifically designed for a free-space photonic switching system, the concepts in aberration corrections and the approaches to reach a high NA within small field of view are applicable in many applications such as microscope objective lens, laser scan lenses. It also serves as a nice guide for a lens designer to understand the whole process of making a lens system which is not only limited to lens design but included tolerancing, lens ordering, the strategy to maintain the budget, assembly and testing details, and the approximate time required for each task. 2. Summary of the synopsis This synopsis mainly focuses on the general concepts in lens design of a fast objective lens with small field of view. It starts with a brief introduction on the lens requirement and lists the common aberration correction methods. Some explanations in aberration corrections are referenced from “Introduction to Lens Design with practical ZEMAX examples” by Joseph M Geary. Lens tolerancing, assembly and testing are included. Details in phonic switching system are neglected. Interested reader can refer the original paper for more details. 3. Lens requirement Lens requirements Focal length: 15mm Focal ratio: 1.5 Field of View: 7 degrees Wavelength: 850 nm Mapping: F-sin( ) ±1.0 Image surface: Flat Performance: Strehl휃 ratio> 0.95휇푚 over the full field Telecentricity: In the image space Lenses: Glass all spherical surfaces Page 1 of 5 4. -
United States Patent (19) 11 Patent Number: 5,838,480 Mcintyre Et Al
USOO583848OA United States Patent (19) 11 Patent Number: 5,838,480 McIntyre et al. (45) Date of Patent: Nov. 17, 1998 54) OPTICAL SCANNING SYSTEM WITH D. Stephenson, “Diffractive Optical Elements Simplify DIFFRACTIVE OPTICS Scanning Systems”, Laser Focus World, pp. 75-80, Jun. 1995. 75 Inventors: Kevin J. McIntyre, Rochester; G. Michael Morris, Fairport, both of N.Y. 73 Assignee: The University of Rochester, Primary Examiner James Phan Rochester, N.Y. Attorney, Agent, or Firm M. Lukacher; K. Lukacher 57 ABSTRACT 21 Appl. No.: 639,588 22 Filed: Apr. 29, 1996 An improved optical System having diffractive optic ele ments is provided for Scanning a beam. This optical System (51) Int. Cl. ............................................... GO2B 26/08 includes a laser Source for emitting a laser beam along a first 52 U.S. Cl. .......................... 359/205; 359/206; 359/207; path. A deflector, Such as a rotating polygonal mirror, 359/212; 359/216; 359/17 intersects the first path and translates the beam into a 58 Field of Search ..................................... 359/205-207, Scanning beam which moves along a Second path in a Scan 359/212-219, 17, 19,563, 568-570,900 plane. A lens System (F-0 lens) in the Second path has first 56) References Cited and Second elements for focusing the Scanning beam onto an image plane transverse to the Scan plane. The first and U.S. PATENT DOCUMENTS Second elements each have a cylindrical, non-toric lens. One 4,176,907 12/1979 Matsumoto et al. .................... 359/217 or both of the first and second elements also provide a 5,031,979 7/1991 Itabashi. -
Characterisation Studies on the Optics of the Prototype Fluorescence Telescope FAMOUS
Characterisation studies on the optics of the prototype fluorescence telescope FAMOUS von Hans Michael Eichler Masterarbeit in Physik vorgelegt der Fakultät für Mathematik, Informatik und Naturwissenschaften der Rheinisch-Westfälischen Technischen Hochschule Aachen im März 2014 angefertigt im III. Physikalischen Institut A bei Prof. Dr. Thomas Hebbeker Erstgutachter und Betreuer Zweitgutachter Prof. Dr. Thomas Hebbeker Prof. Dr. Christopher Wiebusch III. Physikalisches Institut A III. Physikalisches Institut B RWTH Aachen University RWTH Aachen University Abstract In this thesis, the Fresnel lens of the prototype fluorescence telescope FAMOUS, which is built at the III. Physikalisches Institut of the RWTH Aachen, is characterised. Due to the usage of silicon photomultipliers as active detector component, an adequate optical performance is required. The optical performance and transmittance of the used Fresnel lens and the qualification for the operation in the fluorescence telescope FAMOUS is examined in several series of measurements and simulations. Zusammenfassung In dieser Arbeit wird die Fresnel-Linse des Prototyp-Fluoreszenz-Teleskops FAMOUS charakterisiert, welches am III. Physikalischen Institut der RWTH Aachen gebaut wird. Durch die Verwendung von Silizium-Photomultipliern als aktive Detektorkomponente werden besondere Anforderungen an die Optik des Teleskops gestellt. In verschiedenen Messreihen und Simulationen wird untersucht, ob die Abbildungsqualität und die Transmission der verwendeten Fresnel-Linse für die Verwendung in diesem Fluoreszenz- Teleskop geeignet ist. Contents 1. Introduction 1 2. Cosmic rays 3 2.1 Energy spectrum . 4 2.2 Sources of cosmic rays . 6 2.3 Extensive air showers . 7 3. Fluorescence light detection 11 3.1 Fluorescence yield . 11 3.2 The Pierre Auger fluorescence detector . 14 3.3 FAMOUS . -
Representation of Wavefront Aberrations
Slide 1 4th Wavefront Congress - San Francisco - February 2003 Representation of Wavefront Aberrations Larry N. Thibos School of Optometry, Indiana University, Bloomington, IN 47405 [email protected] http://research.opt.indiana.edu/Library/wavefronts/index.htm The goal of this tutorial is to provide a brief introduction to how the optical imperfections of a human eye are represented by wavefront aberration maps and how these maps may be interpreted in a clinical context. Slide 2 Lecture outline • What is an aberration map? – Ray errors – Optical path length errors – Wavefront errors • How are aberration maps displayed? – Ray deviations – Optical path differences – Wavefront shape • How are aberrations classified? – Zernike expansion • How is the magnitude of an aberration specified? – Wavefront variance – Equivalent defocus – Retinal image quality • How are the derivatives of the aberration map interpreted? My lecture is organized around the following 5 questions. •First, What is an aberration map? Because the aberration map is such a fundamental description of the eye’ optical properties, I’m going to describe it from three different, but complementary, viewpoints: first as misdirected rays of light, second as unequal optical distances between object and image, and third as misshapen optical wavefronts. •Second, how are aberration maps displayed? The answer to that question depends on whether the aberrations are described in terms of rays or wavefronts. •Third, how are aberrations classified? Several methods are available for classifying aberrations. I will describe for you the most popular method, called Zernike analysis. lFourth, how is the magnitude of an aberration specified? I will describe three simple measures of the aberration map that are useful for quantifying the magnitude of optical error in a person’s eye. -
Wavefront Aberrations
11 Wavefront Aberrations Mirko Resan, Miroslav Vukosavljević and Milorad Milivojević Eye Clinic, Military Medical Academy, Belgrade, Serbia 1. Introduction The eye is an optical system having several optical elements that focus light rays representing images onto the retina. Imperfections in the components and materials in the eye may cause light rays to deviate from the desired path. These deviations, referred to as optical or wavefront aberrations, result in blurred images and decreased visual performance (1). Wavefront aberrations are optical imperfections of the eye that prevent light from focusing perfectly on the retina, resulting in defects in the visual image. There are two kinds of aberrations: 1. Lower order aberrations (0, 1st and 2nd order) 2. Higher order aberrations (3rd, 4th, … order) Lower order aberrations are another way to describe refractive errors: myopia, hyperopia and astigmatism, correctible with glasses, contact lenses or refractive surgery. Lower order aberrations is a term used in wavefront technology to describe second-order Zernike polynomials. Second-order Zernike terms represent the conventional aberrations defocus (myopia, hyperopia and astigmatism). Lower order aberrations make up about 85 per cent of all aberrations in the eye. Higher order aberrations are optical imperfections which cannot be corrected by any reliable means of present technology. All eyes have at least some degree of higher order aberrations. These aberrations are now more recognized because technology has been developed to diagnose them properly. Wavefront aberrometer is actually used to diagnose and measure higher order aberrations. Higher order aberrations is a term used to describe Zernike aberrations above second-order. Third-order Zernike terms are coma and trefoil. -
Digital Light Field Photography
DIGITAL LIGHT FIELD PHOTOGRAPHY a dissertation submitted to the department of computer science and the committee on graduate studies of stanford university in partial fulfillment of the requirements for the degree of doctor of philosophy Ren Ng July © Copyright by Ren Ng All Rights Reserved ii IcertifythatIhavereadthisdissertationandthat,inmyopinion,itisfully adequateinscopeandqualityasadissertationforthedegreeofDoctorof Philosophy. Patrick Hanrahan Principal Adviser IcertifythatIhavereadthisdissertationandthat,inmyopinion,itisfully adequateinscopeandqualityasadissertationforthedegreeofDoctorof Philosophy. Marc Levoy IcertifythatIhavereadthisdissertationandthat,inmyopinion,itisfully adequateinscopeandqualityasadissertationforthedegreeofDoctorof Philosophy. Mark Horowitz Approved for the University Committee on Graduate Studies. iii iv Acknowledgments I feel tremendously lucky to have had the opportunity to work with Pat Hanrahan, Marc Levoy and Mark Horowitz on the ideas in this dissertation, and I would like to thank them for their support. Pat instilled in me a love for simulating the flow of light, agreed to take me on as a graduate student, and encouraged me to immerse myself in something I had a passion for.Icouldnothaveaskedforafinermentor.MarcLevoyistheonewhooriginallydrewme to computer graphics, has worked side by side with me at the optical bench, and is vigorously carrying these ideas to new frontiers in light field microscopy. Mark Horowitz inspired me to assemble my camera by sharing his love for dismantling old things and building new ones. I have never met a professor more generous with his time and experience. I am grateful to Brian Wandell and Dwight Nishimura for serving on my orals commit- tee. Dwight has been an unfailing source of encouragement during my time at Stanford. I would like to acknowledge the fine work of the other individuals who have contributed to this camera research. Mathieu Brédif worked closely with me in developing the simulation system, and he implemented the original lens correction software. -
Optical Systems for Laser Scanners1 to Provide Yet Another Perspective
2 OpticalSystemsforLaserScanners Stephen F. Sagan NeoOptics Lexington, Massachusetts, USA CONTENTS 2.1 Introduction .......................................................................................................................... 70 2.2 Laser Scanner Configurations ............................................................................................71 2.2.1 Objective Scanning..................................................................................................71 2.2.2 Post-objective Scanning ..........................................................................................72 2.2.3 Pre-objective Scanning............................................................................................72 2.3 Optical Design and Optimization: Overview .................................................................72 2.4 Optical Invariants ................................................................................................................ 74 2.4.1 The Diffraction Limit .............................................................................................. 76 2.4.2 Real Gaussian Beams .............................................................................................. 76 2.4.3 Truncation Ratio ....................................................................................................... 77 2.5 Performance Issues .............................................................................................................. 79 2.5.1 Image Irradiance ......................................................................................................79 -
Ethos 13 Pkg.Pdf
WARRANTY REGISTRATION FORM We sincerely thank you for your purchase and wish you years of pleasure using it! Tele Vue Warranty Summary Eyepieces, Barlows, Powermates, & Paracorr have a “Lifetime Limited” warranty, telescopes & acces- sories are warranted for 5 years. Electronic parts are warranted for 1 year. Warranty is against defects in material or workmanship. No other warranty is expressed or implied. No returns without prior authoriza- tion. Lifetime Limited Warranty details online: http://bit.ly/TVOPTLIFE 5-Year/1-Year Warranty details online: http://bit.ly/TVOPTLIMITED Keep For Your Records Dealer: ________________________________ City/State/Country: ______________________ Date (day/month/yr): ______/______/________ 13.0 Ethos (ETH-13.0) Please fill out, cut out, and mail form below within ® 2-weeks of product purchase. Please include copy of sales receipt that has your name, the Tele Vue 32 Elkay Drive dealer name, and product name. Chester, NY 10918-3001 Cut out mailing address at left, tape to envelope, insert form & sales receipt in envelope and apply U.S.A. sufficient postage to envelope. 13.0 Ethos (ETH-13.0) How did you learn about this product? c Dealer c Friend c Tele Vue Blog c CloudyNights.com c TeleVue.com ______________________________________ c Social Media/Magazine/Other(s): Name Last First ______________________________________ Street Address What made you decide to buy this and your com- ments after using the product? ______________________________________ City State/Province ______________________________________ Postal Country Code Email*: _________________________________ Purchase Information Phone: _________________________________ Dealer: ________________________________ Astro Club: ____________________________ City/State/Country: ______________________ *c Check to receive email blog / newsletter Date (day/month/yr): ______/______/________ Ethos 6, 8, 10, & 13mm 100° Eyepieces Thank you for purchasing this Ethos eyepiece. -
Utilization of a Curved Focal Surface Array in a 3.5M Wide Field of View Telescope
Utilization of a curved focal surface array in a 3.5m wide field of view telescope Lt. Col. Travis Blake Defense Advanced Research Projects Agency, Tactical Technology Office E. Pearce, J. A. Gregory, A. Smith, R. Lambour, R. Shah, D. Woods, W. Faccenda Massachusetts Institute of Technology, Lincoln Laboratory S. Sundbeck Schafer Corporation TMD M. Bolden CENTRA Technology, Inc. ABSTRACT Wide field of view optical telescopes have a range of uses for both astronomical and space-surveillance purposes. In designing these systems, a number of factors must be taken into account and design trades accomplished to best balance the performance and cost constraints of the system. One design trade that has been discussed over the past decade is the curving of the digital focal surface array to meet the field curvature versus using optical elements to flatten the field curvature for a more traditional focal plane array. For the Defense Advanced Research Projects Agency (DARPA) 3.5-m Space Surveillance Telescope (SST)), the choice was made to curve the array to best satisfy the stressing telescope performance parameters, along with programmatic challenges. The results of this design choice led to a system that meets all of the initial program goals and dramatically improves the nation’s space surveillance capabilities. This paper will discuss the implementation of the curved focal-surface array, the performance achieved by the array, and the cost level-of-effort difference between the curved array versus a typical flat one. 1. INTRODUCTION Curved-detector technology for applications in astronomy, remote sensing, and, more recently, medical imaging has been a component in the decision-making process for fielded systems and products in these and other various disciplines for many decades. -
(S15) Joseph A
Optical Design (S15) Joseph A. Shaw – Montana State University The Wave-Front Aberration Polynomial Ideal imaging systems perform point-to-point imaging. This requires that a spherical wave front expanding from each object point (o) is converted to a spherical wave front converging to a corresponding image point (o’). However, real optical systems produce an imperfect “aberrated” image. The aberrated wave front indicated by the solid red line below corresponds to rays near the axis focusing near point a and rays near the margin of the pupil focusing near point b. optical system o b a o’ W(x,y) = awf –rs entrance pupil exit pupil The “wave front aberration function” describes the optical path difference between the aberrated wave front and a spherical reference wave (typically measured in m or “waves”). W(x,y) = aberrated wave front – spherical reference wave front 1 Optical Design (S15) Joseph A. Shaw – Montana State University Coordinate System The unique rotationally invariant combinations of the exit-pupil and image-plane coordinates shown below are x2 + y2, x + yand All others are combinations of these. y x exit pupil image plane For rotationally symmetric optical systems, we can choose the “meridional” plane as our plane of symmetry so that we only need to consider rays that pass through the pupil in the plane. Then = 0 and our variables become the following … = 0 → x2 + y2, y We now convert to circular coordinates in the pupil plane and replace with to match Geary. y x2 + y2 → 2 = normalized exit-pupil radius y → cos = exit-pupil angle from meridional plane → = normalized height of ray intersection in image plane exit pupil image plane 2 Optical Design (S15) Joseph A. -
Lens Design OPTI 517 Seidel Aberration Coefficients
Lens Design OPTI 517 Seidel aberration coefficients Prof. Jose Sasian OPTI 517 Fourth-order terms 2 2 W H, W040 W131H W222 H 2 W220 H H W311H H H W400 H H Spherical aberration Coma Astigmatism (cylindrical aberration!) Field curvature Distortion Piston Prof. Jose Sasian OPTI 517 Coordinate system Prof. Jose Sasian OPTI 517 Spherical aberration h 2 h 4 Z 2r 8r 3 u h y1 y 2r W n'[PB'] n'[PA' ] n'[PB'] n[PB] We have a spherical surface of radius of curvature r, a ray intersecting the surface at point P, intersecting the reference sphere at B’, intersecting the wavefront in object space at B and in image space at A’, and passing in image space by the point Q’’ in the optical axis. The reference sphere in object space is centered at Q and in image space is centered at Q’ Question: how do we draw the first order Prof. Jose Sasian OPTI 517 marginal ray in image space? [PQ]2 s Z 2 h 2 s 2 2sZ Z 2 h 2 2 4 4 2 h h h h 2s 3 2 2r 8r 4r [PB] [OQ] [PQ] s 2 1 2 2 s h 2 1 1 h 4 1 1 h 4 1 1 2 2 s r 8r s r 8s s r 2 4 2 h s h s s 1 1 1 u s 2 r 4r 2 s 2 r h y1 y 2r Prof. Jose Sasian OPTI 517 Spherical aberration ' ' [PB] [OQ] [PQ] [PB'] [OQ ] [PQ ] 2 2 2 4 y 2 u 1 1 y 4 1 1 y u 1 1 y 1 1 1 y 1 y ' 2 ' 2 2 2r s r 8r s r 2 2r s r 8r s r 4 2 4 2 y 1 1 y 1 1 8s ' s ' r 8s s r W n '[PB'] n[PB] y 2 u 1 1 1 1 1 y n ' n ' 2 r s r s r y 4 1 1 1 1 n ' n 2 ' 8r s r s r 2 2 y 4 n ' 1 1 n 1 1 ' ' 8 s s r s s r Prof.