Simple and Robust Method for Determination of Laser Fluence
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Diffraction Interference Induced Superfocusing in Nonlinear Talbot Effect24,25, to Achieve Subdiffraction by Exploiting the Phases of The
OPEN Diffraction Interference Induced SUBJECT AREAS: Superfocusing in Nonlinear Talbot Effect NONLINEAR OPTICS Dongmei Liu1, Yong Zhang1, Jianming Wen2, Zhenhua Chen1, Dunzhao Wei1, Xiaopeng Hu1, Gang Zhao1, SUB-WAVELENGTH OPTICS S. N. Zhu1 & Min Xiao1,3 Received 1National Laboratory of Solid State Microstructures, College of Engineering and Applied Sciences, School of Physics, Nanjing 12 May 2014 University, Nanjing 210093, China, 2Department of Applied Physics, Yale University, New Haven, Connecticut 06511, USA, 3Department of Physics, University of Arkansas, Fayetteville, Arkansas 72701, USA. Accepted 24 July 2014 We report a simple, novel subdiffraction method, i.e. diffraction interference induced superfocusing in Published second-harmonic (SH) Talbot effect, to achieve focusing size of less than lSH/4 (or lpump/8) without 20 August 2014 involving evanescent waves or subwavelength apertures. By tailoring point spread functions with Fresnel diffraction interference, we observe periodic SH subdiffracted spots over a hundred of micrometers away from the sample. Our demonstration is the first experimental realization of the Toraldo di Francia’s proposal pioneered 62 years ago for superresolution imaging. Correspondence and requests for materials should be addressed to ocusing of a light beam into an extremely small spot with a high energy density plays an important role in key technologies for miniaturized structures, such as lithography, optical data storage, laser material nanopro- Y.Z. (zhangyong@nju. cessing and nanophotonics in confocal microscopy and superresolution imaging. Because of the wave edu.cn); J.W. F 1 nature of light, however, Abbe discovered at the end of 19th century that diffraction prohibits the visualization (jianming.wen@yale. of features smaller than half of the wavelength of light (also known as the Rayleigh diffraction limit) with optical edu) or M.X. -
The Gauss-Airy Functions and Their Properties
Annals of the University of Craiova, Mathematics and Computer Science Series Volume 43(2), 2016, Pages 119{127 ISSN: 1223-6934 The Gauss-Airy functions and their properties Alireza Ansari Abstract. In this paper, in connection with the generating function of three-variable Hermite polynomials, we introduce the Gauss-Airy function Z 1 3 1 −yt2 zt GAi(x; y; z) = e cos(xt + )dt; y ≥ 0; x; z 2 R: π 0 3 Some properties of this function such as behaviors of zeros, orthogonal relations, corresponding inequalities and their integral transforms are investigated. Key words and phrases. Gauss-Airy function, Airy function, Inequality, Orthogonality, Integral transforms. 1. Introduction We consider the three-variable Hermite polynomials [ n ] [ n−3j ] X3 X2 zj yk H (x; y; z) = n! xn−3j−2k; (1) 3 n j! k!(n − 2k)! j=0 k=0 2 3 as the coefficient set of the generating function ext+yt +zt 1 n 2 3 X t ext+yt +zt = H (x; y; z) : (2) 3 n n! n=0 For the first time, these polynomials [8] and their generalization [9] was introduced by Dattoli et al. and later Torre [10] used them to describe the behaviors of the Hermite- Gaussian wavefunctions in optics. These are wavefunctions appeared as Gaussian apodized Airy polynomials [3,7] in elegant and standard forms. Also, similar families to the generating function (2) have been stated in literature, see [11, 12]. Now in this paper, it is our motivation to introduce the Gauss-Airy function derived from operational relation 2 3 y d +z d n 3Hn(x; y; z) = e dx2 dx3 x : (3) For this purpose, in view of the operational calculus of the Mellin transform [4{6], we apply the following integral representation 1 2 3 Z eys +zs = esξGAi(ξ; y; z) dξ; (4) −∞ Received February 28, 2015. -
Introduction to Optics Part I
Introduction to Optics part I Overview Lecture Space Systems Engineering presented by: Prof. David Miller prepared by: Olivier de Weck Revised and augmented by: Soon-Jo Chung Chart: 1 16.684 Space Systems Product Development MIT Space Systems Laboratory February 13, 2001 Outline Goal: Give necessary optics background to tackle a space mission, which includes an optical payload •Light •Interaction of Light w/ environment •Optical design fundamentals •Optical performance considerations •Telescope types and CCD design •Interferometer types •Sparse aperture array •Beam combining and Control Chart: 2 16.684 Space Systems Product Development MIT Space Systems Laboratory February 13, 2001 Examples - Motivation Spaceborne Astronomy Planetary nebulae NGC 6543 September 18, 1994 Hubble Space Telescope Chart: 3 16.684 Space Systems Product Development MIT Space Systems Laboratory February 13, 2001 Properties of Light Wave Nature Duality Particle Nature HP w2 E 2 E 0 Energy of Detector c2 wt 2 a photon Q=hQ Solution: Photons are EAeikr( ZtI ) “packets of energy” E: Electric field vector c H: Magnetic field vector Poynting Vector: S E u H 4S 2S Spectral Bands (wavelength O): Wavelength: O Q QT Ultraviolet (UV) 300 Å -300 nm Z Visible Light 400 nm - 700 nm 2S Near IR (NIR) 700 nm - 2.5 Pm Wave Number: k O Chart: 4 16.684 Space Systems Product Development MIT Space Systems Laboratory February 13, 2001 Reflection-Mirrors Mirrors (Reflective Devices) and Lenses (Refractive Devices) are both “Apertures” and are similar to each other. Law of reflection: Mirror Geometry given as Ti Ti=To a conic section rot surface: T 1 2 2 o z()U r r k 1 U Reflected wave is also k 1 in the plane of incidence Specular Circle: k=0 Ellipse -1<k<0 Reflection Parabola: k=-1 Hyperbola: k<-1 sun mirror Detectors resolve Images produced by (solar) energy reflected from detector a target scene* in Visual and NIR. -
Implementation of Airy Function Using Graphics Processing Unit (GPU)
ITM Web of Conferences 32, 03052 (2020) https://doi.org/10.1051/itmconf/20203203052 ICACC-2020 Implementation of Airy function using Graphics Processing Unit (GPU) Yugesh C. Keluskar1, Megha M. Navada2, Chaitanya S. Jage3 and Navin G. Singhaniya4 Department of Electronics Engineering, Ramrao Adik Institute of Technology, Nerul, Navi Mumbai. Email : [email protected], [email protected], [email protected], [email protected] Abstract—Special mathematical functions are an integral part Airy function is the solution to Airy differential equa- of Fractional Calculus, one of them is the Airy function. But tion,which has the following form [22]: it’s a gruelling task for the processor as well as system that is constructed around the function when it comes to evaluating the d2y special mathematical functions on an ordinary Central Processing = xy (1) Unit (CPU). The Parallel processing capabilities of a Graphics dx2 processing Unit (GPU) hence is used. In this paper GPU is used to get a speedup in time required, with respect to CPU time for It has its applications in classical physics and mainly evaluating the Airy function on its real domain. The objective quantum physics. The Airy function also appears as the so- of this paper is to provide a platform for computing the special lution to many other differential equations related to elasticity, functions which will accelerate the time required for obtaining the heat equation, the Orr-Sommerfield equation, etc in case of result and thus comparing the performance of numerical solution classical physics. While in the case of Quantum physics,the of Airy function using CPU and GPU. -
Sub-Airy Disk Angular Resolution with High Dynamic Range in the Near-Infrared A
EPJ Web of Conferences 16, 03002 (2011) DOI: 10.1051/epjconf/20111603002 C Owned by the authors, published by EDP Sciences, 2011 Sub-Airy disk angular resolution with high dynamic range in the near-infrared A. Richichi European Southern Observatory,Karl-Schwarzschildstr. 2, 85748 Garching, Germany Abstract. Lunar occultations (LO) are a simple and effective high angular resolution method, with minimum requirements in instrumentation and telescope time. They rely on the analysis of the diffraction fringes created by the lunar limb. The diffraction phenomen occurs in space, and as a result LO are highly insensitive to most of the degrading effects that limit the performance of traditional single telescope and long-baseline interferometric techniques used for direct detection of faint, close companions to bright stars. We present very recent results obtained with the technique of lunar occultations in the near-IR, showing the detection of companions with very high dynamic range as close as few milliarcseconds to the primary star. We discuss the potential improvements that could be made, to increase further the current performance. Of course, LO are fixed-time events applicable only to sources which happen to lie on the Moon’s apparent orbit. However, with the continuously increasing numbers of potential exoplanets and brown dwarfs beign discovered, the frequency of such events is not negligible. I will list some of the most favorable potential LO in the near future, to be observed from major observatories. 1. THE METHOD The geometry of a lunar occultation (LO) event is sketched in Figure 1. The lunar limb acts as a straight diffracting edge, moving across the source with an angular speed that is the product of the lunar motion vector VM and the cosine of the contact angle CA. -
The Most Important Equation in Astronomy! 50
The Most Important Equation in Astronomy! 50 There are many equations that astronomers use L to describe the physical world, but none is more R 1.22 important and fundamental to the research that we = conduct than the one to the left! You cannot design a D telescope, or a satellite sensor, without paying attention to the relationship that it describes. In optics, the best focused spot of light that a perfect lens with a circular aperture can make, limited by the diffraction of light. The diffraction pattern has a bright region in the center called the Airy Disk. The diameter of the Airy Disk is related to the wavelength of the illuminating light, L, and the size of the circular aperture (mirror, lens), given by D. When L and D are expressed in the same units (e.g. centimeters, meters), R will be in units of angular measure called radians ( 1 radian = 57.3 degrees). You cannot see details with your eye, with a camera, or with a telescope, that are smaller than the Airy Disk size for your particular optical system. The formula also says that larger telescopes (making D bigger) allow you to see much finer details. For example, compare the top image of the Apollo-15 landing area taken by the Japanese Kaguya Satellite (10 meters/pixel at 100 km orbit elevation: aperture = about 15cm ) with the lower image taken by the LRO satellite (0.5 meters/pixel at a 50km orbit elevation: aperture = ). The Apollo-15 Lunar Module (LM) can be seen by its 'horizontal shadow' near the center of the image. -
Telescope Optics Discussion
DFM Engineering, Inc. 1035 Delaware Avenue, Unit D Longmont, Colorado 80501 Phone: 303-678-8143 Fax: 303-772-9411 Web: www.dfmengineering.com TELESCOPE OPTICS DISCUSSION: We recently responded to a Request For Proposal (RFP) for a 24-inch (610-mm) aperture telescope. The optical specifications specified an optical quality encircled energy (EE80) value of 80% within 0.6 to 0.8 arc seconds over the entire Field Of View (FOV) of 90-mm (1.2- degrees). From the excellent book, "Astronomical Optics" page 185 by Daniel J. Schroeder, we find the definition of "Encircled Energy" as "The fraction of the total energy E enclosed within a circle of radius r centered on the Point Spread Function peak". I want to emphasize the "radius r" as we will see this come up again later in another expression. The first problem with this specification is no wavelength has been specified. Perfect optics will produce an Airy disk whose "radius r" is a function of the wavelength and the aperture of the optic. The aperture in this case is 24-inches (610-mm). A typical Airy disk is shown below. This Airy disk was obtained in the DFM Engineering optical shop. Actual Airy disk of an unobstructed aperture with an intensity scan through the center in blue. Perfect optics produce an Airy disk composed of a central spot with alternating dark and bright rings due to diffraction. The Airy disk above only shows the central spot and the first bright ring, the next ring is too faint to be recorded. The first bright ring (seen above) is 63 times fainter than the peak intensity. -
On Airy Solutions of the Second Painlevé Equation
On Airy Solutions of the Second Painleve´ Equation Peter A. Clarkson School of Mathematics, Statistics and Actuarial Science, University of Kent, Canterbury, CT2 7NF, UK [email protected] October 18, 2018 Abstract In this paper we discuss Airy solutions of the second Painleve´ equation (PII) and two related equations, the Painleve´ XXXIV equation (P34) and the Jimbo-Miwa-Okamoto σ form of PII (SII), are discussed. It is shown that solutions which depend only on the Airy function Ai(z) have a completely difference structure to those which involve a linear combination of the Airy functions Ai(z) and Bi(z). For all three equations, the special solutions which depend only on Ai(t) are tronquee´ solutions, i.e. they have no poles in a sector of the complex plane. Further for both P34 and SII, it is shown that amongst these tronquee´ solutions there is a family of solutions which have no poles on the real axis. Dedicated to Mark Ablowitz on his 70th birthday 1 Introduction The six Painleve´ equations (PI–PVI) were first discovered by Painleve,´ Gambier and their colleagues in an investigation of which second order ordinary differential equations of the form d2q dq = F ; q; z ; (1.1) dz2 dz where F is rational in dq=dz and q and analytic in z, have the property that their solutions have no movable branch points. They showed that there were fifty canonical equations of the form (1.1) with this property, now known as the Painleve´ property. Further Painleve,´ Gambier and their colleagues showed that of these fifty equations, forty-four can be reduced to linear equations, solved in terms of elliptic functions, or are reducible to one of six new nonlinear ordinary differential equations that define new transcendental functions, see Ince [1]. -
Part III - Microscopy
Part III - Microscopy Chapter 6: Fundamentals Resolution Limits, Modulation Transfer Function, Lens Aberrations, Comparison Optical and Electron Microscopy, 3D Imaging Chapter 7: X-Ray and Electron Microscopy Chapter 8: Contrast and Modulation Transfer Function Chapter 9: Advanced Techniques Confocal Scanning Microscopy, 3D Optical Imaging, Super-resolution using PALM, STORM, STED, NSOM Chapter VI: Fundamentals of Optical Microscopy G. Springholz - Nanocharacterization I VI / 1 Chapter VI: Fundamentals of Optical Microscopy G. Springholz - Nanocharacterization I VI / 2 Chapter 6 Fundamentals of Optical Microscopy Instrumentation, Resolution Limits, Aberrations, Practical Resolution: Optical Microscopy versus TEM Chapter VI: Fundamentals of Optical Microscopy G. Springholz - Nanocharacterization I VI / 3 Contents - Chapter 6: Fundamentals of Optical Microscopy 6.1 Introduction ......................................................................................................................... 1 6.2 How to Perform Spatial Imaging with High Resolution ? ................................................. 3 6.3 Scanning Microscopy ......................................................................................................... 5 6.4 Imaging Microscopy ............................................................................................................ 7 6.5 Resolution Limits of Imaging Microscopy ....................................................................... 11 6.6 Resolution Limit due to Diffraction (see, e.g., -
Part I Geometrical Optics Part II Diffraction Optics Aperture and Field Stops
Astronomische Waarneemtechnieken (Astronomical Observing Techniques) 6th Lecture: 8 October 2012 1. Geometrical Optics Definitions Aberrations 2. Diffraction Optics Fraunhofer Diff. PSF, MTF SR & EE high contrast im. Based on “Astronomical Optics” by Daniel J. Schroeder, “Principles of 2SWLFVµE\0D[%RUQ (PLO:ROIWKH´2SWLFDO(QJLQHHU·V'HVN Reference” by William L. Wolfe, Lena book, and Wikipedia Part I Geometrical Optics Part II Diffraction Optics Aperture and Field Stops telescope camera Aperture stop: determines the diameter of the light cone from an axial point on the object. Field stop: determines the field of view of the system. Entrance pupil: image of the aperture stop in the object space Exit pupil: image of the aperture stop in the image space Marginal ray: ray from an object point on the optical axis that passes at the edge of the entrance pupil Chief ray: ray from an object point at the edge of the field, passing through the center of the aperture stop. The Speed of the System f IJ D The speed of an optical system is described by the numerical aperture NA and the F number, where: f 1 NA nsinT and F { D 2(NA) Generally, fast optics (large NA) has a high light power, is compact, but has tight tolerances and is difficult to manufacture. Slow optics (small NA) is just the opposite. Étendue and Ax The geometrical étendue (frz. `extent· is the product of area A of the source times the solid angle (of the system's entrance pupil as seen from the source). The étendue is the maximum beam size the instrument can accept. -
Advanced Microscopy Lecture 3 Physical Optics Of
Microscopy Lecture 3: Physical optics of widefield microscopes 2012-10-29 Herbert Gross Winter term 2012 www.iap.uni-jena.de 3 Physical optics of widefield microscopes 2 Preliminary time schedule No Date Main subject Detailed topics Lecturer overview, general setup, binoculars, objective lenses, performance and types of lenses, 1 15.10. Optical system of a microscope I tube optics Gross Etendue, pupil, telecentricity, confocal systems, illumination setups, Köhler principle, 2 22.10. Optical system of a microscope II fluorescence systems and TIRF, adjustment of objective lenses Gross Physical optics of widefield Point spread function, high-NA-effects, apodization, defocussing, index mismatch, 3 29.10. Gross microscopes coherence, partial coherent imaging Wave aberrations and Zernikes, Strehl ratio, point resolution, sine condition, optical 4 05.11. Performance assessment transfer function, conoscopic observation, isoplantism, straylight and ghost images, Gross thermal degradation, measuring of system quality basic concepts, 2-point-resolution (Rayleigh, Sparrow), Frequency-based resolution (Abbe), 5 12.11. Fourier optical description CTF and Born Approximation Heintzmann 6 19.11. Methods, DIC Rytov approximation, a comment on holography, Ptychography, DIC Heintzmann Multibeam illumination, Cofocal coherent, Incoherent processes (Fluorescence, Raman), 7 26.11. Imaging of scatter OTF for incoherent light, Missing cone problem, imaging of a fluorescent plane, incoherent Heintzmann confocal OTF/PSF Fluorescence, Structured illumination, Image based identification of experimental 8 03.12. Incoherent emission to improve resolution parameters, image reconstruction Heintzmann 9 10.12. The quantum world in microscopy Photons, Poisson distribution, squeezed light, antibunching, Ghost imaging Wicker 10 17.12. Deconvolution Building a forward model and inverting it based on statistics Wicker 11 07.01. -
Chapter on Diffraction
Chapter 3 Diffraction While the particle description of Chapter 1 works amazingly well to understand how ra- diation is generated and transported in (and out of) astrophysical objects, it falls short when we investigate how we detect this radiation with our telescopes. In particular the diffraction limit of a telescope is the limit in spatial resolution a telescope of a given size can achieve because of the wave nature of light. Diffraction gives rise to a “Point Spread Function”, meaning that a point source on the sky will appear as a blob of a certain size on your image plane. The size of this blob limits your spatial resolution. The only way to improve this is to go to a larger telescope. Since the theory of diffraction is such a fundamental part of the theory of telescopes, and since it gives a good demonstration of the wave-like nature of light, this chapter is devoted to a relatively detailed ab-initio study of diffraction and the derivation of the point spread function. Literature: Born & Wolf, “Principles of Optics”, 1959, 2002, Press Syndicate of the Univeristy of Cambridge, ISBN 0521642221. A classic. Steward, “Fourier Optics: An Introduction”, 2nd Edition, 2004, Dover Publications, ISBN 0486435040 Goodman, “Introduction to Fourier Optics”, 3rd Edition, 2005, Roberts & Company Publishers, ISBN 0974707724 3.1 Fresnel diffraction Let us construct a simple “Camera Obscura” type of telescope, as shown in Fig. 3.1. We have a point-source at location “a”, and we point our telescope exactly at that source. Our telescope consists simply of a screen with a circular hole called the aperture or alternatively the pupil.