Data Reduction of Hartmann Test Ou Yang, Hsien Supervisor : Shiang-yu Wang.

Slides:

Advertisements

Similar presentations

Zeros of Polynomials Lesson 4.4.

Advertisements

MYOPIA, ASTIGMATISM, HYPEROPIA… PERSONALIZED TREATMENT Bernard Mathys, MD Secretary-general of the Belgian Society of Cataract & Refractive Surgery.

Distribution and like terms A look at the algebra behind algebra tiles….

Geometrical theory of aberration for off-axis reflecting telescope and its applications Seunghyuk Chang SSG13.

RAY TRACING & WAVEFRONT ANALYSIS USING THE TRACEY SYSTEM Donald R. Sanders, M.D., Ph.D. Center For Clinical Research.

1 AN ALIGNMENT STRATEGY FOR THE ATST M2 Implementing a standalone correction strategy for ATST M2 Robert S. Upton NIO/AURA February 11,2005.

MCAO Laser Launch Telescope and Periscope Celine d’Orgeville and Jim Catone.

Optical Aberrations and Aberrometry F. Karimian, MD 2002

LIGHT AND THE RETINAL IMAGE: KEY POINTS Light travels in (more or less) straight lines: the pinhole camera’s inverted image Enlarging the pinhole leads.

Telescopes: Augmenting the Eye Text, Chapter 4 Thanks to: howstuffworks.com bbc/science.

Chapter 6 Optics and Telescopes

Mirrors Law of Reflection The angle of incidence with respect to the normal is equal to the angle of reflection.

Aperture Pupil (stop) Exit Pupil Entrance Pupil.

Chris A. Mack, Fundamental Principles of Optical Lithography, (c) Figure 3.1 Examples of typical aberrations of construction.

Geometric Optics of thick lenses and Matrix methods

3. Geometrical Optics. Geometric optics—process of light ray through lenses and mirrors to determine the location and size of the image from a given object.

Telescope Optics: A Primer for Amateur Astronomers Part 2: Optical aberrations Marc Baril West Hawaii Astronomy Club, October 13, 2009.

Small f/number, “fast” system, little depth of focus, tight tolerances on placement of components Large f/number, “slow” system, easier tolerances,

Adaptive Optics for Wavefront Correction of High Average Power Lasers Justin Mansell, Supriyo Sinha, Todd Rutherford, Eric Gustafson, Martin Fejer and.

Optical Imaging in Astronomy 1st CASSDA School for Observers Observatorio del Teide, 20 – 25 April 2015 Franz Kneer Institut für Astrophysik Göttingen.

1 Optics for Astrometry: a quick introduction William F. van Altena Yale University Basic Astrometric Methods Yale University July 18-22, 2005.

Optical Center Eugene Hecht, Optics, Addison-Wesley, Reading, MA, 1998.

Lenses Physics 202 Professor Lee Carkner Lecture 21.

Fig Spherical aberration for a lens

The SOLARC Off-axis Coronagraph Why a ground-based solar coronagraph SOLARC design and performance Future prospects J.R. Kuhn, R. Coulter, H. Lin, D. Mickey.

Page 1 Lecture 3 Part 1: Finish Geometrical Optics Part 2: Physical Optics Claire Max UC Santa Cruz January 15, 2012.

A microscope is a Complicated Lens n The microscope can be represented by a single convex lens.

OPTI 521 Presentation By Tianquan Su. Background MissionLaunch WorkFail.

Wavefront Sensing of the Human Eye

8 September Observational Astronomy TELESCOPES, Active and adaptive optics Kitchin pp

SAM PDR1 SAM LGS Mechanical Design A. Montane, A. Tokovinin, H. Ochoa SAM LGS Preliminary Design Review September 2007, La Serena.

Optics and Telescopes Lecture 11. Why do we use telescopes? Human eyes are lenses! Human eyes are lenses! Using larger lenses… Using larger lenses… 

Fundamental of Optical Engineering Lecture 3.  Aberration happens when the rays do not converge to a point where it should be. We may distinguish the.

Basic Telescope Design Refractors: Utilizes a lens (or lenses) to produce the refraction of light to focus light from an object. The main lens is called.

PACS IIDR 01/02 Mar 2001 FPFPU Alignment1 D. Kampf KAYSER-THREDE.

Austin Roorda, Ph.D. University of Houston College of Optometry

Psych 221/EE362 Applied Vision and Imaging Systems

Page 1 Adaptive Optics in the VLT and ELT era François Wildi Observatoire de Genève Credit for most slides : Claire Max (UC Santa Cruz) Optics for AO.

Optics Observations Pinholes, apertures and diffraction

Introduction to Aberrations OPTI 518 Jose Sasian

Optical Density - a property of a transparent medium that is an inverse measure of the speed of light through the medium. (how much a medium slows the.

Chapter 25 Optical Instruments 25-1 The Camera The basic parts of a camera are the light-tight box, lens, and shutter. Shutter speed refers to the speed.

Reflecting Telescopes. Mirrors A flat mirror reflects light in straight lines. A curved mirror can focus light to a point. A perfect parabolic mirror.

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.

Telescopes Key Words Optical Telescopes: make use of electromagnetic radiation in the range of visible light Refraction Telescopes: use lenses Reflecting.

A Basic Refractor Telescope The size of the telescope is the diameter of the light-collecting lens.

Sasha Bernard 5A Physics PowerPoint #2 Mr. Davis Sections of the syllabus.

Physics 203/204 4: Geometric Optics Images formed by refraction Lens Makers Equation Thin lenses Combination of thin lenses Aberration Optical Instruments.

Prof. Charles A. DiMarzio Northeastern University Fall 2003 July 2003

On the Evaluation of Optical Performace of Observing Instruments Y. Suematsu (National Astronomical Observatory of Japan) ABSTRACT: It is useful to represent.

Today Multiple Lenses The Eye Magnifiers & Microscopes

P970043/S10 Alcon LADARvision Excimer Laser System FDA Review and Questions for Ophthalmic Devices Panel August 1, 2002.

Adaptive Optics in the VLT and ELT era Optics for AO

Strehl ratio, wavefront power series expansion & Zernike polynomials expansion in small aberrated optical systems By Sheng Yuan OPTI 521 Fall 2006.

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.

Geometric Optics: Mirrors and Lenses. Mirrors with convex and concave spherical surfaces. Note that θ r = θ i for each ray.

Spherical Aberration. Rays emanating from an object point that are incident on a spherical mirror or lens at different distances from the optical axis,

Telescopes I. Refraction: Refraction is the _____________ of light as it passes through glass. II. Reflection: Reflection occurs when light _____________.

Reflective Systems Naomi Pequette

Lab 2 Alignment.

25 Optical Instruments Digital Camera with Zoom Lens.

STAT 312 Chapter 7 - Statistical Intervals Based on a Single Sample

Metamaterials for Curved Lenses Geometric optic analysis of lenses composed of continuous negative index media. UCSD.

آشنايی با اصول و پايه های يک آزمايش

Digital Holographic Microscopy for Quantitative Visualization

(Preliminary) WIYN 0.9 Meter Collimation Procedure

Photonic Band Gap Negative Index Imaging

Polynomial Functions of Higher Degree

Mirrors, Plane and Spherical Spherical Refracting Surfaces

Presentation transcript:

Data Reduction of Hartmann Test Ou Yang, Hsien Supervisor : Shiang-yu Wang

Data Reduction of Hartmann Test Introduction to Hartmann method Hartmann Pattern Data reduction Results & Discussion

Hartmann method Image quality examination method by detecting wavefront deviation w at certain points. The image aberration can be reconstruct by the data reduction.

Hartmann pattern diameter of the hole : 1cm distance between two holes : 4 cm # of holes : 140 The mask was installed in front of the secondary mirror of the TAOS#1 telescope

The Hartmann test image Inside focusOutside focusTilted image

Transverse aberrations for each of the data points on the telescope mirror

Aberration Polynomial for Primary Aberration where –A = spherical aberration coefficient –B = coma coefficient –C = astigmatism coefficient –D = defocusing coefficient –E = tile about x axis –F = tile about y axis

The coefficient of aberration polynomial CoefficientOutside focus Inside focusTilted image A3.585E E E-13 B4.844E E E-9 C-1.883E E E-7 D-7.566E E E-6 E-5.701E E E-2 F3.464E E E-4

The graph of W(x,y) [Outside focus] peak to valley error 11µm

The graph of W(x,y) [Inside focus] peak to valley error 6.8µm

The graph of W(x,y) [ Tilted image] peak to valley error 63µm

The graph of W(x,y) [spherical aberration coefficient] peak to valley error 21µm

The graph of W(x,y)[coma coefficient] peak to valley error 1.2µm

The graph of W(x,y)[astigmatism coefficient] peak to valley error 1.3µm

The graph of W(x,y) [defocusing coefficient] peak to valley error 17µm

The graph of W(x,y) [tilt about x axis] peak to valley error 5.6µm

The graph of W(x,y) [tilt about y axis] peak to valley error 3.4µm

summary The aberration of the optical system can be obtained by the hartmann test. The hartmann test can help the alignment sequence of optical systems. More detailed aberration terms can be obtained by the same procedure.