OPTI 509 Optical Design and Instrumentation II
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1 the Spectroscopic Toolbox
13 1 The Spectroscopic Toolbox 1.1 Introduction Present spectroscopic instruments use essentially bulk optics, that is, with sizes much greater than the wavelengths at which the instruments are used (0.3–2.4 μm in this book). Diffraction effects – due to the finite size of light wavelength – are then usually negligible and light propagation follows the simple precepts of geometrical optics. A special case is the disperser or interferometer that provides the spectral information: these are also large size optical devices (say 5 cm to 1 m across), but which exhibit periodic structures commensurate with the working wavelengths. The next subsection gives a short reminder of geometrical optics formulae that dictate how light beams propagate in bulk optical systems. It is followed by an introduction of a fundamental global invariant (the optical etendue) that governs the 4D geometrical extent of the light beams that any kind of optical system can accept: it is particularly useful to derive what an instrument can – and cannot – offer in terms of 3D coverage (2D of space and 1 of wavelength). 1.1.1 Geometrical Optics #101 As a short reminder of geometrical optics, that is, again the rules that apply to light propagation when all optical elements (lenses, mirrors, stops) have no fea- tures at scales comparable or smaller than light wavelength are listed: 1) Light beams propagate in straight lines in any homogeneous medium (spa- tially constant index of refraction n). 2) When a beam of light crosses from a dielectric medium of index of refraction n1 (e.g., air with n close to 1) to another dielectric of refractive index n2 (e.g., an optical glass with refractive index roughly in the 1.5–1.75 range), part of the beam is transmitted (refracted) and the remainder is reflected. -
Astronomical Instrumentation G
Astronomical Instrumentation G. H. Rieke Contents: 0. Preface 1. Introduction, radiometry, basic optics 2. The telescope 3. Detectors 4. Imagers, astrometry 5. Photometry, polarimetry 6. Spectroscopy 7. Adaptive optics, coronagraphy 8. Submillimeter and radio 9. Interferometry, aperture synthesis 10. X-ray instrumentation Introduction Preface Progress in astronomy is fueled by new technical opportunities (Harwit, 1984). For a long time, steady and overall spectacular advances were made in telescopes and, more recently, in detectors for the optical. In the last 60 years, continued progress has been fueled by opening new spectral windows: radio, X-ray, infrared, gamma ray. We haven't run out of possibilities: submillimeter, hard X-ray/gamma ray, cold IR telescopes, multi-conjugate adaptive optics, neutrinos, and gravitational waves are some of the remaining frontiers. To stay at the forefront requires that you be knowledgeable about new technical possibilities. You will also need to maintain a broad perspective, an increasingly difficult challenge with the ongoing explosion of information. Much of the future progress in astronomy will come from combining insights in different spectral regions. Astronomy has become panchromatic. This is behind much of the push for Virtual Observatories and the development of data archives of many kinds. To make optimum use of all this information requires you to understand the capabilities and limitations of a broad range of instruments so you know the strengths and limitations of the data you are working with. As Harwit (1984) shows, before ~ 1950, discoveries were driven by other factors as much as by technology, but since then technology has had a discovery shelf life of only about 5 years! Most of the physics we use is more than 50 years old, and a lot of it is more than 100 years old. -
Lecture 5. Interstellar Dust: Optical Properties
Lecture 5. Interstellar Dust: Optical Properties 1. Introduction 2. Extinction 3. Mie Scattering 4. Dust to Gas Ratio 5. Appendices References Spitzer Ch. 7, Osterbrock Ch. 7 DC Whittet, Dust in the Galactic Environment (IoP, 2002) E Krugel, Physics of Interstellar Dust (IoP, 2003) B Draine, ARAA, 41, 241, 2003 1. Introduction: Brief History of Dust Nebular gas long accepted but existence of absorbing interstellar dust controversial. Herschel (1738-1822) found few stars in some directions, later extensively demonstrated by Barnard’s photos of dark clouds. Trumpler (PASP 42 214 1930) conclusively demonstrated interstellar absorption by comparing luminosity distances & angular diameter distances for open clusters: • Angular diameter distances are systematically smaller • Discrepancy grows with distance • Distant clusters are redder • Estimated ~ 2 mag/kpc absorption • Attributed it to Rayleigh scattering by gas Some of the Evidence for Interstellar Dust Extinction (reddening of bright stars, dark clouds) Polarization of starlight Scattering (reflection nebulae) Continuum IR emission Depletion of refractory elements from the gas Dust is also observed in the winds of AGB stars, SNRs, young stellar objects (YSOs), comets, interplanetary Dust particles (IDPs), and in external galaxies. The extinction varies continuously with wavelength and requires macroscopic absorbers (or “dust” particles). Examples of the Effects of Dust Extinction B68 Scattering - Pleiades Extinction: Some Definitions Optical depth, cross section, & efficiency: ext ext ext τ λ = ∫ ndustσ λ ds = σ λ ∫ ndust 2 = πa Qext (λ) Ndust nd is the volumetric dust density The magnitude of the extinction Aλ : ext I(λ) = I0 (λ) exp[−τ λ ] Aλ =−2.5log10 []I(λ)/I0(λ) ext ext = 2.5log10(e)τ λ =1.086τ λ 2. -
Optics Microstructured Optics SMS Design Methods Plastic Optics
www.led-professional.com ISSN 1993-890X Review LpR The technology of tomorrow for general lighting applications. Sept/Oct 2008 | Issue 09 Optics Microstructured Optics SMS Design Methods Plastic Optics LED Driver Circuits Display Report Copyright © 2008 Luger Research & LED-professional. All rights reserved. There are over 20 billion light fixtures using incandescent, halogen, Design of LED or fluorescent lamps worldwide. Many of these fixtures are used for directional light applications but are based on lamps that put Optics out light in all directions. The United States Department of Energy (DOE) states that recessed downlights are the most common installed luminaire type in new residential construction. In addition, the DOE reports that downlights using non-reflector lamps are typically only 50% efficient, meaning half the light produced by the lamp is wasted inside the fixture. In contrast, lighting-class LEDs offer efficient, directional light that lasts at least 50,000 hours. Indoor luminaires designed to take advantage of all the benefits of lighting-class LEDs can exceed the efficacy of any incandescent and halogen luminaire. Furthermore, these LEDs match the performance of even the best CFL (compact fluorescent) recessed downlights, while providing a lifetime five to fifty times longer before requiring maintenance. Lastly, this class of LEDs reduces the environmental impact of light (i.e. no mercury, less power-plant pollution, and less landfill waste). Classical LED optics is composed of primary a optics for collimation and a secondary optics, which produces the required irradiance distribution. Efficient elements for primary optics are concentrators, either using total internal reflection or combined refractive/reflective versions. -
Black Body Radiation and Radiometric Parameters
Black Body Radiation and Radiometric Parameters: All materials absorb and emit radiation to some extent. A blackbody is an idealization of how materials emit and absorb radiation. It can be used as a reference for real source properties. An ideal blackbody absorbs all incident radiation and does not reflect. This is true at all wavelengths and angles of incidence. Thermodynamic principals dictates that the BB must also radiate at all ’s and angles. The basic properties of a BB can be summarized as: 1. Perfect absorber/emitter at all ’s and angles of emission/incidence. Cavity BB 2. The total radiant energy emitted is only a function of the BB temperature. 3. Emits the maximum possible radiant energy from a body at a given temperature. 4. The BB radiation field does not depend on the shape of the cavity. The radiation field must be homogeneous and isotropic. T If the radiation going from a BB of one shape to another (both at the same T) were different it would cause a cooling or heating of one or the other cavity. This would violate the 1st Law of Thermodynamics. T T A B Radiometric Parameters: 1. Solid Angle dA d r 2 where dA is the surface area of a segment of a sphere surrounding a point. r d A r is the distance from the point on the source to the sphere. The solid angle looks like a cone with a spherical cap. z r d r r sind y r sin x An element of area of a sphere 2 dA rsin d d Therefore dd sin d The full solid angle surrounding a point source is: 2 dd sind 00 2cos 0 4 Or integrating to other angles < : 21cos The unit of solid angle is steradian. -
Aerosol Optical Depth Value-Added Product
DOE/SC-ARM/TR-129 Aerosol Optical Depth Value-Added Product A Koontz C Flynn G Hodges J Michalsky J Barnard March 2013 DISCLAIMER This report was prepared as an account of work sponsored by the U.S. Government. Neither the United States nor any agency thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the U.S. Government or any agency thereof. The views and opinions of authors expressed herein do not necessarily state or reflect those of the U.S. Government or any agency thereof. DOE/SC-ARM/TR-129 Aerosol Optical Depth Value-Added Product A Koontz C Flynn G Hodges J Michalsky J Barnard March 2013 Work supported by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research A Koontz et al., March 2013, DOE/SC-ARM/TR-129 Contents 1.0 Introduction .......................................................................................................................................... 1 2.0 Description of Algorithm ...................................................................................................................... 1 2.1 Overview -
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Optics Basics 08 N [Compatibility Mode]
Basic Optical Concepts Oliver Dross, LPI Europe 1 Refraction- Snell's Law Snell’s Law: n φ φ n i i Sin ( i ) = f φ Media Boundary Sin ( f ) ni n f φ f 90 Refractive Medium 80 internal 70 external 60 50 40 30 angle of exitance 20 10 0 0 10 20 30 40 50 60 70 80 90 angle of incidence 2 Refraction and TIR Exit light ray n f φ φ f f = 90° Light ray refracted along boundary φ φ n c i i φ Totally Internally Reflected ray i Incident light rays Critical angle for total internal reflection (TIR): φ c= Arcsin(1/n) = 42° (For index of refraction ni =1.5,n= 1 (Air)) „Total internal reflection is the only 100% efficient reflection in nature” 3 Fresnel and Reflection Losses Reflection: -TIR is the most efficient reflection: n An optically smooth interface has 100% reflectivity 1 Fresnel Reflection -Metallization: Al (typical): 85%, Ag (typical): 90% n2 Refraction: -There are light losses at every optical interface -For perpendicular incidence: 1 Internal 0.9 2 Reflection − 0.8 External n1 n2 R = 0.7 Reflection + 0.6 n1 n2 0.5 0.4 Reflectivity -For n 1 =1 (air) and n 2=1.5 (glass): R=(0.5/2.5)^2=4% 0.3 -Transmission: T=1-R. 0.2 0.1 -For multiple interfaces: T tot =T 1 *T 2*T 3… -For a flat window: T=0.96^2=0.92 0 -For higher angles the reflection losses are higher 0 10 20 30 40 50 60 70 80 90 Incidence Angle [deg] 4 Black body radiation & Visible Range 3 Visible Range 6000 K 2.5 2 5500 K 1.5 5000 K 1 4500 K Radiance per wavelength [a.u.] [a.u.] wavelength wavelength per per Radiance Radiance 0.5 4000 K 3500 K 0 2800 K 300 400 500 600 700 800 900 1000 1100 1200 1300 1400 1500 1600 Wavelength [nm] • Every hot surface emits radiation • An ideal hot surface behaves like a “black body” • Filaments (incandescent) behave like this. -
Retrieval of Cloud Optical Thickness from Sky-View Camera Images Using a Deep Convolutional Neural Network Based on Three-Dimensional Radiative Transfer
remote sensing Article Retrieval of Cloud Optical Thickness from Sky-View Camera Images using a Deep Convolutional Neural Network based on Three-Dimensional Radiative Transfer Ryosuke Masuda 1, Hironobu Iwabuchi 1,* , Konrad Sebastian Schmidt 2,3 , Alessandro Damiani 4 and Rei Kudo 5 1 Graduate School of Science, Tohoku University, Sendai, Miyagi 980-8578, Japan 2 Department of Atmospheric and Oceanic Sciences, University of Colorado, Boulder, CO 80309-0311, USA 3 Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303-7814, USA 4 Center for Environmental Remote Sensing, Chiba University, Chiba 263-8522, Japan 5 Meteorological Research Institute, Japan Meteorological Agency, Tsukuba 305-0052, Japan * Correspondence: [email protected]; Tel.: +81-22-795-6742 Received: 2 July 2019; Accepted: 17 August 2019; Published: 21 August 2019 Abstract: Observation of the spatial distribution of cloud optical thickness (COT) is useful for the prediction and diagnosis of photovoltaic power generation. However, there is not a one-to-one relationship between transmitted radiance and COT (so-called COT ambiguity), and it is difficult to estimate COT because of three-dimensional (3D) radiative transfer effects. We propose a method to train a convolutional neural network (CNN) based on a 3D radiative transfer model, which enables the quick estimation of the slant-column COT (SCOT) distribution from the image of a ground-mounted radiometrically calibrated digital camera. The CNN retrieves the SCOT spatial distribution using spectral features and spatial contexts. An evaluation of the method using synthetic data shows a high accuracy with a mean absolute percentage error of 18% in the SCOT range of 1–100, greatly reducing the influence of the 3D radiative effect. -
Radiometry and Photometry
Radiometry and Photometry Wei-Chih Wang Department of Power Mechanical Engineering National TsingHua University W. Wang Materials Covered • Radiometry - Radiant Flux - Radiant Intensity - Irradiance - Radiance • Photometry - luminous Flux - luminous Intensity - Illuminance - luminance Conversion from radiometric and photometric W. Wang Radiometry Radiometry is the detection and measurement of light waves in the optical portion of the electromagnetic spectrum which is further divided into ultraviolet, visible, and infrared light. Example of a typical radiometer 3 W. Wang Photometry All light measurement is considered radiometry with photometry being a special subset of radiometry weighted for a typical human eye response. Example of a typical photometer 4 W. Wang Human Eyes Figure shows a schematic illustration of the human eye (Encyclopedia Britannica, 1994). The inside of the eyeball is clad by the retina, which is the light-sensitive part of the eye. The illustration also shows the fovea, a cone-rich central region of the retina which affords the high acuteness of central vision. Figure also shows the cell structure of the retina including the light-sensitive rod cells and cone cells. Also shown are the ganglion cells and nerve fibers that transmit the visual information to the brain. Rod cells are more abundant and more light sensitive than cone cells. Rods are 5 sensitive over the entire visible spectrum. W. Wang There are three types of cone cells, namely cone cells sensitive in the red, green, and blue spectral range. The approximate spectral sensitivity functions of the rods and three types or cones are shown in the figure above 6 W. Wang Eye sensitivity function The conversion between radiometric and photometric units is provided by the luminous efficiency function or eye sensitivity function, V(λ). -
The Determination of Cloud Optical Depth from Multiple Fields of View Pyrheliometric Measurements
The Determination of Cloud Optical Depth from Multiple Fields of View Pyrheliometric Measurements by Robert Alan Raschke and Stephen K. Cox Department of Atmospheric Science Colorado State University Fort Collins, Colorado THE DETERMINATION OF CLOUD OPTICAL DEPTH FROM HULTIPLE FIELDS OF VIEW PYRHELIOHETRIC HEASUREHENTS By Robert Alan Raschke and Stephen K. Cox Research supported by The National Science Foundation Grant No. AU1-8010691 Department of Atmospheric Science Colorado State University Fort Collins, Colorado December, 1982 Atmospheric Science Paper Number #361 ABSTRACT The feasibility of using a photodiode radiometer to infer optical depth of thin clouds from solar intensity measurements was examined. Data were collected from a photodiode radiometer which measures incident radiation at angular fields of view of 2°, 5°, 10°, 20°, and 28 ° • In combination with a pyrheliometer and pyranometer, values of normalized annular radiance and transmittance were calculated. Similar calculations were made with the results of a Honte Carlo radiative transfer model. 'ill!:! Hunte Carlo results were for cloud optical depths of 1 through 6 over a spectral bandpass of 0.3 to 2.8 ~m. Eight case studies involving various types of high, middle, and low clouds were examined. Experimental values of cloud optical depth were determined by three methods. Plots of transmittance versus field of view were compared with the model curves for the six optical depths which were run in order to obtain a value of cloud optical depth. Optical depth was then determined mathematically from a single equation which used the five field of view transmittances and as the average of the five optical depths calculated at each field of view. -
A Brief Overview of Non-Imaging Optics
2132-40 Winter College on Optics and Energy 8 - 19 February 2010 Overview of non-imaging optics V. Lakshminarayanan University of Waterloo Waterloo CANADA A Brief Overview of Non- Imaging Optics V. Lakshminarayanan University of Waterloo Waterloo, Canada What is Non-Imaging Optics? • Is the branch of optics which deals with transfer of light between a source and an object. • Techniques do not form an optimized (non-aberrated) image of source. • Optimized for radiative transfer from source to target Some examples • Optical light guides, non-imaging reflectors, nonimaging lenses, etc. • Practical examples: auto headlamps, LCD backlights, illuminated instrument panel displays, fiber optics illumination devices, projection display systems, concentration of sunlight for solar power, illumination by solar pipes, etc. Two major components of a non- imaging optics system •1. Concentration – maximize the amount of energy that “falls” on a target –ie., as in solar power •2. Illumination – control the distribution of light, i.e.,it is evenly spread of some areas and completely blocked in other areas - i.e., automobile lamps • Variables: Total radiant flux, angular distribution of optical radiation, spatial distribution of optical radiation • Collection efficiency An Optimized non-imaging optics example • THE flux at the surface of the Sun, 6.3 kW cm-2, falls off with the square of distance to a value of 137 mW cm-2 above the Earth's atmosphere, or typically 80–100 mW cm-2 at the ground. In principle, the second law of thermodynamics permits an optical device to concentrate the solar flux to obtain temperatures at the Earth's surface not exceeding the Sun's surface temperature. -
A Astronomical Terminology
A Astronomical Terminology A:1 Introduction When we discover a new type of astronomical entity on an optical image of the sky or in a radio-astronomical record, we refer to it as a new object. It need not be a star. It might be a galaxy, a planet, or perhaps a cloud of interstellar matter. The word “object” is convenient because it allows us to discuss the entity before its true character is established. Astronomy seeks to provide an accurate description of all natural objects beyond the Earth’s atmosphere. From time to time the brightness of an object may change, or its color might become altered, or else it might go through some other kind of transition. We then talk about the occurrence of an event. Astrophysics attempts to explain the sequence of events that mark the evolution of astronomical objects. A great variety of different objects populate the Universe. Three of these concern us most immediately in everyday life: the Sun that lights our atmosphere during the day and establishes the moderate temperatures needed for the existence of life, the Earth that forms our habitat, and the Moon that occasionally lights the night sky. Fainter, but far more numerous, are the stars that we can only see after the Sun has set. The objects nearest to us in space comprise the Solar System. They form a grav- itationally bound group orbiting a common center of mass. The Sun is the one star that we can study in great detail and at close range. Ultimately it may reveal pre- cisely what nuclear processes take place in its center and just how a star derives its energy.