In Situ Optical Radiometry (V3.0)
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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. -
Fundametals of Rendering - Radiometry / Photometry
Fundametals of Rendering - Radiometry / Photometry “Physically Based Rendering” by Pharr & Humphreys •Chapter 5: Color and Radiometry •Chapter 6: Camera Models - we won’t cover this in class 782 Realistic Rendering • Determination of Intensity • Mechanisms – Emittance (+) – Absorption (-) – Scattering (+) (single vs. multiple) • Cameras or retinas record quantity of light 782 Pertinent Questions • Nature of light and how it is: – Measured – Characterized / recorded • (local) reflection of light • (global) spatial distribution of light 782 Electromagnetic spectrum 782 Spectral Power Distributions e.g., Fluorescent Lamps 782 Tristimulus Theory of Color Metamers: SPDs that appear the same visually Color matching functions of standard human observer International Commision on Illumination, or CIE, of 1931 “These color matching functions are the amounts of three standard monochromatic primaries needed to match the monochromatic test primary at the wavelength shown on the horizontal scale.” from Wikipedia “CIE 1931 Color Space” 782 Optics Three views •Geometrical or ray – Traditional graphics – Reflection, refraction – Optical system design •Physical or wave – Dispersion, interference – Interaction of objects of size comparable to wavelength •Quantum or photon optics – Interaction of light with atoms and molecules 782 What Is Light ? • Light - particle model (Newton) – Light travels in straight lines – Light can travel through a vacuum (waves need a medium to travel in) – Quantum amount of energy • Light – wave model (Huygens): electromagnetic radiation: sinusiodal wave formed coupled electric (E) and magnetic (H) fields 782 Nature of Light • Wave-particle duality – Light has some wave properties: frequency, phase, orientation – Light has some quantum particle properties: quantum packets (photons). • Dimensions of light – Amplitude or Intensity – Frequency – Phase – Polarization 782 Nature of Light • Coherence - Refers to frequencies of waves • Laser light waves have uniform frequency • Natural light is incoherent- waves are multiple frequencies, and random in phase. -
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 -
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 of Light Emitting Diodes Table of Contents
TECHNICAL GUIDE THE RADIOMETRY OF LIGHT EMITTING DIODES TABLE OF CONTENTS 1.0 Introduction . .1 2.0 What is an LED? . .1 2.1 Device Physics and Package Design . .1 2.2 Electrical Properties . .3 2.2.1 Operation at Constant Current . .3 2.2.2 Modulated or Multiplexed Operation . .3 2.2.3 Single-Shot Operation . .3 3.0 Optical Characteristics of LEDs . .3 3.1 Spectral Properties of Light Emitting Diodes . .3 3.2 Comparison of Photometers and Spectroradiometers . .5 3.3 Color and Dominant Wavelength . .6 3.4 Influence of Temperature on Radiation . .6 4.0 Radiometric and Photopic Measurements . .7 4.1 Luminous and Radiant Intensity . .7 4.2 CIE 127 . .9 4.3 Spatial Distribution Characteristics . .10 4.4 Luminous Flux and Radiant Flux . .11 5.0 Terminology . .12 5.1 Radiometric Quantities . .12 5.2 Photometric Quantities . .12 6.0 References . .13 1.0 INTRODUCTION Almost everyone is familiar with light-emitting diodes (LEDs) from their use as indicator lights and numeric displays on consumer electronic devices. The low output and lack of color options of LEDs limited the technology to these uses for some time. New LED materials and improved production processes have produced bright LEDs in colors throughout the visible spectrum, including white light. With efficacies greater than incandescent (and approaching that of fluorescent lamps) along with their durability, small size, and light weight, LEDs are finding their way into many new applications within the lighting community. These new applications have placed increasingly stringent demands on the optical characterization of LEDs, which serves as the fundamental baseline for product quality and product design. -
Radiometric and Photometric Measurements with TAOS Photosensors Contributed by Todd Bishop March 12, 2007 Valid
TAOS Inc. is now ams AG The technical content of this TAOS application note is still valid. Contact information: Headquarters: ams AG Tobelbaderstrasse 30 8141 Unterpremstaetten, Austria Tel: +43 (0) 3136 500 0 e-Mail: [email protected] Please visit our website at www.ams.com NUMBER 21 INTELLIGENT OPTO SENSOR DESIGNER’S NOTEBOOK Radiometric and Photometric Measurements with TAOS PhotoSensors contributed by Todd Bishop March 12, 2007 valid ABSTRACT Light Sensing applications use two measurement systems; Radiometric and Photometric. Radiometric measurements deal with light as a power level, while Photometric measurements deal with light as it is interpreted by the human eye. Both systems of measurement have units that are parallel to each other, but are useful for different applications. This paper will discuss the differencesstill and how they can be measured. AG RADIOMETRIC QUANTITIES Radiometry is the measurement of electromagnetic energy in the range of wavelengths between ~10nm and ~1mm. These regions are commonly called the ultraviolet, the visible and the infrared. Radiometry deals with light (radiant energy) in terms of optical power. Key quantities from a light detection point of view are radiant energy, radiant flux and irradiance. SI Radiometryams Units Quantity Symbol SI unit Abbr. Notes Radiant energy Q joule contentJ energy radiant energy per Radiant flux Φ watt W unit time watt per power incident on a Irradiance E square meter W·m−2 surface Energy is an SI derived unit measured in joules (J). The recommended symbol for energy is Q. Power (radiant flux) is another SI derived unit. It is the derivative of energy with respect to time, dQ/dt, and the unit is the watt (W). -
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 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. -
Simple Radiation Transfer for Spherical Stars
SIMPLE RADIATION TRANSFER FOR SPHERICAL STARS Under LTE (Local Thermodynamic Equilibrium) condition radiation has a Planck (black body) distribution. Radiation energy density is given as 8πh ν3dν U dν = , (LTE), (tr.1) r,ν c3 ehν/kT 1 − and the intensity of radiation (measured in ergs per unit area per second per unit solid angle, i.e. per steradian) is c I = B (T )= U , (LTE). (tr.2) ν ν 4π r,ν The integrals of Ur,ν and Bν (T ) over all frequencies are given as ∞ 4 Ur = Ur,ν dν = aT , (LTE), (tr.3a) Z 0 ∞ ac 4 σ 4 c 3c B (T )= Bν (T ) dν = T = T = Ur = Pr, (LTE), (tr.3b) Z 4π π 4π 4π 0 4 where Pr = aT /3 is the radiation pressure. Inside a star conditions are very close to LTE, but there must be some anisotropy of the radiation field if there is a net flow of radiation from the deep interior towards the surface. We shall consider intensity of radiation as a function of radiation frequency, position inside a star, and a direction in which the photons are moving. We shall consider a spherical star only, so the dependence on the position is just a dependence on the radius r, i.e. the distance from the center. The angular dependence is reduced to the dependence on the angle between the light ray and the outward radial direction, which we shall call the polar angle θ. The intensity becomes Iν (r, θ). The specific intensity is the fundamental quantity in classical radiative transfer. -
Optical-Depth Scaling of Light Scattering from a Dense and Cold Atomic 87Rb Gas
Old Dominion University ODU Digital Commons Physics Faculty Publications Physics 2020 Optical-Depth Scaling of Light Scattering From a Dense and Cold Atomic 87Rb Gas K. J. Kemp Old Dominion University, [email protected] S. J. Roof Old Dominion University, [email protected] M. D. Havey Old Dominion University, [email protected] I. M. Sokolov D. V. Kupriyanov See next page for additional authors Follow this and additional works at: https://digitalcommons.odu.edu/physics_fac_pubs Part of the Atomic, Molecular and Optical Physics Commons, and the Quantum Physics Commons Original Publication Citation Kemp, K. J., Roof, S. J., Havey, M. D., Sokolov, I. M., Kupriyanov, D. V., & Guerin, W. (2020). Optical-depth scaling of light scattering from a dense and cold atomic 87Rb gas. Physical Review A, 101(3), 033832. doi:10.1103/PhysRevA.101.033832 This Article is brought to you for free and open access by the Physics at ODU Digital Commons. It has been accepted for inclusion in Physics Faculty Publications by an authorized administrator of ODU Digital Commons. For more information, please contact [email protected]. Authors K. J. Kemp, S. J. Roof, M. D. Havey, I. M. Sokolov, D. V. Kupriyanov, and W. Guerin This article is available at ODU Digital Commons: https://digitalcommons.odu.edu/physics_fac_pubs/420 PHYSICAL REVIEW A 101, 033832 (2020) Optical-depth scaling of light scattering from a dense and cold atomic 87Rb gas K. J. Kemp, S. J. Roof, and M. D. Havey Department of Physics, Old Dominion University, Norfolk, Virginia 23529, USA I. M. Sokolov Department of Theoretical Physics, Peter the Great St.-Petersburg Polytechnic University, 195251 St.-Petersburg, Russia and Institute for Analytical Instrumentation, Russian Academy of Sciences, 198103 St.-Petersburg, Russia D.