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CIE Technical Note 004:2016
TECHNICAL NOTE The Use of Terms and Units in Photometry – Implementation of the CIE System for Mesopic Photometry CIE TN 004:2016 CIE TN 004:2016 CIE Technical Notes (TN) are short technical papers summarizing information of fundamental importance to CIE Members and other stakeholders, which either have been prepared by a TC, in which case they will usually form only a part of the outputs from that TC, or through the auspices of a Reportership established for the purpose in response to a need identified by a Division or Divisions. This Technical Note has been prepared by CIE Technical Committee 2-65 of Division 2 “Physical Measurement of Light and Radiation" and has been approved by the Board of Administration as well as by Division 2 of the Commission Internationale de l'Eclairage. The document reports on current knowledge and experience within the specific field of light and lighting described, and is intended to be used by the CIE membership and other interested parties. It should be noted, however, that the status of this document is advisory and not mandatory. Any mention of organizations or products does not imply endorsement by the CIE. Whilst every care has been taken in the compilation of any lists, up to the time of going to press, these may not be comprehensive. CIE 2016 - All rights reserved II CIE, All rights reserved CIE TN 004:2016 The following members of TC 2-65 “Photometric measurements in the mesopic range“ took part in the preparation of this Technical Note. The committee comes under Division 2 “Physical measurement of light and radiation”. -
Foot-Candles: Photometric Units
UPDATED EXTRACT FROM CREG JOURNAL. FILE: FOOT3-UP.DOC REV. 8. LAST SAVED: 01/02/01 15:14 PHOTOMETRICS Foot-Candles: Photometric Units More footnotes on optical topics. David Gibson describes the confusing range of photometric units. A discussion of photometric units may the ratio of luminous efficiency to luminous The non-SI unit mean spherical candle- seem out of place in an electronic journal but efficiency at the wavelength where the eye is power is the intensity of a source if its light engineers frequently have to use light sources most sensitive. Unfortunately, however, this output were spread evenly in all directions. It and detectors. The units of photometry are term can be confused with the term efficacy, is therefore equivalent to the flux [lm] ¸ 4p. some of the most confusing and least which is used to describe the efficiency at standardised of units. converting electrical to luminous power. Luminance Photometric units are not difficult to The candela measures the intensity of a understand, but can be a minefield to the Illumination, Luminous Emittance. point source. We also need to define the uninitiated since many non-SI units are still The illumination of a surface is the properties of an extended source. Each small in use, and there are subtle differences incident power flux density measured in element DS of a diffuse reflective surface will between quantities with similar names, such lumens per square metre. A formal definition scatter the incident flux DF and behave as if as illumination and luminance. would be along the lines of: if a flux DF is it were an infinitesimal point source. -
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. -
Guide for the Use of the International System of Units (SI)
Guide for the Use of the International System of Units (SI) m kg s cd SI mol K A NIST Special Publication 811 2008 Edition Ambler Thompson and Barry N. Taylor NIST Special Publication 811 2008 Edition Guide for the Use of the International System of Units (SI) Ambler Thompson Technology Services and Barry N. Taylor Physics Laboratory National Institute of Standards and Technology Gaithersburg, MD 20899 (Supersedes NIST Special Publication 811, 1995 Edition, April 1995) March 2008 U.S. Department of Commerce Carlos M. Gutierrez, Secretary National Institute of Standards and Technology James M. Turner, Acting Director National Institute of Standards and Technology Special Publication 811, 2008 Edition (Supersedes NIST Special Publication 811, April 1995 Edition) Natl. Inst. Stand. Technol. Spec. Publ. 811, 2008 Ed., 85 pages (March 2008; 2nd printing November 2008) CODEN: NSPUE3 Note on 2nd printing: This 2nd printing dated November 2008 of NIST SP811 corrects a number of minor typographical errors present in the 1st printing dated March 2008. Guide for the Use of the International System of Units (SI) Preface The International System of Units, universally abbreviated SI (from the French Le Système International d’Unités), is the modern metric system of measurement. Long the dominant measurement system used in science, the SI is becoming the dominant measurement system used in international commerce. The Omnibus Trade and Competitiveness Act of August 1988 [Public Law (PL) 100-418] changed the name of the National Bureau of Standards (NBS) to the National Institute of Standards and Technology (NIST) and gave to NIST the added task of helping U.S. -
Variable Star Photometry with a DSLR Camera
Variable star photometry with a DSLR camera Des Loughney Introduction now be studied. I have used the method to create lightcurves of stars with an amplitude of under 0.2 magnitudes. In recent years it has been found that a digital single lens reflex (DSLR) camera is capable of accurate unfiltered pho- tometry as well as V-filter photometry.1 Undriven cameras, Equipment with appropriate quality lenses, can do photometry down to magnitude 10. Driven cameras, using exposures of up to 30 seconds, can allow photometry to mag 12. Canon 350D/450D DSLR cameras are suitable for photome- The cameras are not as sensitive or as accurate as CCD try. My experiments suggest that the cameras should be cameras primarily because they are not cooled. They do, used with quality lenses of at least 50mm aperture. This however, share some of the advantages of a CCD as they allows sufficient light to be gathered over the range of have a linear response over a large portion of their range1 exposures that are possible with an undriven camera. For and their digital data can be accepted by software pro- bright stars (over mag 3) lenses of smaller aperture can be grammes such as AIP4WIN.2 They also have their own ad- used. I use two excellent Canon lenses of fixed focal length. vantages as their fields of view are relatively large. This makes One is the 85mm f1.8 lens which has an aperture of 52mm. variable stars easy to find and an image can sometimes in- This allows undriven photometry down to mag 8. -
Chapter 4 Introduction to Stellar Photometry
Chapter 4 Introduction to stellar photometry Goal-of-the-Day Understand the concept of stellar photometry and how it can be measured from astro- nomical observations. 4.1 Essential preparation Exercise 4.1 (a) Have a look at www.astro.keele.ac.uk/astrolab/results/week03/week03.pdf. 4.2 Fluxes and magnitudes Photometry is a technique in astronomy concerned with measuring the brightness of an astronomical object’s electromagnetic radiation. This brightness of a star is given by the flux F : the photon energy which passes through a unit of area within a unit of time. The flux density, Fν or Fλ, is the flux per unit of frequency or per unit of wavelength, respectively: these are related to each other by: Fνdν = Fλdλ (4.1) | | | | Whilst the total light output from a star — the bolometric luminosity — is linked to the flux, measurements of a star’s brightness are usually obtained within a limited frequency or wavelength range (the photometric band) and are therefore more directly linked to the flux density. Because the measured flux densities of stars are often weak, especially at infrared and radio wavelengths where the photons are not very energetic, the flux density is sometimes expressed in Jansky, where 1 Jy = 10−26 W m−2 Hz−1. However, it is still very common to express the brightness of a star by the ancient clas- sification of magnitude. Around 120 BC, the Greek astronomer Hipparcos ordered stars in six classes, depending on the moment at which these stars became first visible during evening twilight: the brightest stars were of the first class, and the faintest stars were of the sixth class. -
Photopic and Scotopic – the “Eyes” Have It
Photopic and Scotopic – The “eyes” have it Dick Erdmann GE Specification Engineer In the human eye the perceived brightness of illumination depends of color. It takes more energy in the blue or red portion of the color spectrum to create the same sensation of brightness as in the yellow-green region. When it comes to sensing light in the human eye there are two main light-sensing cells called rods and cones. If one took a tube and looked straight ahead through it so that it allowed the field of view to be restricted 2 degrees, light photons would fall on the part of the eye called the fovea that consists mainly of cones. The peripheral area surrounding the fovea consists of both rods and cones with the rods outnumbering the cones about 10:1. Cones have a peak response in the yellow-green region of about 555 nano-meters and rods have a peak response in the bluish-green area of about 505 nano-meters. Because both the rods and cones have been shown to have different sensitivities to colors they can be represented by two different sensitivity curves called Photopic Curves (representing the cone) and Scotopic Curves (representing the rod). Years ago it was thought that the cones were responsible for daytime vision and rods for nighttime vision. Because of this, light meters that measure lighting levels such as footcandles, lumens, lux, etc. are weighted to the cone activated part of the eye ignoring the effect of rod-activated vision. But according to a study by Dr. Sam Berman and Dr. -
Basics of Photometry Photometry: Basic Questions
Basics of Photometry Photometry: Basic Questions • How do you identify objects in your image? • How do you measure the flux from an object? • What are the potential challenges? • Does it matter what type of object you’re studying? Topics 1. General Considerations 2. Stellar Photometry 3. Galaxy Photometry I: General Considerations 1. Garbage in, garbage out... 2. Object Detection 3. Centroiding 4. Measuring Flux 5. Background Flux 6. Computing the noise and correlated pixel statistics I: General Considerations • Object Detection How do you mathematically define where there’s an object? I: General Considerations • Object Detection – Define a detection threshold and detection area. An object is only detected if it has N pixels above the threshold level. – One simple example of a detection algorithm: • Generate a segmentation image that includes only pixels above the threshold. • Identify each group of contiguous pixels, and call it an object if there are more than N contiguous pixels I: General Considerations • Object Detection I: General Considerations • Object Detection Measuring Flux in an Image • How do you measure the flux from an object? • Within what area do you measure the flux? The best approach depends on whether you are looking at resolved or unresolved sources. Background (Sky) Flux • Background – The total flux that you measure (F) is the sum of the flux from the object (I) and the sky (S). F = I + S = #Iij + npix " sky / pixel – Must accurately determine the level of the background to obtaining meaningful photometry ! (We’ll return to this a bit later.) Photometric Errors Issues impacting the photometric uncertainties: • Poisson Error – Recall that the statistical uncertainty is Poisson in electrons rather than ADU. -
Light Measurement Handbook from an Oblique Angle, It Should Look As Bright As It Did When Held Perpendicular to Your Line of Vision
Alex Ryer RED Boxes - LINKS to Current Info on Web Site Peabody, MA (USA) To receive International Light's latest Light Measurement Instruments Catalog, contact: InternationalInternational Light Technologies Light 10 Technology Drive Peabody,10 Te11 MA17 01960 Graf Road Tel:New (978) 818-6180 / buryport,Fax: (978) 818-8161 MA 01950 [email protected] / www.intl-lighttech.com Tel: (978) 465-5923 • Fax: (978) 462-0759 [email protected] • http://www.intl-light.com Copyright © 1997 by Alexander D. Ryer All Rights Reserved. No part of this publication may be reproduced or transmitted in any form or by any means, electronic or mechanical, including photocopying, recording, or any information storage and retrieval system, without permission in writing from the copyright owner. Requests should be made through the publisher. Technical Publications Dept. International Light Technologies 10 Technology Drive Peabody, MA 01960 ISBN 0-9658356-9-3 Library of Congress Catalog Card Number: 97-93677 Second Printing Printed in the United States of America. 2 Contents 1 What is Light? ........................................................... 5 Electromagnetic Wave Theory........................................... 5 Ultraviolet Light ................................................................. 6 Visible Light ........................................................................ 7 Color Models ....................................................................... 7 Infrared Light ..................................................................... -
An Introduction to Photometry and Photometric Measurements Henry
An introduction to photometry and photometric measurements Henry Joy McCracken Institut d’Astrophysique de Paris What is photometry? • Photometry is concerned with obtaining quantitative physical measurements of astrophysical objects using electromagnetic radiation. • The challenge is to relate instrumental measurements (like electrons counted in an electronic detector) to physically meaningful quantities like flux and flux density • The ability to make quantitative measurements transformed astronomy from a purely descriptive science to one with great explanative power. To print higher-resolution math symbols, click the Hi-Res Fonts for Printing button on the jsMath control panel. Brightness and Flux Density Astronomers learn about an astronomical source by measuring the strength of its radiation as a function of direction on the sky (by mapping or imaging) and frequency (spectroscopy), plus other quantities (time, polarization) that we ignore for now. We need precise and quantitative definitions to describe the strength of radiation and how it varies with distance between the source and the observer. The concepts of brightness and flux density are deceptively simple, but they regularly trip up experienced astronomers. It is very important to understand them clearly because they are so fundamental. We start with the simplest possible case of radiation traveling from a source through empty space (so there is no absorption, scattering, or emission along the way) to an observer. In the ray-optics approximation, radiated energy flows in straight lines. This approximation is valid only for systems much larger than the wavelength of the radiation, a criterion easily met by astronomical sources. You may find it helpful to visualize electromagnetic radiation as a stream of light particles (photons), essentially bullets that travel in straight lines at the speed of light. -
Transmission of Scotopic Signals from the Rod to Rod-Bipolar Cell in the Mammalian Retina
Vision Research 44 (2004) 3269–3276 www.elsevier.com/locate/visres Transmission of scotopic signals from the rod to rod-bipolar cell in the mammalian retina W. Rowland Taylor a,*, Robert G. Smith b a Neurological Sciences Institute, Oregon Health and Sciences University––West Campus, 505 NW 185th Avenue, Beaverton, OR 97006, United States b Department of Neuroscience, University of Pennsylvania, Philadelphia, PA Received 15 June 2004; received in revised form 27 July 2004 Abstract Mammals can see at low scotopic light levels where only 1 rod in several thousand transduces a photon. The single photon signal is transmitted to the brain by the ganglion cell, which collects signals from more than 1000 rods to provide enough amplification. If the system were linear, such convergence would increase the neural noise enough to overwhelm the tiny rod signal. Recent studies provide evidence for a threshold nonlinearity in the rod to rod bipolar synapse, which removes much of the background neural noise. We argue that the height of the threshold should be 0.85 times the amplitude of the single photon signal, consistent with the saturation observed for the single photon signal. At this level, the rate of false positive events due to neural noise would be masked by the higher rate of dark thermal events. The evidence presented suggests that this synapse is optimized to transmit the single photon signal at low scotopic light levels. Ó 2004 Elsevier Ltd. All rights reserved. Keywords: Retina; Synaptic transmission; Single photon; Photoreceptor; Visual threshold; Scotopic vision 1. Introduction produced by single photons are carried by only a few neurons, whereas all the rods and postreceptoral Many mammals have evolved excellent night vision, neurons in the pool generate noise. -
Comparative Visual Function in Predatory Fishes from the Indian River Lagoon Author(S): D
Comparative Visual Function in Predatory Fishes from the Indian River Lagoon Author(s): D. Michelle McComb, Stephen M. Kajiura, Andrij Z. Horodysky, and Tamara M. Frank Source: Physiological and Biochemical Zoology, Vol. 86, No. 3 (May/June 2013), pp. 285-297 Published by: The University of Chicago Press Stable URL: http://www.jstor.org/stable/10.1086/670260 . Accessed: 16/07/2013 16:00 Your use of the JSTOR archive indicates your acceptance of the Terms & Conditions of Use, available at . http://www.jstor.org/page/info/about/policies/terms.jsp . JSTOR is a not-for-profit service that helps scholars, researchers, and students discover, use, and build upon a wide range of content in a trusted digital archive. We use information technology and tools to increase productivity and facilitate new forms of scholarship. For more information about JSTOR, please contact [email protected]. The University of Chicago Press is collaborating with JSTOR to digitize, preserve and extend access to Physiological and Biochemical Zoology. http://www.jstor.org This content downloaded from 152.3.102.242 on Tue, 16 Jul 2013 16:00:41 PM All use subject to JSTOR Terms and Conditions 285 Comparative Visual Function in Predatory Fishes from the Indian River Lagoon D. Michelle McComb1,* Introduction Stephen M. Kajiura2 Teleost fishes represent a speciose vertebrate lineage that ra- Andrij Z. Horodysky3 diated into distinct aquatic habitats that present unique diver- Tamara M. Frank4 gent light qualities (Jerlov 1968). Selective pressure on the pi- 1Harbor Branch Oceanographic Institute at Florida Atlantic scine eye has resulted in an extensive array of both 2 University, Fort Pierce, Florida 34946; Biological Sciences, morphological and physiological adaptations to maximize vi- Florida Atlantic University, Boca Raton, Florida 33431; sual function under differing light conditions.