AGA5802 Spectroscopy II Prism Gratings Applications
|
|
- Kellie Thompson
- 6 years ago
- Views:
Transcription
1 AGA5802 Spectroscopy II Prism Gratings Applications Bibliography: To Measure the Sky, Kitchin, Lena and others... Prof. Jorge Meléndez 1
2 Slit Basic components of the Spectrograph Prism or grating Roy & Clarke 2
3 Dispersing element Diffraction Grating: diffraction+interference Prism: differential refraction 3
4 Homework #5: build an spectrograph based on a CD or DVD grating : deadline May 4th 07/issue4/spectrometer pt/2007/issue4/spectrometer stro/html/spectrometer.html 4
5 Emission lines in compact fluorescent lamp using spectrograph built by undergrad student of Stellar Astrophysics USP
6 Prism as a dispersing element q exit? n air sin q air = n glass sin q glass q exit n(air) = Kitchin 6
7 Dispersing element: prism 7
8 Snell law in a prism 1 (or n 1 ) is ~ 1 (air), so : n 1 sin i 1 = n 2 sin r 1 means that n 2 = sin i 1 / sin r 1 In the same way : n 2 sin i 2 = n 1 sin r 2 n 2 = sin r 2 / sin i 2 a q r 2 i 1 r 1 i 2 Kitchin 8
9 Refractive index ( l or n l ) varies with wavelength In the visible the variation of n l may be approximated by the Hartmann dispersion formula. A, B and C are known as the Hartmann constants Kitchin 9
10 10
11 a For a given l, the deviation angle is q q r i 1 + a = 180 a q a q r 2 i 1 r 1 i 2 a + 90 r i 2 = Kitchin
12 For a given l, the deviation angle is q a sin r 2 = l sin i 2 i 2 = a r 1 sin r 1 = sin i 1 / l q r 2 i 1 r 1 i 2 r 2 12 Kitchin
13 Maximizing dispersion Dq/Dl Example for dense flint prism Kitchin 13
14 Dq/Dl ( 0 m -1 ) Variation of Dq/Dl with angle of incidence i 1 for different a i 1 a q x10 7 a = 50 73, ,7 73 a = 70 Maximum dispersion of 1,02 x m -1 occurs for i 1 = 90 0 and an apex angle of 73, a = i 1 14
15 Maximizing dispersion Dq/Dl symmetrical passage of the ray through the prism maximizes dispersion and minimizes optical aberrations 15
16 symmetrical passage is also called position of minimum deviation (of q) Example: deviation q for a dense flint prism with apex angle a = 30 O at l = 500 nm q a i 1 r 2 r 1 i 2 minimum deviation At min dev, r 1 = i 2 = a/2 i 1 16
17 a i 1 r 2 r 1 i 2 At min deviation r 1 = i 2 = a/2 symmetrical passage 17
18 Compromise, a = 60 O a r 1 =? dispersion of a prism increases rapidly towards shorter l 18
19 Spectrograph based on prism CCD 19
20 Objective prism spectrograph 20
21 Classic applications of spectrographs 21
22 The beginning of stellar spectroscopy 1802: William Wollaston first observed dark lines in the solar spectrum which he incorrectly interpreted as gaps separating the colors 1817: Joseph Fraunhofer (1817) observed a continuous color change without color discontinuities at the dark lines. He found 574 lines. 1836: Sir David Brewster found that certain lines had strengths that varied with the Sun's elevation. He correctly ascribed these as originating in the terrestrial atmosphere. O 2 (B) O 2 (A) Ca II (K) (H) Ca(g) 4227 H (h) 4102 Fe(e) 4384 H (f) 4340 CH, Fe (G) 4308 Fe (d) 4668 H Fe (F) (E) Mg (b 1, b 2 ) 5184 & 5173 Fe (c) 4958 Na 5890 & 5896 D 2 D 1 Ha (C) 6563
23 Stellar classification Secchi's Classes of Stellar Spectra ( ) Secchi's four classes of stellar spectra, from a colored lithograph in a book published around The principal spectral lines are identified underneath by letters that Fraunhofer assigned. Type I: white-blue; strong H lines. Current class A & early F Type II: yellow, tipo solare. Numerous metallic lines (Na, Ca, Fe), with weaker H. Current class G, K, late F Type III: orangered; metallic lines and bands. Current class M Type IV: stars with emission lines
24 The Harvard classification system s: Harvard classification (E.Pickering + Williamina Fleming + Antonia Maury + Annie J. Cannon): O, B, A, F, G, K, M Women Harvard
25 Stellar classification: O, B, A, F, G, K, M Based on spectra taken at the Harvard North (USA) & South (Arequipa, Peru) stations Annie J. Cannon classified > spectra!
26 The Henry Draper (HD) catalogue Ultimately listed over stars. It is still very useful; the most common ID of stars with V < 9 is its HD number (also HIP) Harvard plate taken with objective prism spectrograph in Arequipa. Field of η Carinae. E. Dorrit Hoffleit, 2002, Phys. Perspect., 4, 370
27 Luminosity class Antonia Maury : hired in 1888 by E. Pickering (Harvard) to classify spectra. She proposed a new system considering also the width of the lines, but was ignored Pickering. Dwarf Supergiant
28 Wavelength (nm)
Stellar Astrophysics: The Classification of Stellar Spectra
Stellar Astrophysics: The Classification of Stellar Spectra Temperature and Color The intensity of light emitted by three hypothetical stars is plotted against wavelength The range of visible wavelengths
More informationSun. Sirius. Tuesday, February 21, 2012
Spectral Classification of Stars Sun Sirius Stellar Classification Spectral Lines H Fe Na H Ca H Spectral Classification of Stars Timeline: 1890s Edward C. Pickering (1846-1919) and Williamina P. Fleming
More informationAstonomy 62 Lecture #10. Last Time. Applications of Stefan-Boltzmann Law Color Magnitudes Color Index
Last Time Applications of Stefan-Boltzmann Law Color Magnitudes Color Index Standard Visual Band Filters U B V R I Flux through filter X: F x = 0 F S x d F x F x W x Apparent Color Magnitude: m x,1 m x,2
More informationFYI: Spectral Classification & Stellar Spectra. 1. Read FYI: Spectral Classification A Look Back and FYI: Stellar Spectra What s in a Star?
FYI: Spectral Classification & Stellar Spectra E3:R1 1. Read FYI: Spectral Classification A Look Back and FYI: Stellar Spectra What s in a Star? As you read use the spaces below to write down any information
More informationScience Lab I Properties of Light
Art & Science of Light Fall 2007 Science Lab I Properties of Light Prepared by: Dr. Dharshi Bopegedera 1 Using the Filtergraph (15 minutes) 1. Turn on the filtergraph, place a card on it and look at the
More informationThe Sun and the Stars
Classification of stellar spectra Potted History : 1802 William Wallaston showed that the spectrum of the sun is not simply a continuous spectrum, but is broken up by a series of dark lines (absorption
More informationAtomic Spectra in Astrophysics
Atomic Spectra in Astrophysics Potsdam University : Dr. Lidia Oskinova lida@astro.physik.uni-potsdam.de Fundamentals of stellar classification 01 Stars are made of hot, dense gas Continuous spectrum from
More informationAstronomical Spectroscopy Introduction PMO David Haworth Copyright 2014
Astronomical Spectroscopy Introduction PMO 2014 David Haworth www.stargazing.net/david Copyright 2014 Astronomical Spectroscopy Astrophysics Quantum Mechanics Electromagnetic spectrum provides insight
More informationThe Temperatures of Stars. Image credit: NOAO
The Temperatures of Stars Image credit: NOAO Understanding Stars Starlight contains a lot of information. This information doesn t decay or expire as the light travels through space. By examining the light
More informationOptical/IR Observational Astronomy Spectroscopy. David Buckley, SALT
David Buckley, SALT 1 Background is really just monochromatic photometry History 1637 Descartes explained the origin of the rainbow. 1666 Newton s classic experiments on the nature of colour. 1752 Melvil
More informationStars: Intro & Classification
Stars: Intro & Classification Astronomy 1 Elementary Astronomy LA Mission College Spring F2015 Quotes & Cartoon of the Day The wonder is, not that the field of stars of so vast, but that man has measured
More informationhf = E 1 - E 2 hc = E 1 - E 2 λ FXA 2008 Candidates should be able to : EMISSION LINE SPECTRA
1 Candidates should be able to : EMISSION LINE SPECTRA Explain how spectral lines are evidence for the existence of discrete energy levels in isolated atoms (i.e. in a gas discharge lamp). Describe the
More informationA Stellar Spectra 3. Stars shine at night (during the day too!). A star is a self-luminous sphere of gas. Stars are held together by gravity.
Stellar Spectra Relativity and Astrophysics Lecture 12 Terry Herter Outline What is a star? Stellar Spectra Kirchhoff s Laws Spectral Classification Spectral Types: O B A F G K M L T Stellar Photometry
More informationOverview: Astronomical Spectroscopy
Overview: Astronomical Spectroscopy or How to Start Thinking Creatively about Measuring the Universe Basic Spectrograph Optics Objective Prism Spectrometers - AESoP Slit Spectrometers Spectrometers for
More informationLecture 2. In this lecture we will go through the chronological development of the Atomic physics.
Lecture 2 TITLE: A brief history of the development of structure of atom Page 1 Objectives In this lecture we will go through the chronological development of the Atomic physics. We will find out the thoughts
More informationThe History and Philosophy of Astronomy
Astronomy 350L (Fall 2006) The History and Philosophy of Astronomy (Lecture 16: Birth of Astrophysics I) Instructor: Volker Bromm TA: Jarrett Johnson The University of Texas at Austin Big Q: What is the
More informationDistances to the stars Friedrich Bessel Cygni 10 light years. Just beat Struve and Henderson who measured Vega and α Centauri respectively.
Distances to the stars Friedrich Bessel 1838 61 Cygni 10 light years. Just beat Struve and Henderson who measured Vega and α Centauri respectively. Distances to the stars the technique p < 1arcsecond d
More informationChapter 4. Spectroscopy. Dr. Tariq Al-Abdullah
Chapter 4 Spectroscopy Dr. Tariq Al-Abdullah Learning Goals: 4.1 Spectral Lines 4.2 Atoms and Radiation 4.3 Formation of the Spectral Lines 4.4 Molecules 4.5 Spectral Line Analysis 2 DR. T. AL-ABDULLAH
More informationLecture 7: Optical Spectroscopy. Astrophysical Spectroscopy. Broadband Filters. Fabry-Perot Filters. Interference Filters. Prism Spectrograph
Lecture 7: Optical Spectroscopy Outline 1 Astrophysical Spectroscopy 2 Broadband Filters 3 Fabry-Perot Filters 4 Interference Filters 5 Prism Spectrograph 6 Grating Spectrograph 7 Fourier Transform Spectrometer
More information13.3 Spectra of Stars
13.3 Spectra of Stars A star's spectrum depicts the energy it emits at each wavelength and is perhaps the single most important thing we can know about the star. From the spectrum we can find the star's
More informationChapter 35 Diffraction and Polarization. Copyright 2009 Pearson Education, Inc.
Chapter 35 Diffraction and Polarization 35-1 Diffraction by a Single Slit or Disk If light is a wave, it will diffract around a single slit or obstacle. 35-1 Diffraction by a Single Slit or Disk The resulting
More informationEXPERIMENT 09 OBSERVATION OF SPECTRA
EXPERIMENT 09 OBSERVATION OF SPECTRA INTRODUCTION: In physics, as in very other area of study, one of the most valuable questions a student can learn to ask is, How do they know that? Thus, when you read
More informationAS 101: Day Lab #2 Summer Spectroscopy
Spectroscopy Goals To see light dispersed into its constituent colors To study how temperature, light intensity, and light color are related To see spectral lines from different elements in emission and
More informationLight or the Electromagnetic spectrum.
Light or the Electromagnetic spectrum www.nasa.gov Diffraction and Light When passed through a prism or grating, light is separated into its component wavelengths This looks like a rainbow in visible light
More informationSpectroscopy in Astronomy
Spectroscopy in Astronomy History 1814 German optician Joseph von Fraunhofer sun with 600+ spectral lines; now we know more than 3000 lines 1860 German chemists Gustav Kirchhoff and Robert W. Bunsen Chemical
More informationName: Partner(s): 1102 or 3311: Desk # Date: Spectroscopy Part I
Name: Partner(s): 1102 or 3311: Desk # Date: Spectroscopy Part I Purpose Investigate Kirchhoff s Laws for continuous, emission and absorption spectra Analyze the solar spectrum and identify unknown lines
More informationA History of Astronomical Spectroscopy
CHAPTER TWO A History of Astronomical Spectroscopy The publication of Kirchhoff s and Bunsen s work brought the awareness of the spectroscope, and what it could reveal, to a wider audience, including astronomers.
More informationHertzsprung-Russell Diagram, Flux, Luminosity, Magnitude 10 Oct
Russell Diagram, Flux, Luminosity, Magnitude 10 Oct Outline Review of 7 Oct Thermal radiation Wien s Law Stefan Boltzmann Law How to measure temperature of stars. AJ Cannon s method of classifying spectra.
More informationCollege of San Mateo Observatory
College of San Mateo Observatory Stellar Spectra Catalog SGS Spectrograph Spectra taken from CSM observatory using SBIG Self Guiding Spectrograph (SGS) A work in progress compiled by faculty, staff, and
More informationSETI and the Spectral Classification of Stars By: J.D.R. Bahng
North American AstroPhysical Observatory (NAAPO) Cosmic Search: Issue 9 (Volume 3 Number 1; Winter 1981) [Article in magazine started on page 2] SETI and the Spectral Classification of Stars By: J.D.R.
More informationParallax: Space Observatories. Stars, Galaxies & the Universe Announcements. Stars, Galaxies & Universe Lecture #7 Outline
Stars, Galaxies & the Universe Announcements HW#4: posted Thursday; due Monday (9/20) Reading Quiz on Ch. 16.5 Monday (9/20) Exam #1 (Next Wednesday 9/22) In class (50 minutes) first 20 minutes: review
More informationChapter 35 Diffraction and Polarization
Chapter 35 Diffraction and Polarization If light is a wave, it will diffract around a single slit or obstacle. The resulting pattern of light and dark stripes is called a diffraction pattern. This pattern
More informationn(λ) = c/v(λ). Figure 1: Dispersion curves for some common optical glass types.
Physics 2310 Lab 2: The Dispersion of Optical Glass Dr. Michael Pierce (Univ. of Wyoming) Based on a lab by Dr. M. Kruger (Univ. of Missouri, Kansas City) Purpose: The purpose of this lab is to introduce
More informationContents Introduction to spectroscopy, spectroscopes and spectrographs The analysis of sunlight: the earliest pioneers
Preface to the second edition Preface to the first edition, 1986 Acknowledgements Acknowledgements for the second edition Acknowledgements for the first edition (1986) xi xiii xv xv xv 1 Introduction to
More informationSPECTRAL WORKSHOP. Picture of the lamps, professional spectroscopes and 'DIY' spectroscopes. Larger view of the 'DIY' spectroscopes
SPECTRAL WORKSHOP OVERVIEW I STEP-BY-STEP GUIDE Equipment List Workshop guides II ADDITIONAL MATERIAL Picture of the lamps, professional spectroscopes and 'DIY' spectroscopes III Larger view of the 'DIY'
More informationSPH4U UNIVERSITY PHYSICS
SPH4U UNIVERSITY PHYSICS THE WAVE NATURE OF LIGHT L (P.520-525) Wave Nature of Light Not only did Young s double-slit experiment demonstrate the wave nature of light, it also paved the way for applications
More informationThe Fundamentals of Spectroscopy: Theory BUILDING BETTER SCIENCE AGILENT AND YOU
The Fundamentals of Spectroscopy: Theory BUILDING BETTER SCIENCE AGILENT AND YOU 1 Agilent is committed to the educational community and is willing to provide access to company-owned material. This slide
More informationOptical/NIR Spectroscopy A3130. John Wilson Univ of Virginia
Optical/NIR Spectroscopy A3130 John Wilson Univ of Virginia Topics: Photometry is low resolution spectroscopy Uses of spectroscopy in astronomy Data cubes and dimensionality challenge Spectrograph design
More informationThe Spectra of Stars and Binary Stars (Masses and Radii)
The Spectra of Stars and Binary Stars (Masses and Radii) Colors of Stars Stars are made of hot, dense gas Con$nuous spectrum from the lowest visible layers ( photosphere ). Approximates a blackbody spectrum.
More informationDISPERSION VERY SHORT ANSWER QUESTIONS. Two identical prisms made of the same material placed with their based on opposite sides (of the
DISPERSION VERY SHORT ANSWER QUESTIONS Q-1. What will be the spectrum of sun during a total solar eclipse? Q-2. Why the secondary rainbow is always fainter than the primary rainbow? Q-3. Two identical
More informationDAY LABORATORY EXERCISE: SPECTROSCOPY
AS101 - Day Laboratory: Spectroscopy Page 1 DAY LABORATORY EXERCISE: SPECTROSCOPY Goals: To see light dispersed into its constituent colors To study how temperature, light intensity, and light color are
More informationLIGHT. Question. Until very recently, the study of ALL astronomical objects, outside of the Solar System, has been with telescopes observing light.
LIGHT Question Until very recently, the study of ALL astronomical objects, outside of the Solar System, has been with telescopes observing light. What kind of information can we get from light? 1 Light
More informationUNIVERSITY COLLEGE LONDON. PHAS : Classification of Stellar Spectra
UNIVERSITY COLLEGE LONDON University Of London Observatory PHAS1510 Certificate in Astronomy 0708.01 PHAS1510-02: Classification of Stellar Spectra Name: An experienced student should aim to spend not
More informationThe Spectroscopy of Stars
The Spectroscopy of Stars In this activity you will use a hand held spectroscope to investigate a number of known and unknown light sources. A spectroscope is an instrument that helps to observe the spectrum
More informationLecture 14: Studying the stars. Astronomy 111 Monday October 16, 2017
Lecture 14: Studying the stars Astronomy 111 Monday October 16, 2017 Reminders Homework #7 due Monday I will give a lecture on DES and LIGO tomorrow at 4pm in the Mitchell Institute Studying the stars
More informationRADIAL VELOCITIES AND SPECTRAL TYPES FOR FOURTEEN STARS *
RADIAL VELOCITIES AND SPECTRAL TYPES FOR FOURTEEN STARS * NANCY G. ROMAN National Aeronautics and Space Administration Washington, D.C. Kitt Peak National Observatoryt Tucson, Arizona Received December
More informationAstronomical Techniques
Astronomical Techniques Spectrographs & Spectroscopy Spectroscopy What is spectroscopy? A little history. What can we learn from spectroscopy? Play with simple spectrographs. Basic optics of a spectrograph.
More informationPhys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 5
Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 5 MULTIPLE CHOICE 1. What is the wavelength of the longest wavelength light visible to the human eye? a. 400 nm b. 4000 nm c. 7000 nm
More informationHistorical Remarks. 1.1 Early Pioneers
1 Historical Remarks The purpose of this book is to provide an introduction to present-day astronomical spectroscopy. Thus, this chapter on the historical development will be restricted to a brief outline
More informationChapter 10 Measuring the Stars
Chapter 10 Measuring the Stars Some of the topics included in this chapter Stellar parallax Distance to the stars Stellar motion Luminosity and apparent brightness of stars The magnitude scale Stellar
More informationHertzsprung-Russell Diagram 7 Oct
Hertzsprung-Russell Diagram 7 Oct Outline Thermal radiation Wien s Law Stefan Boltzmann Law Hertzsprung Russell diagram There are 3 types of stars: main sequence or dwarfs, giants, white dwarfs Missouri
More informationOptical/IR Observational Astronomy Telescopes I: Telescope Basics. David Buckley, SAAO
David Buckley, SAAO 27 Feb 2012 1 Some other Telescope Parameters 1. Plate Scale This defines the scale of an image at the telescopes focal surface For a focal plane, with no distortion, this is just related
More informationReview: Properties of a wave
Radiation travels as waves. Waves carry information and energy. Review: Properties of a wave wavelength (λ) crest amplitude (A) trough velocity (v) λ is a distance, so its units are m, cm, or mm, etc.
More informationTaking fingerprints of stars, galaxies, and interstellar gas clouds. Absorption and emission from atoms, ions, and molecules
Taking fingerprints of stars, galaxies, and interstellar gas clouds Absorption and emission from atoms, ions, and molecules 1 Periodic Table of Elements The universe is mostly hydrogen H and helium He
More informationPreview from Notesale.co.uk Page 1 of 38
F UNDAMENTALS OF PHOTONICS Module 1.1 Nature and Properties of Light Linda J. Vandergriff Director of Photonics System Engineering Science Applications International Corporation McLean, Virginia Light
More informationCharacterizing Stars
Characterizing Stars 1 Guiding Questions 1. How far away are the stars? 2. What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a first-magnitude or second magnitude star?
More informationOhio University - Lancaster Campus slide 1 of 47 Spring 2009 PSC 100. A star s color, temperature, size, brightness and distance are all related!
Ohio University - Lancaster Campus slide 1 of 47 A star s color, temperature, size, brightness and distance are all related! Ohio University - Lancaster Campus slide 2 of 47 The Beginnings Late 1800 s,
More informationCharacterizing Stars. Guiding Questions. Parallax. Careful measurements of the parallaxes of stars reveal their distances
Guiding Questions Characterizing Stars 1. How far away are the stars? 2. What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a first-magnitude or second magnitude star?
More informationTHE SPECTRUM OF A STAR
THE SPECTRUM OF A STAR Overview: Stars can be classified by using the general shape and specific lines of their spectra. Objectives: The student will: perform a simple analysis of spectral lines to classify
More informationMass-Luminosity and Stellar Lifetimes WS
Name Mass-Luminosity and Stellar Lifetimes WS The graph shows the Mass-Luminosity Relationship for main sequence stars. Use it to answer questions 1-3. 1) A star with a mass of 0.5 solar masses would be
More informationBuy-back points tallied and added: 750 points bought-back. Last Withdrawal date: this friday, Oct 31st.
Announcements HW #3: Available online now. Due in 1 week, Nov 3rd, 11pm. Buy-back points tallied and added: 750 points bought-back. Last Withdrawal date: this friday, Oct 31st. Evening Observing: next
More informationTaking Fingerprints of Stars, Galaxies, and Other Stuff. The Bohr Atom. The Bohr Atom Model of Hydrogen atom. Bohr Atom. Bohr Atom
Periodic Table of Elements Taking Fingerprints of Stars, Galaxies, and Other Stuff Absorption and Emission from Atoms, Ions, and Molecules Universe is mostly (97%) Hydrogen and Helium (H and He) The ONLY
More informationIntroduction to Stellar Spectra
Introduction to Stellar Spectra We are about to start down a long road as we search for the chemical composition of the stars. The journey won't be short, or easy, but along the way you'll meet a number
More informationAPAS Laboratory { PAGE } Spectroscopy SPECTROSCOPY
SPECTROSCOPY SYNOPSIS: In this lab you will eplore different types of emission spectra, calibrate a spectrometer using the spectrum of a known element, and use your calibration to identify an unknown element.
More informationPhotosphere. Bob Stein s simulation movie. Chromosphere. Corona. Solar wind
Photosphere Layer from which light escapes directly into space. Photosphere is what we see. Light from lower layers scatters. Q: Suppose we observe the neutrinos from the sun. The size of the sun when
More informationStars: some basic characteristics
Stars: some basic characteristics Stars! How bright are they? How massive are they? What are the different types? How long do they live? How hot are they? Stellar brightness and luminosity The apparent
More informationDiscussion. Summary Clicker -- Solar Wind. What are effects of solar activity on our technological society? A. Auroral
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nicholas Nelson Lecture 10 Thur 10 Feb 11 zeus.colorado.edu/astr1040-toomre toomre Planetary Nebula NGC 3132 Today What can we measure in other
More informationChapter 8. Spectroscopy. 8.1 Purpose. 8.2 Introduction
Chapter 8 Spectroscopy 8.1 Purpose In the experiment atomic spectra will be investigated. The spectra of three know materials will be observed. The composition of an unknown material will be determined.
More informationLecture 2: Basic Astronomical Optics. Prisms, Lenses, and Mirrors
Lecture 2: Basic Astronomical Optics Prisms, Lenses, and Mirrors Basic Optical Elements Refraction (Lenses) No longer used for large telescopes Widely used for instrument optics Reflection (mirrors) Widely
More informationLights. And God said, "Let there be light"; and there was light. And God saw that the light was good; (Bible: Genesis I)
Lights Astronomy is based on observing lights from celestial bodies. And God said, "Let there be light"; and there was light. And God saw that the light was good; (Bible: Genesis I) Cat's Eye planetary
More informationBook page cgrahamphysics.com Stellar Spectra
Book page 650-652 Stellar Spectra Emission and absorption Spectra The black lines of the absorption spectrum match up with the bright lines of the emission spectrum Spectra unique to each element Emission
More informationGalaxies Galore. Types of Galaxies: Star Clusters. Spiral spinning wit arms Elliptical roundish Irregular no set pattern
Stars Studying Stars Astronomers use a spectroscope to study the movement of stars Blue shift towards earth Red shift away from earth Change in a wavelength moving toward or away from earth is the Doppler
More informationTaking fingerprints of stars, galaxies, and interstellar gas clouds
- - Taking fingerprints of stars, galaxies, and interstellar gas clouds Absorption and emission from atoms, ions, and molecules Periodic Table of Elements The universe is mostly hydrogen H and helium He
More informationSkoog Chapter 6 Introduction to Spectrometric Methods
Skoog Chapter 6 Introduction to Spectrometric Methods General Properties of Electromagnetic Radiation (EM) Wave Properties of EM Quantum Mechanical Properties of EM Quantitative Aspects of Spectrochemical
More informationSpeed of Light in Glass
Experiment (1) Speed of Light in Glass Objective:- This experiment is used to determine the speed of propagation of light waves in glass. Apparatus:- Prism, spectrometer, Halogen lamp source. Theory:-
More informationPHY410 Optics Exam #3
PHY410 Optics Exam #3 NAME: 1 2 Multiple Choice Section - 5 pts each 1. A continuous He-Ne laser beam (632.8 nm) is chopped, using a spinning aperture, into 500 nanosecond pulses. Compute the resultant
More informationWe now realize that the phenomena of chemical interactions, and, ultimately life itself, are to be understood in terms of electromagnetism".
We now realize that the phenomena of chemical interactions, and, ultimately life itself, are to be understood in terms of electromagnetism". -Richard Feynman Quantum H Atom Review Radia Wave Function (1s):
More informationLaboratory Exercise. Atomic Spectra A Kirchoff Potpourri
1 Name: Laboratory Exercise Atomic Spectra A Kirchoff Potpourri Purpose: To examine the atomic spectra from several gas filled tubes and understand the importance of spectroscopy to astronomy. Introduction
More informationDiffraction gratings. B.Tech-I
Diffraction gratings B.Tech-I Introduction Diffraction grating can be understood as an optical unit that separates polychromatic light into constant monochromatic composition. Uses are tabulated below
More informationExperiment 7: Spectrum of the Hydrogen Atom
Experiment 7: Spectrum of the Hydrogen Nate Saffold nas2173@columbia.edu Office Hour: Mondays, 5:30-6:30PM INTRO TO EXPERIMENTAL PHYS-LAB 1493/1494/2699 Introduction The physics behind: The spectrum of
More informationTHE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES DAVID F. GRAY University of Western Ontario, London, Ontario, Canada CAMBRIDGE UNIVERSITY PRESS Contents Preface to the first edition Preface to the
More informationSpectral Classification of Stars
Sun Sirius Stellar Classification Spectral Lines CaH H Fe Na H Timeline: Edward C. Pickering (1846-1919) and Williamina P. Fleming 1890s (1857-1911) label spectra alphabetically according to strength of
More informationPhys102 Lecture Diffraction of Light
Phys102 Lecture 31-33 Diffraction of Light Key Points Diffraction by a Single Slit Diffraction in the Double-Slit Experiment Limits of Resolution Diffraction Grating and Spectroscopy Polarization References
More informationChapter 15 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Surveying the Stars Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition Surveying the Stars 15.1 Properties of Stars How do we measure stellar luminosities? How do we measure stellar temperatures? How do we measure
More informationAstrophysical Techniques. opt nd Year Astrophysics Group Research Project
Astrophysical Techniques opt.292 2 nd Year Astrophysics Group Research Project Paul O Brien & Rhaana Starling For this lecture and lab handout see http://www2.star.le.ac.uk/pto/astrolab2.html Aim of this
More informationChapter 6 Telescopes: Portals of Discovery. Agenda. How does your eye form an image? Refraction. Example: Refraction at Sunset
Chapter 6 Telescopes: Portals of Discovery Agenda Announce: Read S2 for Thursday Ch. 6 Telescopes 6.1 Eyes and Cameras: Everyday Light Sensors How does your eye form an image? Our goals for learning How
More information1. The symbols below represent the Milky Way galaxy, the solar system, the Sun, and the universe.
Name Date 1. The symbols below represent the Milky Way galaxy, the solar system, the Sun, and the universe. 4. The diagram below illustrates three stages of a current theory of the formation of the universe.
More informationQuantum Mechanics and Stellar Spectroscopy.
Quantum Mechanics and Stellar Spectroscopy http://apod.nasa.gov/apod/ Recall the electric force. Like gravity it is a 1/r 2 force/ That is: F elec = Z 1 Z 2 e2 r 2 where Z 1 and Z 2 are the (integer) numbers
More informationFor instance, for a particular star cluster, these data were derived:
Astronomy 100 Name(s): Exercise 5: The H-R diagram and spectroscopy A very basic correlation using the color index By the 1920 s, various astronomers had evidence that the temperature of a star was also
More informationProperties of Stars (continued) Some Properties of Stars. What is brightness?
Properties of Stars (continued) Some Properties of Stars Luminosity Temperature of the star s surface Mass Physical size 2 Chemical makeup 3 What is brightness? Apparent brightness is the energy flux (watts/m
More informationMeasuring Radial & Tangential Velocity. Radial velocity measurement. Tangential velocity measurement. Measure the star s Doppler shift
17. The Nature of the Stars Parallax reveals stellar distance Stellar distance reveals luminosity Luminosity reveals total energy production The stellar magnitude scale Surface temperature determines stellar
More informationThe Electromagnetic Spectrum
The Electromagnetic Spectrum Outcomes: http://www.avclub.com/article/marvel-made-its-own-movies-ang-lee-offered-idiosyn-204118 Qualitatively describe the electromagnetic spectrum in terms of frequency,
More informationTelescopes: Portals of Discovery
Telescopes: Portals of Discovery How do light and matter interact? Emission Absorption Transmission Transparent objects transmit light Opaque objects block (absorb) light Reflection or Scattering Reflection
More informationOptical Spectrometers
Optical Spectrometers Prism Spectrometers Grating Spectrometers Interferential Spectrometers Hyperspectral Spectrometers Credit: www.national.com Experimental Methods in Physics [2011-2012] EPFL - SB -
More informationModern Astronomy Review #1
Modern Astronomy Review #1 1. The red-shift of light from distant galaxies provides evidence that the universe is (1) shrinking, only (3) shrinking and expanding in a cyclic pattern (2) expanding, only
More informationThe Spectroscope: New Meanings in Light
TOPIC 3 The Spectroscope: New Meanings in Light Now that astronomers could gaze deeper into the universe using simple telescopes, they faced a new challenge the stars. Galileo had seen the stars through
More informationRAY OPTICS 6. DISPERSION POINTS TO REMEMBER
Y OPTICS 6. DISPESION POINTS TO EMEMBE. Dispersion : a) The splitting of white light into constituent colours is called dispersion and the band of colours is called spectrum. b) Dispersion of light was
More informationAstronomy. Optics and Telescopes
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Optics and Telescopes - Refraction, lenses and refracting telescopes - Mirrors and reflecting telescopes - Diffraction limit,
More informationPlanetary Science: Investigations 9-10 I-Check Quiz STUDY GUIDE- ANSWER KEY Name HR Date
1. How are different types of radiation arranged along the electromagnetic spectrum? A. By how fast they travel incorrect answer B. By their sources incorrect answer C. By the amount of energy they carry
More informationChapter 6 Telescopes: Portals of Discovery
Chapter 6 Telescopes: Portals of Discovery 6.1 Eyes and Cameras: Everyday Light Sensors Our goals for learning: How does your eye form an image? How do we record images? How does your eye form an image?
More information