Learning Objectives. distances to objects in our Galaxy and to other galaxies? apparent magnitude key to measuring distances?
|
|
- Roy Grant
- 5 years ago
- Views:
Transcription
1 The Distance Ladder
2 Learning Objectives! What is the distance ladder? How do we measure distances to objects in our Galaxy and to other galaxies?! How are the concepts of absolute magnitude and apparent magnitude key to measuring distances?! What are the main techniques to measure distances? To what approximate distance can each technique be used?! What are Hubble s Law and Constant? How were they discovered? Can we use them to measure distances?! Are any distant galaxies blueshifted? Does the expansion of the Universe mean that we are at the center of the Universe? Are people expanding (and why or why not)?! How is the Universe structured? Are galaxies isolated?
3 Measuring Distances! To study the structure of the Universe we need to know the distance of different objects! Basic idea (other than gold standard parallax):! Determine the intrinsic brightness of an object! Absolute magnitude! Compare to the observed brightness in our sky! Apparent magnitude! Use the difference between apparent and absolute magnitude to determine the distance! No method is good for all distances! Different techniques have been developed for different distances
4 The Distance Ladder! Methods of finding distances in the Universe build on other methods! We step farther into the Universe with each method Parallax (from Gaia) as far as 8 kpc distance
5 Spectroscopic Distances! For nearby stars, we find distances by parallax! For more distant stars if we can determine a star s type (i.e. O, B, A F, G, K, M), we can use the H-R diagram to find its absolute magnitude! This is easy with star clusters, since we can match to the Main Sequence! This technique is called spectroscopic distance
6 Cepheid Variable Stars! Pulsating supergiant stars! They re bright visible out to about 30 million parsecs (100 million light years!)! Pulsation period is directly related to intrinsic luminosity (i.e. to absolute magnitude) Measure pulsation period from light curve
7 White Dwarf Supernovae! Because white dwarf (Type Ia) supernovae happen at a similar mass (about the Chandrasekhar limit), the explosions are always similar in energy! Absolute brightnesses of these supernovae should be the same! Problem: We have to wait for them to happen. Fortunately, they re fairly common! This method currently gets us out in distance to over 3 billion parsecs (10 billion light years) White dwarf Supernova
8 Galaxy Spectra! Since the light from galaxies comes mostly from stars, galaxy spectra look like a lot of spectra of stars added together
9 Redshifted Galaxies! In 1928, Hubble observed that the spectral lines of essentially all galaxies are redshifted! They appear to be receding (moving away) from us!! Exceptions are the 1 or 2 very closest galaxies (e.g. the Andromeda galaxy is blueshifted)! Redshift (z) in terms of observed (λ obs ) and emitted (λ em ) wavelength (where λ em is the wavelength we d measure on Earth for that line): z = (λ obs -λ em )/λ em! At low redshifts, the resulting Doppler velocity is just a fraction of the speed of light (c), i.e. v = cz
10 Spectrum shifts redder and redder blueshift redshift
11 Most Important Astronomical Discovery of the 20th Century Plot from Edwin Hubble s original 1929 paper which first described the expansion of the Universe
12 ! Hubble noticed a correlation between redshift and distance! The farther a galaxy is from us, the faster it moves away from us! This can be described by the equation v=h o d Hubble s Law! Where v is velocity in km/s, d is distance in millions of parsecs (Mpc), and H o is the Hubble constant! Current best estimate of H o is about 70 km/s/mpc
13 What Does This Mean?! More distant objects appear to move away from us faster! From any galaxy s point of view, every other galaxy appears to be moving away from it! THE UNIVERSE IS EXPANDING!!!
14 What Does This NOT Mean?! We are NOT in a special location (because from any galaxy s point of view, every other galaxy appears to move away)! Note that planets, stars individual galaxies, cats that love teddy bears are NOT being pulled apart. Over small distances, the expansion of the Universe does NOT overcome the forces that bind atoms
15 Redshift and Distance! The Hubble Law gives us a new way of finding distances! Remember,! v=cz! v=h o d! Therefore, d=cz/h o! We can now measure distances to extremely distant galaxies just by taking a spectrum and using it to measure a galaxy s redshift
16 The Local Group
17 The Virgo Cluster! Over 1,000 galaxies! 50 million light-years away from our Milky Way galaxy! About 13 million lightyears across! Dominated by three giant elliptical galaxies
18 Structure of the Universe! Clusters of galaxies are grouped together in superclusters! Superclusters occur in filaments and sheets! Large voids of nothing between them
19 Next Time The Dawn of Time
Hubble s Law. Tully-Fisher relation. The redshift. λ λ0. Are there other ways to estimate distances? Yes.
Distances to galaxies Cepheids used by Hubble, 1924 to show that spiral nebulae like M31 were further from the Sun than any part of the Milky Way, therefore galaxies in their own right. Review of Cepheids
More informationLecture 32: The Expanding Universe Readings: Sections 26-5 and 28-2
Lecture 32: The Expanding Universe Readings: Sections 26-5 and 28-2 Key Ideas Measuring the Distances to Galaxies and Determining the Scale of the Universe Distance Methods: Trigonometric Parallaxes Spectroscopic
More informationThe Cosmic Distance Ladder
The Cosmic Distance Ladder (Mário Santos) What is it? A way to calculate distances to objects very far away based on the measured distances to nearby objects: 1. Start with the distance to the Sun (1 AU)
More informationCosmic Distance Determinations
Cosmic Distance Determinations Radar (works for inner solar system) Parallax D(pc) = 1 p(arcsec) GAIA satellite (2013) 20 micro-arcsec resolution! Thus D < 10 kpc Beyond Parallax: Standard Candles Use
More informationThe Cosmological Redshift. Cepheid Variables. Hubble s Diagram
SOME NEGATIVE EFFECTS OF THE EXPANSION OF THE UNIVERSE. Lecture 22 Hubble s Law and the Large Scale Structure of the Universe PRS: According to modern ideas and observations, what can be said about the
More informationThe Cosmic Distance Ladder. Hubble s Law and the Expansion of the Universe!
The Cosmic Distance Ladder Hubble s Law and the Expansion of the Universe! Last time: looked at Cepheid Variable stars as standard candles. Massive, off-main sequence stars: at a certain stage between
More informationAstronomy 102 Lab: Distances to Galaxies
Name: Astronomy 102 Lab: Distances to Galaxies You will access your textbook for this lab. Pre-Lab Assignment: As we began to talk about stars beyond the Sun, one of the most important pieces of information
More informationBig Galaxies Are Rare! Cepheid Distance Measurement. Clusters of Galaxies. The Nature of Galaxies
Big Galaxies Are Rare! Potato Chip Rule: More small things than large things Big, bright spirals are easy to see, but least common Dwarf ellipticals & irregulars are most common Faint, hard to see Mostly
More informationPHY 475/375. Lecture 2. (March 28, 2012) The Scale of the Universe: The Shapley-Curtis Debate
PHY 475/375 Lecture 2 (March 28, 2012) The Scale of the Universe: The Shapley-Curtis Debate By the 1920 s a debate had developed over whether some of the spiral nebulae catalogued in the 18th century by
More informationGalaxies & Introduction to Cosmology
Galaxies & Introduction to Cosmology Other Galaxies: How many are there? Hubble Deep Field Project 100 hour exposures over 10 days Covered an area of the sky about 1/100 the size of the full moon Probably
More informationGalaxies. The majority of known galaxies fall into one of three major classes: spirals (78 %), ellipticals (18 %) and irregulars (4 %).
Galaxies Collection of stars, gas and dust bound together by their common gravitational pull. Galaxies range from 10,000 to 200,000 light-years in size. 1781 Charles Messier 1923 Edwin Hubble The distribution
More informationAST 101 General Astronomy: Stars & Galaxies
Summary Distance Ladder to measure universe REVIEW AST 101 General Astronomy: Stars & Galaxies Different standard candles are useful for different distances Distance measurements allowed to make a MAJOR
More informationA 103 Notes, Week 14, Kaufmann-Comins Chapter 15
NEARBY GALAXIES I. Brief History A 103 Notes, Week 14, Kaufmann-Comins Chapter 15 A. Kant B. Curtis-Shapley debate C. Distance to Andromeda II. Classification of nearby galaxies: Spirals, Ellipticals,
More informationThe Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds.
The Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds. Image taken from the European Southern Observatory in Chile
More informationLecture Outlines. Chapter 24. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 24 Astronomy Today 8th Edition Chaisson/McMillan Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble
More informationGalaxies and Cosmology
Galaxies and Cosmology Attendance Quiz Are you here today? (a) yes (b) no Here! (c) Cosmetology? Like hair and nails and makeup? Next Tuesday, 5/30: Dr. Jorge Moreno is unavailable, so class will be cancelled
More information11/9/2010. Stars, Galaxies & the Universe Announcements. Sky & Telescope s Week at a Glance. iphone App available now.
Stars, Galaxies & the Universe Announcements Reading Quiz #11 Wednesday Mix of questions from today s lecture & reading for Wed. on active galaxies HW#10 in ICON due Friday (11/12) by 5 pm - available
More informationAddition to the Lecture on Galactic Evolution
Addition to the Lecture on Galactic Evolution Rapid Encounters In case the encounter of two galaxies is quite fast, there will be not much dynamical friction due to lack of the density enhancement The
More informationV. M. Slipher ( ) was an astronomer who worked at Lowell Observatory in Flagstaff, Arizona. In 1909 he began studying the spectrum of the
Hubble s Law V. M. Slipher (1875-1969) was an astronomer who worked at Lowell Observatory in Flagstaff, Arizona. In 1909 he began studying the spectrum of the Andromeda Nebula. He found that that object
More informationChapter 15 2/19/2014. Lecture Outline Hubble s Galaxy Classification. Normal and Active Galaxies Hubble s Galaxy Classification
Lecture Outline Chapter 15 Normal and Active Galaxies Spiral galaxies are classified according to the size of their central bulge. Chapter 15 Normal and Active Galaxies Type Sa has the largest central
More informationThe Discovery of Other Galaxies. 24. Normal Galaxies
24. Normal Galaxies The discovery of other galaxies Edwin Hubble proved galaxies are very distant Edwin Hubble classified galaxies by shape Methods for determining distances to galaxies The Hubble Law
More informationThe Extragalactic Distance Scale
One of the important relations in Astronomy. It lets us Measure the distance to distance objects. Each rung on the ladder is calibrated using lower-rung calibrations. Distance Objects Technique 1-100 AU
More informationTA Final Review. Class Announcements. Objectives Today. Compare True and Apparent brightness. Finding Distances with Cepheids
Class Announcements Vocab Quiz 4 deadline is Saturday Midterm 4 has started, ends Monday Lab was in the Planetarium. You still need to do the 2 questions Check PS100 webpage, make sure your clicker is
More information24.1 Hubble s Galaxy Classification
Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble s Law 24.4 XXActive Galactic Nuclei XXRelativistic Redshifts and Look-Back
More informationRevision Guide for Chapter 12
Revision Guide for Chapter 12 Contents Student s Checklist Revision Notes The speed of light... 4 Doppler effect... 4 Expansion of the Universe... 5 Microwave background radiation... 5 Galaxy... 6 Summary
More informationNormal Galaxies (Ch. 24) + Galaxies and Dark Matter (Ch. 25) Symbolically: E0.E7.. S0..Sa..Sb..Sc..Sd..Irr
Normal Galaxies (Ch. 24) + Galaxies and Dark Matter (Ch. 25) Here we will cover topics in Ch. 24 up to 24.4, but then skip 24.4, 24.5 and proceed to 25.1, 25.2, 25.3. Then, if there is time remaining,
More informationChapter 20 Lecture. The Cosmic Perspective Seventh Edition. Galaxies and the Foundation of Modern Cosmology Pearson Education, Inc.
Chapter 20 Lecture The Cosmic Perspective Seventh Edition Galaxies and the Foundation of Modern Cosmology Galaxies and the Foundation of Modern Cosmology 20.1 Islands of Stars Our goals for learning: How
More informationThe Extragalactic Distance Scale
One of the important relations in Astronomy. It lets us Measure the distance to distance objects. Each rung on the ladder is calibrated using lower-rung calibrations. Distance Objects Technique 1-100 AU
More informationThere are three basic types of galaxies:
Galaxies There are three basic types of galaxies: Spirals Ellipticals Irregulars To make a long story short, elliptical galaxies are galaxies that have used up all their gas forming stars, or they have
More informationASTRONOMY 2 Overview of the Universe Second Practice Problem Set Solutions
ASTRONOMY 2 Overview of the Universe Second Practice Problem Set Solutions 1. Consider a 2 M neutron star. The mass of a neutron is 1.67 10 24 g, and 1 M = 2 10 33 g. (i) How many neutrons are in this
More informationGalaxies. Hubbleʼs Law. Author: Sarah Roberts
Galaxies Hubbleʼs Law Author: Sarah Roberts Hubbleʼs Law Introduction The first galaxies were identified in the 17th Century by the French astronomer Charles Messier, although at the time he did not know
More informationGalaxies. Galaxy Diversity. Galaxies, AGN and Quasars. Physics 113 Goderya
Galaxies, AGN and Quasars Physics 113 Goderya Chapter(s): 16 and 17 Learning Outcomes: Galaxies Star systems like our Milky Way Contain a few thousand to tens of billions of stars. Large variety of shapes
More informationChapter 20 Lecture. The Cosmic Perspective. Seventh Edition. Galaxies and the Foundation of Modern Cosmology Pearson Education, Inc.
Chapter 20 Lecture The Cosmic Perspective Seventh Edition Galaxies and the Foundation of Modern Cosmology 20.1 Islands of Stars Our goals for learning: How do galaxies evolve? What are the three major
More informationThe Milky Way. Finding the Center. Milky Way Composite Photo. Finding the Center. Milky Way : A band of and a. Milky Way
The Milky Way Milky Way : A band of and a The band of light we see is really 100 billion stars Milky Way probably looks like Andromeda. Milky Way Composite Photo Milky Way Before the 1920 s, astronomers
More informationASTR 1040: Stars & Galaxies
ASTR 1040: Stars & Galaxies Our wide world (universe) of Galaxies Expanding universe: Hubble s discovery #2 Challenge of measuring s in universe review methods used Subtle concept of Lookback time Active
More informationGalaxies and Cosmology
4/28/17 The Discovery of Galaxies Up to the 1920 s, astronomers were not sure exactly how far away galaxies were, and thus didn t know how big they are! Spiral Nebulae could be assumed to be inside our
More informationTHE EXPANSION RATE AND AGE OF THE UNIVERSE
THE EXPANSION RATE AND AGE OF THE UNIVERSE I. Introduction: The visible Universe contains about 100 billion galaxies of several different types. The oldest galaxies are the elliptical galaxies, which show
More informationLecture 14: Other Galaxies A2020 Prof. Tom Megeath. The Milky Way in the Infrared 3/17/10. NGC 7331: the Milky Way s Twins. Spiral Galaxy bulge halo
Lecture 14: Other Galaxies A2020 Prof. Tom Megeath Our Galaxy: Side View We see our galaxy edge-on Primary features: Disk: young and old stars where we live. Bulge: older stars Halo: oldest stars, globular
More informationHow Did the Universe Begin?
How Did the Universe Begin? As we will discuss in this lecture, it looks like the Universe started about 14 billion years ago and has been expanding (space stretching) ever since. The model of what happened
More informationXII. The distance scale. h"p://sgoodwin.staff.shef.ac.uk/phy111.html
XII. The distance scale h"p://sgoodwin.staff.shef.ac.uk/phy111.html 0. How far away are galaxies? We discussed galaxies without thinking about how we know the distances to these galaxies. Only in the past
More informationComplete Cosmos Chapter 23: Infinity Outline Sub-chapters
Complete Cosmos Chapter 23: Infinity The structure of the Universe - galaxies, clusters, strands. How we measure to a nearby galaxy and to the farthest quasar. Outline In the Australian night sky, the
More informationFigure 19.19: HST photo called Hubble Deep Field.
19.3 Galaxies and the Universe Early civilizations thought that Earth was the center of the universe. In the sixteenth century, we became aware that Earth is a small planet orbiting a medium-sized star.
More information4/10/18. Our wide world (universe) of Galaxies. Spirals ~80% of galaxies
ASTR 1040: Stars & Galaxies Prof. Juri Toomre TAs: Peri Johnson, Ryan Horton Lecture 23 Tues 10 Apr 2018 zeus.colorado.edu/astr1040-toomre Our wide world (universe) of Galaxies The rich range of galaxies:
More informationGalaxies and Hubble s Law
Galaxies and Hubble s Law Some Important History: Charles Messier In the early 19 th century, Charles Messier was hunting for comets, but in the telescopes of the time, identifying comets was difficult
More informationToday s Topics & Events
ASTR 1120: Stars & Galaxies Prof. Juri Toomre TA: Licia Ray Lecture 34 Wed 7 Apr 04 zeus.colorado.edu/astr1120-toomre toomre NGC 1232 Today s Topics & Events Today we look at the challenge of measuring
More informationObserving the Night Sky. Observing the Night Sky. Observing the Night Sky. Observing the Night Sky. Observing the Night Sky. Chapter 29 THE UNIVERSE
Hewitt/Lyons/Suchocki/Yeh Conceptual Integrated Science Constellations are groups of stars named over antiquity. A familiar constellation is Ursa Major, the Great Bear. Chapter 29 THE UNIVERSE The monthly
More information2. Can observe radio waves from the nucleus see a strong radio source there Sagittarius A* or Sgr A*.
7/7 The Nucleus of the MW its center 1. Can t see the nucleus in visible light too much stuff in the way. 2. Can observe radio waves from the nucleus see a strong radio source there Sagittarius A* or Sgr
More informationThe Cosmological Distance Ladder. It's not perfect, but it works!
The Cosmological Distance Ladder It's not perfect, but it works! First, we must know how big the Earth is. Next, we must determine the scale of the solar system. Copernicus (1543) correctly determined
More informationASTRONOMY QUIZ NUMBER 11
ASTRONOMY QUIZ NUMBER. Suppose you measure the parallax of a star and find 0. arsecond. The distance to this star is A) 0 light-years B) 0 parsecs C) 0. light-year D) 0. parsec 2. A star is moving toward
More informationGalaxies and the expansion of the Universe
Review of Chapters 14, 15, 16 Galaxies and the expansion of the Universe 5/4/2009 Habbal Astro 110-01 Review Lecture 36 1 Recap: Learning from Light How does light tell us what things are made of? Every
More information1. This question is about Hubble s law. The light received from many distant galaxies is red-shifted. (a) State the cause of this red-shift (1)
ROUND 2 - QUESTIONS 1. This question is about Hubble s law. The light received from many distant galaxies is red-shifted. (a) State the cause of this red-shift (1) expanding universe (b) State Hubble s
More informationHow do we measure properties of a star? Today. Some Clicker Questions - #1. Some Clicker Questions - #1
Today Announcements: HW#8 due Friday 4/9 at 8:00 am. The size of the Universe (It s expanding!) The Big Bang Video on the Big Bang NOTE: I will take several questions on exam 3 and the final from the videos
More informationChapter 25 (and end of 24): Lecture Notes
Chapter 25 (and end of 24): Lecture Notes In order to understand the Hubble Law and its implications both for estimating distances and for interpreting the evolution of the universe, you have to be comfortable
More informationPrelab Questions for Hubble Expansion Lab. 1. Why does the pitch of a firetruck s siren change as it speeds past you?
AST 114 Spring 2011 NAME: Prelab Questions for Lab 1. Why does the pitch of a firetruck s siren change as it speeds past you? 2. What color light has a longer wavelength blue or red? 3. What are the typical
More informationSurvey of Astrophysics A110
Goals: Galaxies To determine the types and distributions of galaxies? How do we measure the mass of galaxies and what comprises this mass? How do we measure distances to galaxies and what does this tell
More informationPrelab 9: The Hubble Redshift Distance Relation
Name: Section: Date: Prelab 9: The Hubble Redshift Distance Relation The Doppler Effect: When objects are moving, the frequency or pitch of waves can change. Think of the noise a car makes when you are
More informationLecture 22: The expanding Universe. Astronomy 111 Wednesday November 15, 2017
Lecture 22: The expanding Universe Astronomy 111 Wednesday November 15, 2017 Reminders Online homework #10 due Monday at 3pm Then one week off from homeworks Homework #11 is the last one The nature of
More informationThe Scale of the Universe
The Scale of the Universe The Measurement of distance in our Univers! Chapters 12.1.1 Allday; Chapter 3 Silk Measurement of Distance in the Universe Two IMPORTANT concepts that you should know well from
More informationCHAPTER 28 STARS AND GALAXIES
CHAPTER 28 STARS AND GALAXIES 28.1 A CLOSER LOOK AT LIGHT Light is a form of electromagnetic radiation, which is energy that travels in waves. Waves of energy travel at 300,000 km/sec (speed of light Ex:
More informationThe Milky Way Galaxy (ch. 23)
The Milky Way Galaxy (ch. 23) [Exceptions: We won t discuss sec. 23.7 (Galactic Center) much in class, but read it there will probably be a question or a few on it. In following lecture outline, numbers
More informationLESSON 1. Solar System
Astronomy Notes LESSON 1 Solar System 11.1 Structure of the Solar System axis of rotation period of rotation period of revolution ellipse astronomical unit What is the solar system? 11.1 Structure of the
More informationM31 - Andromeda Galaxy M110 M32
UNIT 4 - Galaxies XIV. The Milky Way galaxy - a huge collection of millions or billions of stars, gas, and dust, isolated in space and held together by its own gravity M110 M31 - Andromeda Galaxy A. Structure
More informationA100 Exploring the Universe: Measuring the Universe. Martin D. Weinberg UMass Astronomy
A100 Exploring the : Measuring the Martin D. Weinberg UMass Astronomy weinberg@astro.umass.edu November 18, 2014 Read: Chaps 20, 21 11/18/14 slide 1 Age of the in an Exam #2 scores posted in Mastering.
More informationStar systems like our Milky Way. Galaxies
Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in
More informationTuesday, Thursday 2:30-3:45 pm. Astronomy 100. Tom Burbine
Astronomy 100 Tuesday, Thursday 2:30-3:45 pm Tom Burbine tburbine@mtholyoke.edu www.xanga.com/astronomy100 OWL assignment (Due Today) There is be an OWL assignment due on Thursday April 14 at 11:59 pm.
More information5. A particular star has an angle of parallax of 0.2 arcsecond. What is the distance to this star? A) 50 pc B) 2 pc C) 5 pc D) 0.
Name: Date: 1. How far away is the nearest star beyond the Sun, in parsecs? A) between 1 and 2 pc B) about 12 pc C) about 4 pc D) between 1/2 and 1 pc 2. Parallax of a nearby star is used to estimate its
More informationThis Week in Astronomy
Homework #8 Due Wednesday, April 18, 11:59PM Covers Chapters 15 and 16 Estimated time to complete: 40 minutes Read chapters, review notes before starting This Week in Astronomy Credit: NASA/JPL-Caltech
More informationWhat is the solar system?
Notes Astronomy What is the solar system? 11.1 Structure of the Solar System Our solar system includes planets and dwarf planets, their moons, a star called the Sun, asteroids and comets. Planets, dwarf
More information- M31) Biggest is Andromeda (Sb. On Galaxy Evolution Lane. Large & Small Magellanic Clouds. ASTR 1040 Accel Astro: Stars & Galaxies
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nicholas Nelson Lecture 24 Thur 7 Apr 2011 zeus.colorado.edu/astr1040-toomre toomre Stefan s Quintet On Galaxy Evolution Lane Look at our local
More information29:50 Stars, Galaxies, and the Universe Final Exam December 13, 2010 Form A
29:50 Stars, Galaxies, and the Universe Final Exam December 13, 2010 Form A There are 40 questions. Read each question and all of the choices before choosing. Budget your time. No whining. Walk with Ursus!
More informationGalaxies. With a touch of cosmology
Galaxies With a touch of cosmology Types of Galaxies Spiral Elliptical Irregular Spiral Galaxies Spiral Galaxies Disk component where the spiral arms are Interstellar medium Star formation Spheroidal
More informationGalaxies Guiding Questions
Galaxies Guiding Questions How did astronomers first discover other galaxies? How did astronomers first determine the distances to galaxies? Do all galaxies have spiral arms, like the Milky Way? How do
More information2011 Arizona State University Page 1 of 6
AST 114 Spring 2017 NAME: HUBBLE EXPANSION What will you learn in this Lab? In this lab, you will reproduce the 20 th century discovery by Edwin Hubble that the Universe is expanding. You will determine
More informationThe Doppler Effect is the change in frequency observed when a source of sound waves is moving relative to an observer.
Doppler Effect The Doppler Effect is the change in frequency observed when a source of sound waves is moving relative to an observer. Examples of the Doppler effect are: Hearing an increase in a car horn
More informationChapter 8: The Family of Stars
Chapter 8: The Family of Stars Motivation We already know how to determine a star s surface temperature chemical composition surface density In this chapter, we will learn how we can determine its distance
More informationLecture Outlines. Chapter 25. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 25 Astronomy Today 7th Edition Chaisson/McMillan Chapter 25 Galaxies and Dark Matter Units of Chapter 25 25.1 Dark Matter in the Universe 25.2 Galaxy Collisions 25.3 Galaxy Formation
More informationBeyond Our Solar System Chapter 24
Beyond Our Solar System Chapter 24 PROPERTIES OF STARS Distance Measuring a star's distance can be very difficult Stellar parallax Used for measuring distance to a star Apparent shift in a star's position
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 informationExam 3 Astronomy 100, Section 3. Some Equations You Might Need
Exam 3 Astronomy 100, Section 3 Some Equations You Might Need modified Kepler s law: M = [a(au)]3 [p(yr)] (a is radius of the orbit, p is the rotation period. You 2 should also remember that the period
More informationStars & Galaxies. Chapter 27 Modern Earth Science
Stars & Galaxies Chapter 27 Modern Earth Science Chapter 27, Section 1 27.1 Characteristics of Stars How do astronomers determine the composition and surface temperature of a star? Composition & Temperature
More informationBROCK UNIVERSITY. Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015
BROCK UNIVERSITY Page 1 of 9 Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015 Number of hours: 50 min Time of Examination: 18:00 18:50
More informationCOSMOLOGY PHYS 30392 OBSERVING THE UNIVERSE Part I Giampaolo Pisano - Jodrell Bank Centre for Astrophysics The University of Manchester - January 2013 http://www.jb.man.ac.uk/~gp/ giampaolo.pisano@manchester.ac.uk
More informationHubble s Law: Finding the Age of the Universe
Lab 16 Name: Hubble s Law: Finding the Age of the Universe 16.1 Introduction In your lecture sessions (or the lab on spectroscopy), you will find out that an object s spectrum can be used to determine
More informationChapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc.
Chapter 23 Lecture The Cosmic Perspective Seventh Edition Dark Matter, Dark Energy, and the Fate of the Universe Curvature of the Universe The Density Parameter of the Universe Ω 0 is defined as the ratio
More informationIsland Universes. Up to 1920 s, many thought that Milky Way encompassed entire universe.
Island Universes Up to 1920 s, many thought that Milky Way encompassed entire universe. Observed three types of nebulas (clouds): - diffuse, spiral, elliptical - many were faint, indistinct - originally
More informationThe King's University College Astronomy 201 Mid-Term Exam Solutions
The King's University College Astronomy 201 Mid-Term Exam Solutions Instructions: The exam consists of two sections. Part A is 20 multiple choice questions - please record answers on the sheet provided.
More informationIt is about 100,000 ly across, 2,000 ly thick, and our solar system is located 26,000 ly away from the center of the galaxy.
The Galaxies The Milky Way Galaxy Is a spiral galaxy in which our solar system is located. The center of the galaxy lies in the Sagittarius Constellation. It is about 100,000 ly across, 2,000 ly thick,
More informationHubble s Law and the Cosmic Distance Scale
Lab 7 Hubble s Law and the Cosmic Distance Scale 7.1 Overview Exercise seven is our first extragalactic exercise, highlighting the immense scale of the Universe. It addresses the challenge of determining
More informationExam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti
Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti INSTRUCTIONS: Please, use the `bubble sheet and a pencil # 2 to answer the exam questions, by marking
More informationHUBBLE SPACE TELESCOPE
ASTRO 202 Age of the Universe Tuesday February 19, 2008 STARS: How and where do they form? From clouds of dust and gas primarily hydrogen -in our galaxy and other galaxies Part of the Orion nebula (Hubble
More informationStars & Galaxies. Chapter 27, Section 1. Composition & Temperature. Chapter 27 Modern Earth Science Characteristics of Stars
Stars & Galaxies Chapter 27 Modern Earth Science Chapter 27, Section 1 27.1 Characteristics of Stars Composition & Temperature Scientists use the following tools to study stars Telescope Observation Spectral
More informationChapter 20 Galaxies and the Foundation of Modern Cosmology Pearson Education, Inc.
Chapter 20 Galaxies and the Foundation of Modern Cosmology 20.1 Islands of Stars Our goals for learning: How are the lives of galaxies connected with the history of the universe? What are the three major
More informationAstronomy 114. Lecture35:TheBigBang. Martin D. Weinberg. UMass/Astronomy Department
Astronomy 114 Lecture35:TheBigBang Martin D. Weinberg weinberg@astro.umass.edu UMass/Astronomy Department A114: Lecture 35 09 May 2005 Read: Ch. 28,29 Astronomy 114 1/18 Announcements PS#8 due Monday!
More informationBROCK UNIVERSITY. Test 2, March 2018 Number of pages: 9 Course: ASTR 1P02, Section 1 Number of Students: 465 Date of Examination: March 12, 2018
BROCK UNIVERSITY Page 1 of 9 Test 2, March 2018 Number of pages: 9 Course: ASTR 1P02, Section 1 Number of Students: 465 Date of Examination: March 12, 2018 Number of hours: 50 min Time of Examination:
More informationLecture 25: The Cosmic Distance Scale Sections 25-1, 26-4 and Box 26-1
Lecture 25: The Cosmic Distance Scale Sections 25-1, 26-4 and Box 26-1 Key Ideas The Distance Problem Geometric Distances Trigonometric Parallaxes Luminosity Distances Standard Candles Spectroscopic Parallaxes
More informationQuasars: Back to the Infant Universe
Quasars: Back to the Infant Universe Learning Objectives! What is a quasar? What spectral features tell us quasars are very redshifted (very distant)? What spectral features tell us they are composed of
More informationLecture 16 The Measuring the Stars 3/26/2018
Lecture 16 The Measuring the Stars 3/26/2018 Test 2 Results D C B A Questions that I thought were unfair: 13, 18, 25, 76, 77, 80 Curved from 85 to 79 Measuring stars How far away are they? How bright are
More informationAccording to the currents models of stellar life cycle, our sun will eventually become a. Chapter 34: Cosmology. Cosmology: How the Universe Works
Chapter 34: Cosmology According to the currents models of stellar life cycle, our sun will eventually become a a) Cloud of hydrogen gas b) Protostar c) Neutron star d) Black hole e) White dwarf id you
More informationName Date Period. 10. convection zone 11. radiation zone 12. core
240 points CHAPTER 29 STARS SECTION 29.1 The Sun (40 points this page) In your textbook, read about the properties of the Sun and the Sun s atmosphere. Use each of the terms below just once to complete
More information