Cosmology. Clusters of galaxies. Redshift. Late 1920 s: Hubble plots distances versus velocities of galaxies. λ λ. redshift =
|
|
- Gabriel Payne
- 6 years ago
- Views:
Transcription
1 Cosmology Study of the structure and origin of the universe Observational science The large-scale distribution of galaxies Looking out to extremely large distances The motions of galaxies Clusters of galaxies Galaxy - huge group of stars, dust, gas, and other celestial bodies bound together by gravitational forces. Single galaxies (field galaxies): less than 8 % of total number of galaxies Groups of galaxies - the smallest aggregates of galaxies (N=10 to 100 members in a diameter of 2 Mpc) Cluster of galaxies - contain up to one thousand galaxies (N=10 2 to 10 3 ) Superclusters of galaxies - contain up to thousands of galaxies (N=10 3 to 10 4 ) Enormous clouds of extremely hot intergalactic gas and Dark matter Average distance between clusters r ~(10 x Cluster s Diameter ) -- much larger spatial concentration in comparison to the concentration of stars in a given galaxy ( r between stars = 10 5 to 10 6 x D star ) The known part of the Universe - to a distance of ~ 4000 Mpc 1 2 Redshift in spectra of galaxies Redshift shifted wavelength real wavelength speed of object = speed of light real wavelength shifted wavelength real wavelength redshift = real wavelength λ λ 0 z = λ v = zc 0 Late 1920 s: Hubble plots distances versus velocities of galaxies 1
2 Implications of the Hubble s Law Space between galaxies is expanding uniformly - the universe itself is expanding - the further away a galaxy is from us the higher the recession velocity Even though the galaxies appear to be moving away from us, we are not at the centre of the universe an observer in a distant galaxy would see the same effect Cosmological principle: the universe is homogeneous and isotropic no preferred places and directions Distance and Velocity (away) are related! v = H x D What exactly is expanding? Ordinary things are not expanding The expansion is noticeable only at fairly large separations The cosmological redshift means expansion of space Therefore, the redshift of distant galaxies is not because they speed up away from us, but because the Universe expands The Big Bang and the expansion age of the Universe Everything was located very close together in the past, Universe was very dense and hot about 14 billion years ago The expansion began with the Big Bang expansion of space the universe is expanding everywhere we look: there is no special location in the universe where the Big Bang originated the Universe has no centre How long a galaxy has been traveling: t=d / v t=d/(hd) t=1/h Hubble time one Hubble time ago all of the matter of the Universe was located Cosmological redshift together - estimation of the expansion age of the Universe light waves stretch as space expands 8 2
3 The Big Bang Tremendous explosion (filling all of space with all of the particles ) We can t see radiation produced during the first yrs Enormous increase of scale during a very short time in the early universe (inflation model) yrs after BB universe had cooled to about 3000 billion degrees Kelvin The universe became transparent for the radiation isotropic cosmic background radiation 9 Tests of Big Bang Theory The Universe at high redshifts galaxies look more irregular, different star-formation rate; galaxy interactions; quasars The expansion of the universe Galaxies are generally receding from each other The abundance of the light elements H and He observations agree with amounts of H and He from the Big Bang theory The cosmic microwave background (CMB) radiation The cosmic microwave background radiation is the remnant heat leftover from the early universe. 10 Galaxy Cluster in the Early Universe The cosmic microwave background (CMB) radiation 11 3
4 Satellite missions detected fluctuations in the microwave background: COBE (1989) and WMAP (2001) Will The Universe Expand Forever? The universe is currently expanding 2001, NASA s -- Wilkinson Microwave Anisotropy Probe Universe will expand forever: unbound universe Stars will consume their hydrogen and die. Universe will become a black, cold, empty space Universe might eventually stop expanding and begin to collapse: bound universe All objects and atoms will be compressed to higher and higher densities: Big Crunch Any alternatives? The expansion will stop after time = infinity 14 Expansion forever or collapse? Expansion forever or collapse? Factors affecting the expansion or collapse The Big Bang began the expansion of the Universe The gravitational force between galaxies has slowed the expansion Relative strength of these two effects expansion energy vs. gravitational energy Total energy = positive energy of expansion +negative gravitational binding energy 15 A sketch of how gravity and the energy of expansion determine the behavior of the Universe. 16 4
5 The fate of the Universe Not enough information about the parameters of the Universe Cosmological models: the fate depends on average density Critical density 3H 2 / 8πG = 8.3 x g/cm 3 Ω = actual density / critical density Ω = 0, the universe is empty, will expand forever Ω > 1, the universe will recollapse, bound universe Ω < 1, the universe will expand forever, unbound universe Ω = 1, still unbound universe 17 Fading light of the cosmic explosion that gave birth to our universe Radiation we receive now when the universe was one thousandth of its current size Cosmic Microwave Background 18 The makeup of the universe The fate of the Universe Deduced from observations of the brightness variations in the CMB
6 The Universe Flat or Curved? (Geometry) Bound or Unbound? Finite or Infinite? Closed or Open? (Shape or Evolution) Density of matter geometry of space The shape of the universe is determined by a struggle between the momentum of expansion and the pull of gravity Geometry of the Universe Geometry: Positively curved Closed space; finite Universe; Ω > 1 (Big Crunch) Negatively curved Open space; infinite Universe; Ω < 1 (expands forever) Flat Open space, infinite Universe; Ω = Geometry of Universe 2001, NASA s -- Wilkinson Microwave Anisotropy Probe What created the galactic clusters? Primordial ripples in density created the large-scale structure that we observe now
7 Fig Other Superclusters Superclusters Virgo Coma Centaurus Large Sheets of Galaxies Great Wall Perseus-Pisces Great Wall Voids Great Wall Large single structure Dimensions are about 600x250x30 million light years Giant quilt of galaxies across the sky The fate of the Universe Not enough information about the parameters of the Universe Cosmological models: the fate depends on average density 3H 2 / 8πG = 8.3 x g/cm 3 Ω = actual density / critical density Ω = 0, the universe is empty, will expand forever Ω > 1, the universe will recollapse, bound universe Ω < 1, the universe will expand forever, unbound universe Ω = 1, still unbound universe 26 Obtaining the mass of clusters of galaxies HST Image of a gravitational lens Geometry of Universe 2001, NASA s -- Wilkinson Microwave Anisotropy Probe
8 The fate of the Universe 29 8
Implications of the Hubble Law: - it is not static, unchanging - Universe had a beginning!! - could not have been expanding forever HUBBLE LAW:
Cosmology and the Evolution of the Universe Edwin Hubble, 1929: -almost all galaxies have a redshift -moving away from us -greater distance greater redshift Implications of the Hubble Law: - Universe is
More informationCosmology and the Evolution of the Universe. Implications of the Hubble Law: - Universe is changing (getting bigger!) - it is not static, unchanging
Cosmology and the Evolution of the Edwin Hubble, 1929: -almost all galaxies have a redshift -moving away from us -exceptions in Local Group -with distance measurements - found a relationship greater distance
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 informationLecture 37 Cosmology [not on exam] January 16b, 2014
1 Lecture 37 Cosmology [not on exam] January 16b, 2014 2 Structure of the Universe Does clustering of galaxies go on forever? Looked at very narrow regions of space to far distances. On large scales the
More informationThe Big Bang Theory was first proposed in the late 1920 s. This singularity was incredibly dense and hot.
The Big Bang Theory was first proposed in the late 1920 s. It states that there was an infinitely small, infinitely dense point that contained everything that is the universe. This singularity was incredibly
More informationHomework 6 Name: Due Date: June 9, 2008
Homework 6 Name: Due Date: June 9, 2008 1. Where in the universe does the general expansion occur? A) everywhere in the universe, including our local space upon Earth, the solar system, our galaxy and
More informationFormation of the Universe. What evidence supports current scientific theory?
Formation of the Universe What evidence supports current scientific theory? Cosmology Cosmology is the study of the Nature, Structure, Origin, And fate of the universe. How did it all begin? Astronomers
More informationChapter 21 Evidence of the Big Bang. Expansion of the Universe. Big Bang Theory. Age of the Universe. Hubble s Law. Hubble s Law
Chapter 21 Evidence of the Big Bang Hubble s Law Universal recession: Slipher (1912) and Hubble found that all galaxies seem to be moving away from us: the greater the distance, the higher the redshift
More informationEnergy Source for Active Galactic Nuclei
Quasars Quasars are small, extremely luminous, extremely distant galactic nuclei Bright radio sources Name comes from Quasi-Stellar Radio Source, as they appeared to be stars! Can have clouds of gas near
More informationCOSMOLOGY The Universe what is its age and origin?
COSMOLOGY The Universe what is its age and origin? REVIEW (SUMMARY) Oppenheimer Volkhoff limit: upper limit to mass of neutron star remnant more than 1.4 M à neutron degeneracy Supernova à extremely dense
More informationCosmology: The History of the Universe
Cosmology: The History of the Universe The Universe originated in an explosion called the Big Bang. Everything started out 13.7 billion years ago with zero size and infinite temperature. Since then, it
More information3. It is expanding: the galaxies are moving apart, accelerating slightly The mystery of Dark Energy
II. Cosmology: How the universe developed Outstanding features of the universe today: 1. It is big, and full of galaxies. 2. It has structure: the galaxies are clumped in filaments and sheets The structure
More informationIf there is an edge to the universe, we should be able to see our way out of the woods. Olber s Paradox. This is called Olber s Paradox
Suppose the Universe were not expanding, but was in some kind of steady state. How should galaxy recession velocities correlate with distance? They should a) be directly proportional to distance. b) reverse
More informationAstronomy 162, Week 10 Cosmology Patrick S. Osmer Spring, 2006
Astronomy 162, Week 10 Cosmology Patrick S. Osmer Spring, 2006 Information Makeup quiz Wednesday, May 31, 5-6PM, Planetarium Review Session, Monday, June 5 6PM, Planetarium Cosmology Study of the universe
More informationThe Cosmic Microwave Background
The Cosmic Microwave Background The Cosmic Microwave Background Key Concepts 1) The universe is filled with a Cosmic Microwave Background (CMB). 2) The microwave radiation that fills the universe is nearly
More informationExpanding Universe. 1) Hubble s Law 2) Expanding Universe 3) Fate of the Universe. Final Exam will be held in Ruby Diamond Auditorium
Expanding Universe November 20, 2002 1) Hubble s Law 2) Expanding Universe 3) Fate of the Universe Final Exam will be held in Ruby Diamond Auditorium NOTE THIS!!! not UPL Dec. 11, 2002 10am-noon Review
More informationTesting the Big Bang Idea
Reading: Chapter 29, Section 29.2-29.6 Third Exam: Tuesday, May 1 12:00-2:00 COURSE EVALUATIONS - please complete these online (recitation and lecture) Last time: Cosmology I - The Age of the & the Big
More informationCosmology. Big Bang and Inflation
Cosmology Big Bang and Inflation What is the Universe? Everything we can know about is part of the universe. Everything we do know about is part of the universe. Everything! The Universe is expanding If
More informationChapter 17 Cosmology
Chapter 17 Cosmology Over one thousand galaxies visible The Universe on the Largest Scales No evidence of structure on a scale larger than 200 Mpc On very large scales, the universe appears to be: Homogenous
More informationThe Expanding Universe
Cosmology Expanding Universe History of the Universe Cosmic Background Radiation The Cosmological Principle Cosmology and General Relativity Dark Matter and Dark Energy Primitive Cosmology If the universe
More informationCH 14 MODERN COSMOLOGY The Study of Nature, origin and evolution of the universe Does the Universe have a center and an edge? What is the evidence
CH 14 MODERN COSMOLOGY The Study of Nature, origin and evolution of the universe Does the Universe have a center and an edge? What is the evidence that the Universe began with a Big Bang? How has the Universe
More informationOlbers Paradox. Lecture 14: Cosmology. Resolutions of Olbers paradox. Cosmic redshift
Lecture 14: Cosmology Olbers paradox Redshift and the expansion of the Universe The Cosmological Principle Ω and the curvature of space The Big Bang model Primordial nucleosynthesis The Cosmic Microwave
More informationThe Dawn of Time - II. A Cosmos is Born
The Dawn of Time - II. A Cosmos is Born Learning Objectives! Why does Olbers paradox show the Universe began?! How does Hubble s Law tell us the age of the Universe? If Hubble s Constant is large, is the
More informationMIT Exploring Black Holes
THE UNIVERSE and Three Examples Alan Guth, MIT MIT 8.224 Exploring Black Holes EINSTEIN'S CONTRIBUTIONS March, 1916: The Foundation of the General Theory of Relativity Feb, 1917: Cosmological Considerations
More information4/29/14. Vital diagram. Our Schedule. Cosmology topics and issues. Cosmological (Big) Redshifts (from expansion of universe)
ASTR 1040: Stars & Galaxies Our Schedule Homework #13 due today Review Set #4 available -- final review on Wed Apr 30 (tomorrow) 5pm-7pm by Ryan Focus on 22.3 Big Bang and Inflation Complete detailed read
More informationChapter 18. Cosmology in the 21 st Century
Chapter 18 Cosmology in the 21 st Century Guidepost This chapter marks a watershed in our study of astronomy. Since Chapter 1, our discussion has focused on learning to understand the universe. Our outward
More informationChapter 25: Galaxy Clusters and the Structure of the Universe
Chapter 25: Galaxy Clusters and the Structure of the Universe Distribution of galaxies Evolution of galaxies Study of distant galaxies Distance derived from redshift Hubble s constant age of the Universe:
More informationFXA ρ 0 = 3(H 0 ) 2. UNIT G485 Module Universe Evolution. Candidates should be able to : age of the universe 1/H 0
1 Candidates should be able to : Explain that the standard (hot big bang) model of the universe implies a finite age for the universe. Select and use the expression : age of the universe 1/H 0 Describe
More informationToday. Course Evaluations Open. Modern Cosmology. The Hot Big Bang. Age & Fate. Density and Geometry. Microwave Background
Today Modern Cosmology The Hot Big Bang Age & Fate Density and Geometry Microwave Background Course Evaluations Open Cosmology The study of the universe as a physical system Historically, people have always
More information26. Cosmology. Significance of a dark night sky. The Universe Is Expanding
26. Cosmology Significance of a dark night sky The Universe is expanding The Big Bang initiated the expanding Universe Microwave radiation evidence of the Big Bang The Universe was initially hot & opaque
More informationLecture #24: Plan. Cosmology. Expansion of the Universe Olber s Paradox Birth of our Universe
Lecture #24: Plan Cosmology Expansion of the Universe Olber s Paradox Birth of our Universe Reminder: Redshifts and the Expansion of the Universe Early 20 th century astronomers noted: Spectra from most
More informationGalaxies 626. Lecture 3: From the CMBR to the first star
Galaxies 626 Lecture 3: From the CMBR to the first star Galaxies 626 Firstly, some very brief cosmology for background and notation: Summary: Foundations of Cosmology 1. Universe is homogenous and isotropic
More informationLecture 20 Cosmology, Inflation, dark matter
The Nature of the Physical World November 19th, 2008 Lecture 20 Cosmology, Inflation, dark matter Arán García-Bellido 1 News Exam 2: good job! Ready for pick up after class or in my office Average: 74/100
More informationThe Big Bang Theory PRESS Chung Wai Man Camus, Wong Lai Yin Rita, Kum Kit Ying Cathy, Yeung Shuet Wah Sarah, Yu Wai Sze Alice
The Big Bang Theory PRESS-2002 Chung Wai Man Camus, Wong Lai Yin Rita, Kum Kit Ying Cathy, Yeung Shuet Wah Sarah, Yu Wai Sze Alice Supervised by: Dr KY Szeto, HKUST Abstract: We did a survey at our current
More informationThe Search for the Complete History of the Cosmos. Neil Turok
The Search for the Complete History of the Cosmos Neil Turok * The Big Bang * Dark Matter and Energy * Precision Tests * A Cyclic Universe? * Future Probes BIG Questions * What are the Laws of Nature?
More informationCosmology: Building the Universe.
Cosmology: Building the Universe. The term has several different meanings. We are interested in physical cosmology - the study of the origin and development of the physical universe, and all the structure
More informationLecture Outlines. Chapter 26. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 26 Astronomy Today 8th Edition Chaisson/McMillan Chapter 26 Cosmology Units of Chapter 26 26.1 The Universe on the Largest Scales 26.2 The Expanding Universe 26.3 The Fate of the
More informationCosmology. Thornton and Rex, Ch. 16
Cosmology Thornton and Rex, Ch. 16 Expansion of the Universe 1923 - Edwin Hubble resolved Andromeda Nebula into separate stars. 1929 - Hubble compared radial velocity versus distance for 18 nearest galaxies.
More informationB. The blue images are a single BACKGROUND galaxy being lensed by the foreground cluster (yellow galaxies)
ASTR 1040 Accel Astro: Stars & Galaxies Today s s `Cosmological Events Look at models for our universe,, and what prompted ideas about big-bang bang beginnings Cosmic Microwave Background Simulation: Large-scale
More informationAstronomy 210 Final. Astronomy: The Big Picture. Outline
Astronomy 210 Final This Class (Lecture 40): The Big Bang Next Class: The end HW #11 Due next Weds. Final is May 10 th. Review session: May 6 th or May 9 th? Designed to be 2 hours long 1 st half is just
More informationCosmology. What is Cosmology?
Cosmology What is Cosmology? The study of the structure and evolution of the entire universe The idea is to form picture of the entire Universe: origin, size, and future We will make assumptions that what
More informationLecture 11. The standard Model
Lecture 11 The standard Model Standard Model The standard model assumes that the universe is filled with matter and other forms of energy (photons) but that matter is dominant today. The standard model
More informationCosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE
Cosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE Cosmology Cosmology is the study of the universe; its nature, origin and evolution. General Relativity is the mathematical basis of cosmology from which
More informationWhat is the evidence that Big Bang really occurred
What is the evidence that Big Bang really occurred Hubble expansion of galaxies Microwave Background Abundance of light elements but perhaps most fundamentally... Darkness of the night sky!! The very darkness
More informationThe best evidence so far in support of the Big Bang theory is:
Notes about the final exam: Saturday May 17th, 7:45 AM-9:45 AM Chamberlain 2103 If you have a CONFLICT email me or Ella before the end of this week. No excuses accepted after exam. Comprehensive, covering
More informationTHE UNIVERSE CHAPTER 20
THE UNIVERSE CHAPTER 20 THE UNIVERSE UNIVERSE everything physical in and Includes all space, matter, and energy that has existed, now exists, and will exist in the future. How did our universe form, how
More informationIntroduction. How did the universe evolve to what it is today?
Cosmology 8 1 Introduction 8 2 Cosmology: science of the universe as a whole How did the universe evolve to what it is today? Based on four basic facts: The universe expands, is isotropic, and is homogeneous.
More informationCosmology. Chapter 18. Cosmology. Observations of the Universe. Observations of the Universe. Motion of Galaxies. Cosmology
Cosmology Chapter 18 Cosmology Cosmology is the study of the structure and evolution of the Universe as a whole How big is the Universe? What shape is it? How old is it? How did it form? What will happen
More informationDoppler Effect. Sound moving TOWARDS. Sound moving AWAY 9/22/2017. Occurs when the source of sound waves moves towards or away
Burkey- ESS QUIZ Thursday At the instant of the Big Bang, all the matter, energy, time, & space in the Universe was condensed into a single, tiny point. We call this Singularity. Doppler Effect Occurs
More informationFinal Exam Study Guide
Final Exam Study Guide Final is Comprehensive! Covers content of the entire course Please be sure to look at the Study Guides for the first three in-class exams All of that material will be on the final
More informationChapter 18. Cosmology. Copyright The McGraw-Hill Companies, Inc. Permission required for reproduction or display.
Chapter 18 Cosmology Copyright The McGraw-Hill Companies, Inc. Permission required for reproduction or display. Cosmology Cosmology is the study of the structure and evolution of the Universe as a whole
More informationClass 5 Cosmology Large-Scale Structure of the Universe What do we see? Big Bang Cosmology What model explains what we see?
Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System
More informationCosmology. Jörn Wilms Department of Physics University of Warwick.
Cosmology Jörn Wilms Department of Physics University of Warwick http://astro.uni-tuebingen.de/~wilms/teach/cosmo Contents 2 Old Cosmology Space and Time Friedmann Equations World Models Modern Cosmology
More informationCosmology: The Origin and Evolution of the Universe Chapter Twenty-Eight. Guiding Questions
Cosmology: The Origin and Evolution of the Universe Chapter Twenty-Eight Guiding Questions 1. What does the darkness of the night sky tell us about the nature of the universe? 2. As the universe expands,
More informationComplete Cosmos Chapter 24: Big Bang, Big Crunch Outline Sub-chapters
Complete Cosmos Chapter 24: Big Bang, Big Crunch Theory of the Big Bang. From that cataclysmic explosion, the Universe continues to expand. But will it stop and reverse? Outline How did the Universe begin?
More informationPlanetarium/Observing: the clock is ticking! Don t forget to fill out your Planetarium/ Observing impression online.
Announcements HW #5 Due Wed, Dec. 10th. Planetarium/Observing: the clock is ticking! Don t forget to fill out your Planetarium/ Observing impression online. NOTE: Planetarium: Large dome you sit inside.
More informationHubble's Law. H o = 71 km/s / Mpc. The further a galaxy is away, the faster it s moving away from us. V = H 0 D. Modern Data.
Cosmology Cosmology is the study of the origin and evolution of the Universe, addressing the grandest issues: How "big" is the Universe? Does it have an "edge"? What is its large-scale structure? How did
More informationASTR 1P02 Test 2, March 2017 Page 1 BROCK UNIVERSITY. Test 2: March 2017 Number of pages: 9 Course: ASTR 1P02, Section 2 Number of students: 1193
ASTR 1P02 Test 2, March 2017 Page 1 BROCK UNIVERSITY Test 2: March 2017 Number of pages: 9 Course: ASTR 1P02, Section 2 Number of students: 1193 Examination date: 4 March 2017 Time limit: 50 min Time of
More informationModeling the Universe A Summary
Modeling the Universe A Summary Questions to Consider 1. What does the darkness of the night sky tell us about the nature of the universe? 2. As the universe expands, what, if anything, is it expanding
More informationChapter 25: Beyond our Solar System The Universe pp
Chapter 25: Beyond our Solar System 25.3 The Universe pp 715-721 The Milky Way Galaxy On a clear and moonless night, away from city lights, you might see a a band of light in the sky. This band is The
More informationCosmology. An Analogy 11/28/2010. Cosmology Study of the origin, evolution and future of the Universe
Cosmology Cosmology Study of the origin, evolution and future of the Universe Obler s Paradox If the Universe is infinite why is the sky dark at night? Newtonian Universe The Universe is infinite and unchanging
More informationLecture 10: Cosmology and the Future of Astronomical Research
Lecture 10: Cosmology and the Future of Astronomical Research 1 ! The study of the Universe " Origin " Evolution " Eventual Fate! Physical Cosmology " Includes studies of large-scale structure and dynamics
More informationKiller Skies. Last time: Hubble s Law Today: Big Bang. HW 11 due next Monday Exam 3, Dec 11. Music: Rocket Man Elton John
Killer Skies HW 11 due next Monday Exam 3, Dec 11 Last time: Hubble s Law Today: Big Bang Music: Rocket Man Elton John 1 Hour Exam 3 Hour Exam 3 Wed, Dec 11th, in class information on course website 40
More informationThe oldest science? One of the most rapidly evolving fields of modern research. Driven by observations and instruments
The oldest science? One of the most rapidly evolving fields of modern research. Driven by observations and instruments Intersection of physics (fundamental laws) and astronomy (contents of the universe)
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 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 informationv = H o d Hubble s Law: Distant galaxies move away fastest Velocity (v) is proportional to Distance (d):
Hubble s Law: Distant galaxies move away fastest Velocity (v) is proportional to Distance (d): v = H o d The Hubble Constant was measured after decades of observation: H 0 = 70 km/s/mpc Velocity (km/s)
More informationModule 3: Astronomy The Universe Topic 1 Content: Cosmology Presentation Notes
Pretend that you have been given the opportunity to travel through time to explore cosmology. Cosmology is the study of how the universe formed and what will happen to it. Watch through your viewport as
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 informationThe Universe. What is it? What is in it? How did it form? How will it end? How do we know?
The Universe What is it? What is in it? How did it form? How will it end? How do we know? What is your place in the Universe? What is the universe? a. The study of the universe its nature, origins, and
More informationDistances to Quasars. Quasars. The Luminosity Puzzle. Seyfert Galaxies. Seyfert galaxies have
Quasars In 1963 Martin Schmidt was trying to understand some unidentified lines in the optical spectra from a star that had a strong radio signal He realized that the lines were Balmer lines that were
More informationBASICS OF COSMOLOGY Astro 2299
BASICS OF COSMOLOGY Astro 2299 We live in a ΛCDM universe that began as a hot big bang (BB) and has flat geometry. It will expand forever. Its properties (laws of physics, fundamental constants) allow
More information8/30/2010. Classifying Stars. Classifying Stars. Classifying Stars
Classifying Stars In the early 1900s, Ejnar Hertzsprung and Henry Russell made some important observations. They noticed that, in general, stars with higher temperatures also have brighter absolute magnitudes.
More informationEl Universo en Expansion. Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004
El Universo en Expansion Juan García-Bellido Inst. Física Teórica UAM Benasque, 12 Julio 2004 5 billion years (you are here) Space is Homogeneous and Isotropic General Relativity An Expanding Universe
More informationAstronomy 113. Dr. Joseph E. Pesce, Ph.D Joseph E. Pesce, Ph.D.
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Big Bang & Matter 17-2 Cosmology ³ The study of the origins, structure, and evolution of the universe ³ Key moments: ² Einstein General Theory of Relativity
More informationAstronomy 113. Dr. Joseph E. Pesce, Ph.D. The Big Bang & Matter. Olber s Paradox. Cosmology. Olber s Paradox. Assumptions 4/20/18
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Big Bang & Matter Cosmology ³The study of the origins, structure, and evolution of the universe ³Key moments: ²Einstein General Theory of Relativity ²Hubble
More informationAstronomy 122 Outline
Astronomy 122 Outline This Class (Lecture 26): The Primeval Fireball Next Class: Dark Matter & Dark Energy ICES Form!!! HW10 due Friday Hubble s Law implications An expanding Universe! Run in movie in
More informationThe Early Universe: A Journey into the Past
Gravity: Einstein s General Theory of Relativity The Early Universe A Journey into the Past Texas A&M University March 16, 2006 Outline Gravity: Einstein s General Theory of Relativity Galileo and falling
More informationAstro 101 Fall 2013 Lecture 12. Cosmology. T. Howard
Astro 101 Fall 2013 Lecture 12 Cosmology T. Howard Cosmology = study of the Universe as a whole? What is it like overall?? What is its history? How old is it?? What is its future?? How do we find these
More informationThe Early Universe: A Journey into the Past
The Early Universe A Journey into the Past Texas A&M University March 16, 2006 Outline Galileo and falling bodies Galileo Galilei: all bodies fall at the same speed force needed to accelerate a body is
More informationThe slides with white background you need to know. The slides with blue background just have some cool information.
The slides with white background you need to know. The slides with blue background just have some cool information. The Big Bang cosmology the study of the origin, properties, processes, and evolution
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 informationThe Big Bang. Olber s Paradox. Hubble s Law. Why is the night sky dark? The Universe is expanding and We cannot see an infinite Universe
The Big Bang Olber s Paradox Why is the night sky dark? The Universe is expanding and We cannot see an infinite Universe Hubble s Law v = H0 d v = recession velocity in km/sec d = distance in Mpc H 0 =
More informationThe first 400,000 years
The first 400,000 years All about the Big Bang Temperature Chronology of the Big Bang The Cosmic Microwave Background (CMB) The VERY early universe Our Evolving Universe 1 Temperature and the Big Bang
More informationDark Energy and the Accelerating Universe
Dark Energy and the Accelerating Universe Dragan Huterer Department of Physics University of Michigan The universe today presents us with a grand puzzle: What is 95% of it made of? Shockingly, we still
More informationThe Standard Big Bang What it is: Theory that the universe as we know it began billion years ago. (Latest estimate: 13:82 ± 0:05 billion years!)
The Standard Big Bang What it is: Theory that the universe as we know it began 13-14 billion years ago. (Latest estimate: 13:82 ± 0:05 billion years!) Initial state was a hot, dense, uniform soup of particles
More informationFURTHER COSMOLOGY Book page T H E M A K E U P O F T H E U N I V E R S E
FURTHER COSMOLOGY Book page 675-683 T H E M A K E U P O F T H E U N I V E R S E COSMOLOGICAL PRINCIPLE Is the Universe isotropic or homogeneous? There is no place in the Universe that would be considered
More informationThe Contents of the Universe (or/ what do we mean by dark matter and dark energy?)
The Contents of the Universe (or/ what do we mean by dark matter and dark energy?) Unseen Influences Dark Matter: An undetected form of mass that emits little or no light but whose existence we infer from
More informationInflationary Universe and. Quick survey about iclickers Review of Big Bang model of universe Review of Evidence for Big Bang Examining Inflation
Inflationary Universe and Quick survey about iclickers Review of Big Bang model of universe Review of Evidence for Big Bang Examining Inflation Survey questions 1. The iclickers used in class encouraged
More informationSurvey questions. Inflationary Universe and. Survey Questions. Survey questions. Survey questions
Inflationary Universe and Quick survey about iclickers Review of Big Bang model of universe Review of Evidence for Big Bang Examining Inflation Survey questions 1. The iclickers used in class encouraged
More informationThe Cosmic Microwave Background
The Cosmic Microwave Background Our probe of the birth of the universe Will Handley wh260@cam.ac.uk Astrophysics Department Cavendish Laboratory University of Cambridge 20 th March 2013 Overview Light
More informationVisit for more fantastic resources. Edexcel. A Level. A Level Physics. Astrophysics 2 (Answers) Name: Total Marks: /30
Visit http://www.mathsmadeeasy.co.uk/ for more fantastic resources. Edexcel A Level A Level Physics Astrophysics 2 (Answers) Name: Total Marks: /30 Maths Made Easy Complete Tuition Ltd 2017 1. The Doppler
More informationLarge-Scale Structure
Large-Scale Structure Evidence for Dark Matter Dark Halos in Ellipticals Hot Gas in Ellipticals Clusters Hot Gas in Clusters Cluster Galaxy Velocities and Masses Large-Scale Distribution of Galaxies 1
More informationLecture #25: Plan. Cosmology. The early Universe (cont d) The fate of our Universe The Great Unanswered Questions
Lecture #25: Plan Cosmology The early Universe (cont d) The fate of our Universe The Great Unanswered Questions Announcements Course evaluations: CourseEvalUM.umd.edu Review sheet #3 was emailed to you
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 informationOUSSEP Final Week. If we run out of time you can look at uploaded slides Pearson Education, Inc.
OUSSEP Final Week Last week hopefully read Holiday-Week 23rd November Lecture notes Hand in your Hubble Deep Field Reports today! (If not today then in my mail box @ International College.) Today we will
More informationStudy Guide Chapter 2
Section: Stars Pages 32-38 Study Guide Chapter 2 Circle the letter of the best answer for each question. 1. What do scientists study to learn about stars? a. gravity c. space b. starlight d. colors COLOR
More informationThe expansion of the Universe, and the big bang
The expansion of the Universe, and the big bang Q: What is Hubble s law? A. The larger the galaxy, the faster it is moving way from us. B. The farther away the galaxy, the faster it is moving away from
More informationAstronomy 422. Lecture 20: Cosmic Microwave Background
Astronomy 422 Lecture 20: Cosmic Microwave Background Key concepts: The CMB Recombination Radiation and matter eras Next time: Astro 422 Peer Review - Make sure to read all 6 proposals and send in rankings
More information12/6/18. Our Schedule. Cosmology topics and issues. Cosmological (Big) Redshifts (from expansion of universe)
ASTR 1040: Stars & Galaxies Our Schedule Homework #13 due today Review Set #4 available -- final review on next Wed Dec 12, 5pm-7pm by Ryan Please do course evaluation (FCQ) online for course + recitation
More information