Lecture 30: Geometry & Expansion of the. Astronomy 101
|
|
|
- Duane Todd
- 5 years ago
- Views:
Transcription
1 Lecture 30: Geometry & Expansion of the Universe Astronomy 101
2 Cosmology Cosmology is the study of the entire Universe: Physics of the Universe. Distribution of objects on allscales scales. Motions of objects in the Universe. Evolution of the Universe. Age, Origin, and Fate of the Universe.
3 The Universe in : Einstein explored the cosmological implications of General Relativity. Observational State in 1917: Kapteyn model of the Milky Way was favored by some (but not all) astronomers. No agreement on the spiral nebulae. First good calibrations of the P L relation lti for Cepheids and RR Lyrae variables.
4 The Cosmological Principle The Universe is Homogeneous and Isotropic on the Largest Scales. Critical assumption underlying Cosmology. Homogeneous: No special places in the Universe. Isotropic: No special directions
5 Homogeneity When viewed on thelargest scales: The average density of matter is about the same in allplaces in the Universe. The Universe is fairly smooth on large scales. Does not apply locally: We see planets, stars, galaxies in regions nearby in space. The Universe is locally rather lumpy.
6 Isotropy When viewed on thelargest scales: The Universe looks the same to all observers. TheUniverse looks the same in all directions as viewed by a particular observer. Does not apply locally: We see different numbers of local objects in different directions.
7 The Dynamic Universe Einstein applied thecosmological Principle to General Relativity and got a surprise: Thespacetime of the Universe could not be static and unchanging. TheUniverse must either expand or contract! Astronomers assured him that no such general motion was observed
8 The Cosmological Constant To make the Universe static, he added a new term in his field equations: The Cosmological Constant, : Repulsive gravitation like force term Ai Arises from empty space. Balances the effects of gravity.
9 Discovery of Expansion : Vesto Slipher, Lowell Observatory Measured radial velocities from spectra of 25 galaxies. Found: 21 of the 25 galaxies show a redshift. speeds of some >1000 km/sec Most galaxies are rapidly receding from us.
10 Hubble s Discovery 1929: Edwin Hubble Measured distances to 25 galaxies: Used dcepheids and brightest biht tstars. Compared distances with recession velocities. Discovered: Recession velocity gets larger with distance. Systematic expansion of the Universe.
11 Hubble s Data (1929) Rece ession Vel locity (km m/sec) Distance (Mpc)
12 Refinement The 1929 work was very suggestive of an effect, but the uncertainties were large. Setabout collecting moredata: By 1931: Added 8 more galaxies with distance estimates Most distant galaxy had a recession velocity of nearly 20,000 km/sec! Showed a stronger, tighter trend with distance
13 Hubble & Humason (1931) Re ecession Velocity (k km/sec) 20, ,000 10, Data Distance (Mpc)
14 Hubble s Law v H d v = recession velocity in km/sec d = distance dsa in Mpc H = Hubble s Constant = 75 km/sec/mpc In words: The more distant a galaxy, the faster its recession velocity.
15 Interpretation Hubble s Law demonstrates that theuniverse is expanding in a systematic way: The more distant a galaxy is, the faster it appears to be moving away from us. Rateof expansion = Hubble Constant. Comments: Hubble s Law is empirical ii based only on data Not an exact law.
16 Nature of the Expansion General Expansion of Spacetime: All observers in different galaxies see the same expansion around them. No center all observers appear to be at the center. What is the recession velocity? NOT motion through space... Expansion of spacetime: galaxies carried along.
17 Systematic Expansion Universe 2x larger Galaxies are 2x further apart
18 Cosmological Redshift Most galaxies are receding from us. Convenient to express recession velocity as a redshift for the galaxy. Redshift (z): Directly observable quantity. Measured accurately from spectral lines shifts. Often express cosmic distances as redshifts.
19 Redshift Distances d v H Distances estimated using Hubble s Law even for very distant objects
20 Mapping the Universe Can map the distribution of galaxies using redshifts. Largest map includes ~1,000,000 galaxies Reveals sheets and filaments of galaxies surrounding great voids. Depth is ~500 Mpc (or so)
21 Sloan Digital Sky Survey Dedicated meter telescope in New Mexico Image 1/4 of the sky in 5 colors: 100 Million Galaxies 100 Million Stars RdhiftS Redshift Survey: 1 Million Galaxies 100, Quasars
22 1920s: What about the Cosmological Constant? DeSitter corrects an error in Einstein s math, showed that the Universe was unstable. Friedmann & Lemaître showed that without, GR predicts that the Universe expands. Hubble firmly established cosmic expansion observationally
23 State of the Art Einstein s guess about the homogeneity and isotropy of the Universe was brilliant and far ahead of the scanty empirical data of his time. Modern observations bear out large scale homogeneity and isotropy: Large scale galaxy surveys. Maps of the cosmic background radiation.
24
25
26 Modern Cosmological Constant In current cosmological theory, reappears in a somewhat modified form: Introduced as the vacuum energy of space. Quantum ground state of empty space. Assumed to be either very very small or zero. Distinction: Its use today is arguably better physically motivated than when Einstein used it in 1917.
27 Modern Cosmological Constant Recent supernova observations suggest a non zero May mean that there is a form of dark energy pushing against gravity Form is almost completely l unknown and a subject for 21st century astrophysics Many projects are planned over the next 10 years to characterize dark energy
28 Vesto Slipher Willem de Sitter Georges Lemaître Edwin Hubble Albert Einstein Alexsandr Friedmann
29 Summary: Cosmological Principle: The Universe is Homogeneous and Isotropic on Large Scales. No special places or directions. General Relativity predicts an expanding universe. Cosmological lconstant
30 Hubble s Law: Summary: Galaxies are receding from us. Recession velocity gets larger with distance. Hubble Constant: Rateof expansion of the Universe. Cosmological Redshift: Redshift distances Redshift maps of the Universe.
Lecture 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
Lecture 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
The History and Philosophy of Astronomy
Astronomy 350L (Fall 2006) The History and Philosophy of Astronomy (Lecture 22: Hubble II) Instructor: Volker Bromm TA: Jarrett Johnson The University of Texas at Austin Edwin P. Hubble: Mariner of the
V. 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
AST 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
Lecture 14: Cosmological Principles
Lecture 14: Cosmological Principles The basic Cosmological Principles The geometry of the Universe The scale factor R and curvature constant k Comoving coordinates Einstein s initial solutions 3/28/11
Ay1 Lecture 17. The Expanding Universe Introduction to Cosmology
Ay1 Lecture 17 The Expanding Universe Introduction to Cosmology 17.1 The Expanding Universe General Relativity (1915) A fundamental change in viewing the physical space and time, and matter/energy Postulates
There 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
Lecture 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
Today in Astronomy 102: relativity and the Universe
Today in Astronomy 102: relativity and the Universe General relativity and the Universe. Hubble: the Universe is observed to be homogeneous, isotropic, and expanding Redshift and distance: Hubble s Law
VM Slipher and the discovery of the expanding universe The Big Bang: Fact or Fiction?
VM Slipher and the discovery of the expanding universe The Big Bang: Fact or Fiction? Cormac O Raifeartaigh Waterford Institute of Technology Overview A brief history of experiment (1912-1931) The redshifts
Learning Objectives. distances to objects in our Galaxy and to other galaxies? apparent magnitude key to measuring distances?
The Distance Ladder 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
The 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
ASTR 200 : Lecture 27. Expansion and large scale structure
ASTR 200 : Lecture 27 Expansion and large scale structure 1 A preference for recession In 1912, american astronomer Vesto Slipher began painstakingly acquiring spectra of `spiral nebulae' and was the first
Cosmic 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
Chapter 26: Cosmology
Chapter 26: Cosmology Cosmology means the study of the structure and evolution of the entire universe as a whole. First of all, we need to know whether the universe has changed with time, or if it has
The 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
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
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
Galaxies 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
Cosmology with the Sloan Digital Sky Survey Supernova Search. David Cinabro
Cosmology with the Sloan Digital Sky Survey Supernova Search David Cinabro Cosmology Background The study of the origin and evolution of the Universe. First real effort by Einstein in 1916 Gravity is all
Based on observations with the 2-m RCC telescope of Rozhen National. Academy of Sciences.
Based on observations with the 2-m RCC telescope of Rozhen National Astronomical Observatory operated by Institute of Astronomy, Bulgarian Academy of Sciences. http://www.nao-rozhen.org Photo: P. Markishky
LARGE QUASAR GROUPS. Kevin Rahill Astrophysics
LARGE QUASAR GROUPS Kevin Rahill Astrophysics QUASARS Quasi-stellar Radio Sources Subset of Active Galactic Nuclei AGNs are compact and extremely luminous regions at the center of galaxies Identified as
Hubble Ultra Deep Space View
Galaxies stars come in large groups (20-1000 billion stars) called Galaxies >2 trillion observable galaxies. Come in Shapes and Sizes depending on how they were formed Elliptical (football shape) Spirals
Astronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 7 Oct. 30, 2015 Today Relativistic Cosmology Dark Side of the Universe I: Dark Matter Assignments This week: read Hawley and
Physics 24: The Big Bang, Week 3: Hubble s Law David Schlegel, LBNL
Physics 24: The Big Bang, Week 3: Hubble s Law David Schlegel, LBNL 1905: Albert Einstein s theory of special relativity 1915: Albert Einstein s theory of general relativity 1920: Harlow Shapley & Heber
The Big Bang: Fact or Fiction?
The discovery of the expanding universe Paradigm shift or slow dawning? The Big Bang: Fact or Fiction? Cormac O Raifeartaigh FRAS 223 rd AAS meeting, Washington D.C. 5/01/14 Open-top bus tour A brief history
The Big Bang Theory. Rachel Fludd and Matthijs Hoekstra
The Big Bang Theory Rachel Fludd and Matthijs Hoekstra Theories from Before the Big Bang came from a black hole from another universe? our universe is part of a multiverse? just random particles? The Big
Short introduction to the accelerating Universe
SEMINAR Short introduction to the accelerating Universe Gašper Kukec Mezek Our expanding Universe Albert Einstein general relativity (1917): Our expanding Universe Curvature = Energy Our expanding Universe
Cosmology with the Sloan Digital Sky Survey Supernova Search. David Cinabro
Cosmology with the Sloan Digital Sky Survey Supernova Search David Cinabro Cosmology Background The study of the origin and evolution of the Universe. First real effort by Einstein in 1916 Gravity is all
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
The 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
The 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.
Island 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
The 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
Astronomy 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!
Astronomy Hour Exam 2 March 10, 2011 QUESTION 1: The half-life of Ra 226 (radium) is 1600 years. If you started with a sample of 100 Ra 226
Astronomy 101.003 Hour Exam 2 March 10, 2011 QUESTION 1: The half-life of Ra 226 (radium) is 1600 years. If you started with a sample of 100 Ra 226 atoms, approximately how many Ra 226 atoms would be left
Galaxies. 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
Chapter 1 Introduction 1.1 The Relevance of Very Distant Galaxies
Chapter 1 Introduction 1.1 The Relevance of Very Distant Galaxies From observations of the Cosmic Microwave Background (e.g., [491]) and from other, independent astronomical observations we know that,
The 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
Slipher, galaxies, and cosmic velocity fields
Slipher, galaxies, and cosmic velocity fields John Peacock University of Edinburgh Origins of the expanding universe Flagstaff, 15 Sept 2012 The Hubble expansion V = H D in 1929, Hubble discovered the
Astro 13 Galaxies & Cosmology LECTURE 4 Tues 18 Jan 2011 P. Madau. I Cosmological Principles 25m II Why is the Sky Dark? (Olber s
Astro 13 Galaxies & Cosmology LECTURE 4 Tues 18 Jan 2011 P. Madau 20m I Cosmological Principles 25m II Why is the Sky Dark? (Olber s Paradox) 10m III Break 15m IV Expanding Univ. - Hubble Constant 20m
Class 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
- 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
Lecture 37 Cosmology [not on exam] January 16b, 2014
![Lecture 37 Cosmology [not on exam] January 16b, 2014](/thumbs/75/72758061.jpg "Lecture 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
BROCK 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
ASTR 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
Universal redshift, the Hubble constant The cosmic background radiation until COBE
Universal redshift, the Hubble constant The cosmic background radiation until COBE Sylwester Radomski Gesellschaft fuer Schwerionenforschung November 11, 2004 1 1 Dimensions in the Universe The scale of
Jodrell Bank Discovery Centre
A-level Physics: Radio Telescopes Consolidation questions For these questions, we will be considering galaxy NGC 660 (below), a rare polar-ring galaxy in the constellation of Pisces. NGC 660 consists of
The Cosmological Principle
Cosmological Models John O Byrne School of Physics University of Sydney Using diagrams and pp slides from Seeds Foundations of Astronomy and the Supernova Cosmology Project http://www-supernova.lbl.gov
Big 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
Modeling the Universe Chapter 11 Hawley/Holcomb. Adapted from Dr. Dennis Papadopoulos UMCP
Modeling the Universe Chapter 11 Hawley/Holcomb Adapted from Dr. Dennis Papadopoulos UMCP Spectral Lines - Doppler λ λ em 1+ z = obs z = λ obs λ λ em em Doppler Examples Doppler Examples Expansion Redshifts
Astroparticle physics the History of the Universe
Astroparticle physics the History of the Universe Manfred Jeitler and Wolfgang Waltenberger Institute of High Energy Physics, Vienna TU Vienna, CERN, Geneva Wintersemester 2016 / 2017 1 The History of
Hubble, using the new Cepheid variable technique, was able to measure the distances to
Cosmology The Discovery of the Universe You may recall that in 4-dimensions, the Einstein tensor is the only second rank, divergence free tensor composed of the metric and its first and second derivatives.
PHY 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
Galaxies & 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
Chapter 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
THE 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
Einstein s steady-state theory. The Big Bang: Fact or Fiction?
Einstein s steady-state theory An abandoned model of the universe The Big Bang: Fact or Fiction? Cormac O Raifeartaigh, Brendan Mcann (WIT) Werner Nahm (DIAS) and Simon Mitton (Univ. of Cambridge) Cosmology
Dark Energy and Dark Matter
Dark Energy and Dark Matter Attendance Quiz Are you here today? (a) yes (b) no Here! (c) The Dark Lord wants his ring back! Final Exam The final exam is Thursday, 6/8, from 11:30am to 1:30pm (2 hours),
Astronomy 102 Lab: Hubble Law
Name: Astronomy 102 Lab: Hubble Law Part of today s lab will involve the use of laptops. If you own one, please bring it to class. Pre-Lab Assignment: In this week's lab, you will study the expansion of
Hubble Ultra Deep Space View PHYS 162 2
Galaxies stars come in large groups (20-200 billion stars) called Galaxies >2 trillion observable galaxies. Come in Shapes and Sizes depending on how they were formed Elliptical (football shape) Spirals
Astronomy 150: Killer Skies Lecture 35, April 23
Assignments: ICES available online Astronomy 150: Killer Skies Lecture 35, April 23 HW11 due next Friday: last homework! note: lowest HW score dropped but: HW11 material will be on Exam 3, so be sure to
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.
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
BROCK UNIVERSITY. Test 2: July 2015 Number of pages: 9 Course: ASTR 1P02, Section 2 Number of students: 318
BROCK UNIVERSITY Page 1 of 9 Test 2: July 2015 Number of pages: 9 Course: ASTR 1P02, Section 2 Number of students: 318 Examination date: 4 July 2015 Time limit: 50 min Time of Examination: 13:00 13:50
The final is Thursday, July 2nd in class. Don t be late! The test will cover Chapters 1-16 and with a STRONG EMPHASIS on Chapters 9-16, 18, and
Final Exam!!! The final is Thursday, July 2nd in class. Don t be late! The test will cover Chapters 1-16 and 18-19 with a STRONG EMPHASIS on Chapters 9-16, 18, and 19. It will consist of 50 questions and
Spectroscopy in Motion: A Method to Measure Velocity
Name Partner(s) Date Spectroscopy in Motion: A Method to Measure Velocity Did you ever hear a train whistle or truck on a highway as it approaches you and then passes at a high rate of speed? Go to and
Galaxies 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
Today 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
Active Galaxies and Galactic Structure Lecture 22 April 18th
Active Galaxies and Galactic Structure Lecture 22 April 18th FINAL Wednesday 5/9/2018 6-8 pm 100 questions, with ~20-30% based on material covered since test 3. Do not miss the final! Extra Credit: Thursday
Cosmology. 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.
Chapter 1 Introduction. Particle Astrophysics & Cosmology SS
Chapter 1 Introduction Particle Astrophysics & Cosmology SS 2008 1 Ptolemäus (85 165 b.c.) Kopernicus (1473 1543) Kepler (1571 1630) Newton (1643 1727) Kant (1724 1630) Herschel (1738 1822) Einstein (1917)
Overview DARK MATTER & DARK ENERGY. Dark Matter and Dark Energy I. Definition Current Understanding Detection Methods Cosmological Impact
DARK MATTER & DARK ENERGY Source: Max Ehrhardt Modiefied for Astronomy 101 Dark Matter and Dark Energy I Physics 113 Goderya Chapter(s): 18 Learning Outcomes: Overview Definition Current Understanding
The 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
How 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
Addition 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
According 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
A100 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.
New Ideas from Astronomy and Cosmology. Martin Buoncristiani Session 5 4/21/2011
New Ideas from Astronomy and Cosmology Martin Buoncristiani Session 5 Agenda Introduction Space, Time and Matter Early views of the cosmos Important Ideas from Classical Physics Two 20 th Century revolutions
BROCK 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:
INFLATIONARY COSMOLOGY. and the ACCELERATING UNIVERSE. Alan Guth, MIT
INFLATIONARY COSMOLOGY and the ACCELERATING UNIVERSE Alan Guth, MIT An Open World of Physics Talks and Discussion by Friends of Fred Goldhaber Harriman Hall, SUNY Stony Brook, October 7, 2001 OUTLINE The
Supernovae Observations of the Expanding Universe. Kevin Twedt PHYS798G April 17, 2007
Supernovae Observations of the Expanding Universe Kevin Twedt PHYS798G April 17, 2007 Overview How do we measure expansion? Use of supernovae 1a as a good measuring stick Techniques for observing supernovae
Galaxies 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
Hubble 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
Exam 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
arxiv: v2 [physics.hist-ph] 9 Oct 2014
![arxiv: v2 [physics.hist-ph] 9 Oct 2014](/thumbs/76/73256269.jpg "arxiv: v2 [physics.hist-ph] 9 Oct 2014")
arxiv:1312.0472v2 [physics.hist-ph] 9 Oct 2014 Solar-motion correction in early extragalactic astrophysics Domingos Soares and Luiz Paulo R. Vaz Departamento de Física, ICEx, UFMG C.P. 702 30123-970, Belo
Licia Verde. ICREA & ICC-UB-IEEC CERN Theory Division.
Licia Verde ICREA & ICC-UB-IEEC CERN Theory Division http://icc.ub.edu/~liciaverde AIMS and GOALS Observational cosmology has been evolving very rapidly over the past few years Theoretical cosmology is
A 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,
Cosmology. Stellar Parallax seen. The modern view of the universe
Cosmology The modern view of the universe SC/NATS 1730, XXVIIICosmology 1 Stellar Parallax Copernicus said stellar parallax couldn t be seen because the stars were so far away. A strictly ad hoc explanation
The phenomenon of gravitational lenses
The phenomenon of gravitational lenses The phenomenon of gravitational lenses If we look carefully at the image taken with the Hubble Space Telescope, of the Galaxy Cluster Abell 2218 in the constellation
IB Physics - Astronomy
Solar System Our Solar System has eight planets. The picture below shows their relative sizes, but NOT their relative distances. A planet orbits the sun, and has gravitationally cleared its orbital area
Homework 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
Sun Building Activity 2 The Signature of the Stars
Sun Building The Signature of the Stars Rainbows reveal that white light is a combination of all the colours. In 1666, Isaac Newton showed that white light could be separated into its component colours
Lecture #21: Plan. Normal Galaxies. Classification Properties Distances
Lecture #21: Plan Normal Galaxies Classification Properties Distances Messier 31 = M31 Early 20 th Century The Great Debate (4/26/1920): Harlow Shapley (Mt Wilson) vs Heber Curtis (Lick Observatory) Smithsonian
Olbers 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
Paradigm Shifts in Cosmology
FEATURE Principal Investigator Naoshi Sugiyama Research Area Astrophysics Paradigm Shifts in Cosmology The paradigm shift as put forward by Thomas Kuhn means revolutionary changes in the normative concepts
Astronomy 25. Astronomy 25. Anything back then that could not be seen clearly was called a nebulae. detect fuzzy light objects.
Astronomy 25 Astronomy 25 Before the 1920 s s telescopes would detect fuzzy light objects. Anything back then that could not be seen clearly was called a nebulae. Immanuel Kant (1724-1804) 1804) Kant had
Astronomy 1 Winter Lecture 24; March
Astronomy 1 Winter 2011 Lecture 24; March 7 2011 Previously on Astro-1 Introduction to special relativity Introduction to general relativity Introduction to black holes, stellar and supermassive Today..
Dark Energy in Our Expanding Universe Joe Mohr Department of Astronomy Department of Physics NCSA
Dark Energy in Our Expanding Universe Joe Mohr Department of Astronomy Department of Physics NCSA 2/19/05 Saturday Morning Physics - Joe Mohr 1 Galaxies and Stars 2/19/05 Saturday Morning Physics - Joe
Cosmology. Lecture Topics. Colliding Galaxy Simulations The expanding universe Cosmology. The Age of the Universe The Big Bang
Cosmology Lecture 27: Cosmology 27 1 APOD: GOODS project Lecture Topics Colliding Galaxy Simulations The expanding universe Cosmology The cosmological principle The Age of the Universe The Big Bang 2 27-1