The Mystery of Dark Matter
|
|
- Roy Stanley
- 6 years ago
- Views:
Transcription
1 The Mystery of Dark Matter Maxim Perelstein, LEPP/Cornell U. CIPT Fall Workshop, Ithaca NY, September
2 Introduction Last Fall workshop focused on physics of the very small - elementary particles This time, we ll talk about very large - astronomical - distance scales... and some interesting connections between the two!
3 Distances in the Universe Solar System 10^12 m Galaxy 10^21 m Cluster of Galaxies 10^23 m Visible Universe 10^26 m Earth 10^7 m Evidence for Dark Matter comes from these scales
4 Measuring Distances
5 Doppler Effect in Astronomy Analyze spectra of light from distant stars/galaxies Identify absorption (or emission) line patterns of familiar elements observed on Earth Overall shift of lines - Doppler effect - allows to determine relative velocity of the star/galaxy with respect to Earth
6 Expanding Universe Light from all distant galaxies is redshifted they are running away from us! (Hubble, 1930 s) Picture: Universe is like an expanding gas of galaxies Extrapolate back in time: there was a time when density was infinite - BIG BANG! Note: Uniformly expanding gas has no center - any observer (far away from the walls) would see the same picture!
7 Universe: Infinite or Finite? horizon : signals sent from here 14 bln years ago are just reaching us now (R ~ 10^26 m) Light: c=3*10^8 m/sec You Are Here visible universe : inside the horizon Big Bang Theory: Age = 14 billion years Inaccessible universe : outside the horizon. Finite? Not? We have no way to tell.
8 Evidence for DM on the Galactic Scale Most galaxies (including ours) are orbited by satellites, much like Sun is orbited by planets. Satellites are just baby galaxies.
9 Rotation Curves Predicted Newton s law of gravitation
10 Rotation Curves Observed? NO! Kuzio de Naray et al, The Astrophysical Journal Letters, Volume 710, L161-L166 (2010) Two Possible Conclusions: Newton s Law of Gravity is wrong at large distances OR... Visible galaxy is surrounded by gravitating dark matter
11 Dark Matter Halo v independent of R implies
12 Gravitational Lensing Einstein s General Relativity: any gravitating mass should bend light Massive objects between source and observer can act as gravitational lenses Observation of lensing provides information about the mass of the lens - a way to weigh distant galaxies
13 Weak Lensing Distortion of shapes of distant sources Allows to map spatial profile, or distribution, of mass in the distant galaxy (or cluster of galaxies) that acted as the lens
14 Evidence for DM: Bullet Cluster Observation: profile of gravitating mass is NOT the same as the profile of visible (luminous) mass direct evidence for the existence of dark matter inconsistent with modifications of Newton s law
15 Summary So Far Motion of galactic satellites breakdown of Newton s law OR extra matter, gravitating but invisible ( dark ) Gravitational lensing must be dark matter Some possibilities: Huge hydrogen clouds? Non-luminous star remnants? Black holes? Sub-stellar mass objects (e.g. MACHOs )? The answer turns out to be much more exciting - stay tuned!
16 More Evidence for DM: Echoes from the Early Universe Nucleosynthesis : protons+neutrons combined to form He, Li, B,... Recombination : protons+electrons combined to form atoms
17 Cosmic Microwave Background Light: c=3*10^8 m/sec You Are Here In the early universe, photons are part of charged plasma - a hot gas, at a temperature of about 4000 K at recombination After recombination, photons no longer interact - decouple - and they come straight to us and can be observed! Provide direct information about conditions in the Universe just 400,000 yrs after Big Bang.
18 CMB:Observations Observing CMB: see Michael Niemack s talk and lab tour later today Photon energy can be measured, and is simply related to the temperature of the gas at the time when it decoupled, in the place where it comes from First conclusion: Universe at 400,000 years of age was remarkably homogeneous - no big lumps! But subtle variations in energy (at the level of 1 part in 100,000) exist, indicating tiny inhomogeneities in the primordial plasma
19 CMB:Observations Details of CMB inhomogeneities contain a wealth of information about properties of the Universe (average on very large distance scales) Since their discovery in 1992 by the COBE satellite, measuring and interpreting the CMB inhomogeneities has been a major research program Now we know (among other things): the total (average) density of the Universe, and the total (average) density of ordinary matter (protons, neutrons, electrons).
20 Weighing the Universe Space can be curved : e.g. a 2D world on a sphere In curved space, parallel lines can meet, and triangle angles do not add up to 180 What about our 3D space? On everyday distance scales, experience suggests it is flat At cosmological scales (~10^26 m), this is an experimental question, which was only answered recently, by studying CMB Einstein s General Relativity connects the average density of energy (or mass) in the Universe to the curvature: FLAT CLOSED OPEN
21 CMB:Curvature Determination Need an object of a known size, at a known distance from us Measure its apparent size infer bending of light rays infer curvature The size of hot/cold spots in the primordial gas at recombination time provides just such an object!
22 CMB:Curvature Determination Need an object of a known size, at a known distance from us Measure its apparent size infer bending of light rays infer curvature The size of hot/cold spots in the primordial gas at recombination time provides just such an object! The Universe Is Flat:
23 Normal Matter Density Nucleosynthesis : protons+neutrons combined to form He, Li, B,... All matter on Earth consists of: protons, neutrons, electrons, photons, neutrinos Almost all mass is contained in protons and neutrons: CMB hot/cold spot pattern provides information about the density of these particles at recombination time Independent verification is provided by measurements of abundances of He, Li, B, etc., which are related to proton and neutron densities by the theory of nucleosynthesis
24 Normal Matter Density Nucleosynthesis : protons+neutrons combined to form He, Li, B,... All matter on Earth consists of: protons, neutrons, electrons, photons, neutrinos Almost all mass is contained in protons and neutrons: CMB hot/cold spot pattern provides information about the density of these particles at recombination time Independent verification is provided by measurements of abundances of He, Li, B, etc., which are related to proton and neutron densities by the theory of nucleosynthesis Normal Matter is 4% of the Total
25 What Is the Universe Made Of? 96% of the Universe is Dark : Dark Matter and Dark Energy (DE is topic for another day!) Dark matter CANNOT be gas, small stars, MACHOs, etc. - all those things are made of protons, neutrons, and electrons, while DM is NOT!
26 DM and Particle Physics Particle physicists love their Standard Model, considered a great triumph of physics [see my Fall 12 CIPT talk] Most particles in the SM are highly unstable - cannot account for DM Only stable particle that s not constrained by 4% is neutrino, but they are too light to be DM Conclusion: DM must be made out of NEW, as yet undiscovered particles!!! DM? DM particle must be electrically neutral, and interact only weakly with ordinary matter
27 Example: Supersymmetry DM Candidates Supersymmetry is the idea that each SM particle has a new, much heavier (but still tiny) particle associated with it - superpartner In simple models, the lightest supersymmetric particle - LSP - is stable If electrically neutral, it can be dark matter!
28 Dark Matter and Colliders collider detector High-energy colliders, such as the Large Hadron Collider (LHC), can produce new dark matter particles! Signature in the detector: missing momentum event : DM production (computer simulation) Not observed so far - another chance in the next LHC run, in
29 Dark Matter Underground There s dark matter all around us! Density depends on the mass of the DM particle: e.g. for SUSY dark matter, expect about 1 per coffee cup DM particles can scatter on ordinary nuclei, deposit (small) energy Detecting requires going deep underground (to shield from cosmic rays), low temperatures (to suppress thermal noise), and large detectors (to increase signal rates) Many experiments around the world - the hunt is on!
30 Direct DM Searches Evolution of the s SI for a 50 GeVêc 2 WIMP WIMP-Nucleon 2 D Ê Ê Ê Ú Ê Ê Ú Ê ÚÚ Ê ÚÁ Ì Ì Ûı Ì Û Ì Û Á Ê Cryogenic Detectors Crystals Ï Liquid Argon Ú Liquid Xenon Ù Threshold Detectors Year
31 γ γ Dark Matter in the Sky Indirect Detection Indirect Detection γ γ Fermi Fermi VERITAS VERITAS Super-K Super-K ICECUBE ICECUBE Super K Super K PAMELA PAMELA +, e+, p, p e e, e, p, p AMS AMS
32 Cosmic Positrons data data consistent with DM origin of the excess, although more prosaic explanations (e.g. pulsars) are also possible standard astrophysics prediction
33 Conclusions Evidence for dark matter comes from dynamics of galaxies, gravitational lensing, and cosmic microwave background The scientific case for existence of dark matter is rock-solid. It makes ~25% of mass in the Universe It cannot be made of known elementary particles Theories of new elementary particles often have dark matter candidates, e.g. supersymmetry The hunt is on for the DM particle: at colliders, underground, and in the sky Stay Tuned!
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
More informationDennis Silverman UC Irvine Physics and Astronomy Talk to UC Irvine OLLI May 9, 2011
Dennis Silverman UC Irvine Physics and Astronomy Talk to UC Irvine OLLI May 9, 2011 First Discovery of Dark Matter As you get farther away from the main central mass of a galaxy, the acceleration from
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 informationTa-Pei Cheng PCNY 9/16/2011
PCNY 9/16/2011 Ta-Pei Cheng For a more quantitative discussion, see Relativity, Gravitation & Cosmology: A Basic Introduction (Oxford Univ Press) 2 nd ed. (2010) dark matter & dark energy Astronomical
More informationDark Matter Searches. Marijke Haffke University of Zürich
University of Zürich Structure Ι. Introduction - Dark Matter - WIMPs Ι Ι. ΙΙΙ. ΙV. V. Detection - Philosophy & Methods - Direct Detection Detectors - Scintillators - Bolometer - Liquid Noble Gas Detectors
More informationParticles in the Early Universe
Particles in the Early Universe David Morrissey Saturday Morning Physics, October 16, 2010 Using Little Stuff to Explain Big Stuff David Morrissey Saturday Morning Physics, October 16, 2010 Can we explain
More informationToday. Gravitational Lenses 11/19/2013. Astronomy Picture of the Day
ASTR 1020: Stars & Galaxies November 15, 2013 Reading for Monday: Chapter 23, section 23.1-23.3. MasteringAstronomy homework on Galaxy Evolution is due tonight at midnight. Exam 3 is on Wednesday, Nov.
More informationReview of Lecture 15 3/17/10. Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath
Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath A2020 Disk Component: stars of all ages, many gas clouds Review of Lecture 15 Spheroidal Component: bulge & halo, old
More informationDark Matter & Dark Energy. Astronomy 1101
Dark Matter & Dark Energy Astronomy 1101 Key Ideas: Dark Matter Matter we cannot see directly with light Detected only by its gravity (possible future direct detection in the lab) Most of the matter in
More informationGravity and the Universe
Gravity and the Universe Test general rela7vity via: Solar System / lab tests Binary pulsars Black hole mergers (future) Cosmology evolu7on of the Universe Gravita7onal 7me dila7on observable directly
More informationChapter 16 Dark Matter, Dark Energy, & The Fate of the Universe
16.1 Unseen Influences Chapter 16 Dark Matter, Dark Energy, & The Fate of the Universe Dark Matter: An undetected form of mass that emits little or no light but whose existence we infer from its gravitational
More informationA100H Exploring the Universe: Quasars, Dark Matter, Dark Energy. Martin D. Weinberg UMass Astronomy
A100H Exploring the :, Dark Matter, Dark Energy Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 19, 2016 Read: Chaps 20, 21 04/19/16 slide 1 BH in Final Exam: Friday 29 Apr at
More informationMoment of beginning of space-time about 13.7 billion years ago. The time at which all the material and energy in the expanding Universe was coincident
Big Bang Moment of beginning of space-time about 13.7 billion years ago The time at which all the material and energy in the expanding Universe was coincident Only moment in the history of the Universe
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 information3 The lives of galaxies
Discovering Astronomy : Galaxies and Cosmology 24 3 The lives of galaxies In this section, we look at how galaxies formed and evolved, and likewise how the large scale pattern of galaxies formed. But before
More informationDark Matter: Finding the Invisible
Dark Matter: Finding the Invisible Laura Storch Boston University WR150 LA Image courtesy of Hubble Deep Field Overview: Dark Matter: -Why do we think it exists? -Observational evidence -What are its properties?
More informationAstro-2: History of the Universe. Lecture 5; April
Astro-2: History of the Universe Lecture 5; April 23 2013 Previously.. On Astro-2 Galaxies do not live in isolation but in larger structures, called groups, clusters, or superclusters This is called the
More informationWeek 3 - Part 2 Recombination and Dark Matter. Joel Primack
Astro/Phys 224 Spring 2012 Origin and Evolution of the Universe Week 3 - Part 2 Recombination and Dark Matter Joel Primack University of California, Santa Cruz http://pdg.lbl.gov/ In addition to the textbooks
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 informationDark matter: summary
Dark matter: summary Gravity and detecting Dark Matter Massive objects, even if they emit no light, exert gravitational forces on other massive objects. m 1 r 12 m 2 We study the motions (dynamics) of
More informationChapter 23: Dark Matter, Dark Energy & Future of the Universe. Galactic rotation curves
Chapter 23: Dark Matter, Dark Energy & Future of the Universe Galactic rotation curves Orbital speed as a function of distance from the center: rotation_of_spiral_galaxy.htm Use Kepler s Third Law to get
More informationThe Universe: What We Know and What we Don t. Fundamental Physics Cosmology Elementary Particle Physics
The Universe: What We Know and What we Don t Fundamental Physics Cosmology Elementary Particle Physics 1 Cosmology Study of the universe at the largest scale How big is the universe? Where What Are did
More informationUSC Engineering Honors Colloquium 26 April Rene A. Ong (UCLA)
Hunting for the Dark Matter of the Universe USC Engineering Honors Colloquium 26 April 2013 Rene A. Ong (UCLA) Outline What is Dark Matter? How do we know it s there? What could it be and how are we trying
More informationActive 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
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 informationDark Matter in Particle Physics
High Energy Theory Group, Northwestern University July, 2006 Outline Framework - General Relativity and Particle Physics Observed Universe and Inference Dark Energy, (DM) DM DM Direct Detection DM at Colliders
More informationDark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab
Dark Matter ASTR 2120 Sarazin Bullet Cluster of Galaxies - Dark Matter Lab Mergers: Test of Dark Matter vs. Modified Gravity Gas behind DM Galaxies DM = location of gravity Gas = location of most baryons
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 informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 12 Nov. 18, 2015 Today Big Bang Nucleosynthesis and Neutrinos Particle Physics & the Early Universe Standard Model of Particle
More informationREALIZING EINSTEIN S DREAM. Exploring Our Mysterious Universe
REALIZING EINSTEIN S DREAM Exploring Our Mysterious Universe Mysteries of the Universe Quarks Leptons Higgs Bosons Supersymmetric Particles SuperString Theory Dark Matter Dark Energy and the cosmological
More informationDARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1
DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark
More informationCosmologists dedicate a great deal of effort to determine the density of matter in the universe. Type Ia supernovae observations are consistent with
Notes for Cosmology course, fall 2005 Dark Matter Prelude Cosmologists dedicate a great deal of effort to determine the density of matter in the universe Type Ia supernovae observations are consistent
More informationToday. Last homework Due next time FINAL EXAM: 8:00 AM TUE Dec. 14 Course Evaluations Open. Modern Cosmology. Big Bang Nucleosynthesis.
Today Modern Cosmology Big Bang Nucleosynthesis Dark Matter Dark Energy Last homework Due next time FINAL EXAM: 8:00 AM TUE Dec. 14 Course Evaluations Open Elements of Modern Cosmology 1.Expanding Universe
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 informationLearning Objectives: Chapter 13, Part 1: Lower Main Sequence Stars. AST 2010: Chapter 13. AST 2010 Descriptive Astronomy
Chapter 13, Part 1: Lower Main Sequence Stars Define red dwarf, and describe the internal dynamics and later evolution of these low-mass stars. Appreciate the time scale of late-stage stellar evolution
More informationChapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo
Chapter 19 Galaxies Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past halo disk bulge Barred Spiral Galaxy: Has a bar of stars across the bulge Spiral Galaxy 1
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 informationThe Search for Dark Matter. Jim Musser
The Search for Dark Matter Jim Musser Composition of the Universe Dark Matter There is an emerging consensus that the Universe is made of of roughly 70% Dark Energy, (see Stu s talk), 25% Dark Matter,
More informationDark Matter: What is it?
Dark Matter: What is it? Dark Matter: What is it? Key Concepts 1) Some dark matter consists of MACHOs (MAssive Compact Halo Objects). 2) Some dark matter may consist of WIMPs (Weakly Interacting Massive
More informationAstr 102: Introduction to Astronomy. Lecture 16: Cosmic Microwave Background and other evidence for the Big Bang
Astr 102: Introduction to Astronomy Fall Quarter 2009, University of Washington, Željko Ivezić Lecture 16: Cosmic Microwave Background and other evidence for the Big Bang 1 Outline Observational Cosmology:
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 informationWhere we left off last time...
Where we left off last time... The Planck Era is pure speculation about topics that are being explored in detail today (gravity, string theory, etc.) The GUT era matches what physicists see in particle
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 informationNew 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
More informationCOSMOLOGY and DARK MATTER
Physics 10 1 st Lecture September 28, 2004 COSMOLOGY and DARK MATTER Joel Primack Introduction Modern cosmology the study of the universe as a whole is undergoing a scientific revolution. New ground- and
More informationBlack Holes Thursday, 14 March 2013
Black Holes General Relativity Intro We try to explain the black hole phenomenon by using the concept of escape velocity, the speed to clear the gravitational field of an object. According to Newtonian
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 informationChapter 27 The Early Universe Pearson Education, Inc.
Chapter 27 The Early Universe Units of Chapter 27 27.1 Back to the Big Bang 27.2 The Evolution of the Universe More on Fundamental Forces 27.3 The Formation of Nuclei and Atoms 27.4 The Inflationary Universe
More informationDark Matter. Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET)
Dark Matter Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET) 1 Dark Matter 1933 r. - Fritz Zwicky, COMA cluster. Rotation
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 informationUNVEILING THE ULTIMATE LAWS OF NATURE: DARK MATTER, SUPERSYMMETRY, AND THE LHC. Gordon Kane, Michigan Center for Theoretical Physics Warsaw, June 2009
UNVEILING THE ULTIMATE LAWS OF NATURE: DARK MATTER, SUPERSYMMETRY, AND THE LHC Gordon Kane, Michigan Center for Theoretical Physics Warsaw, June 2009 OUTLINE! Some things we ve learned about the physical
More informationLecture PowerPoints. Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli
Lecture PowerPoints Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching
More informationASTR 101 General Astronomy: Stars & Galaxies
ASTR 101 General Astronomy: Stars & Galaxies ANNOUNCEMENTS MIDTERM III: Tuesday, Nov 24 th Midterm alternate day: Fri, Nov 20th, 11am, ESS 450 At LAST: In the very Beginning BIG BANG: beginning of Time
More informationToday. Lookback time. ASTR 1020: Stars & Galaxies. Astronomy Picture of the day. April 2, 2008
ASTR 1020: Stars & Galaxies April 2, 2008 Astronomy Picture of the day Reading: Chapter 21, sections 21.3. MasteringAstronomy Homework on Galaxies and Hubble s Law is due April 7 th. Weak Lensing Distorts
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 information2. The evolution and structure of the universe is governed by General Relativity (GR).
7/11 Chapter 12 Cosmology Cosmology is the study of the origin, evolution, and structure of the universe. We start with two assumptions: 1. Cosmological Principle: On a large enough scale (large compared
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 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 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 informationD.V. Fursaev JINR, Dubna. Mysteries of. the Universe. Problems of the Modern Cosmology
Mysteries of D.V. Fursaev JINR, Dubna the Universe Problems of the Modern Cosmology plan of the lecture facts about our Universe mathematical model, Friedman universe consequences, the Big Bang recent
More informationLab Monday optional: review for Quiz 3. Lab Tuesday optional: review for Quiz 3.
Announcements SEIs! Quiz 3 Friday. Lab Monday optional: review for Quiz 3. Lab Tuesday optional: review for Quiz 3. Lecture today, Wednesday, next Monday. Final Labs Monday & Tuesday next week. Quiz 3
More informationChapter 27: The Early Universe
Chapter 27: The Early Universe The plan: 1. A brief survey of the entire history of the big bang universe. 2. A more detailed discussion of each phase, or epoch, from the Planck era through particle production,
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 informationOverview of Dark Matter models. Kai Schmidt-Hoberg
Overview of Dark Matter models. Kai Schmidt-Hoberg Evidence for dark matter. Compelling evidence for dark matter on all astrophysical scales: Galactic scales: Rotation curves of Galaxies Kai Schmidt-Hoberg
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 11 Nov. 13, 2015 Today Cosmic Microwave Background Big Bang Nucleosynthesis Assignments This week: read Hawley and Holcomb,
More informationPhysics 133: Extragalactic Astronomy ad Cosmology
Physics 133: Extragalactic Astronomy ad Cosmology Lecture 2; January 8 2014 Previously on PHYS133 Units in astrophysics Olbers paradox The night sky is dark. Inconsistent with and eternal, static and infinite
More informationBrief Introduction to Cosmology
Brief Introduction to Cosmology Matias Zaldarriaga Harvard University August 2006 Basic Questions in Cosmology: How does the Universe evolve? What is the universe made off? How is matter distributed? How
More informationOther Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies
Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at
More informationDark Matter and Dark Energy
Dark Matter and Dark Energy Jim Pivarski March 4, 2012 Matter as we know it is a minority of the universe. Jim Pivarski 2/51 Jim Pivarski 3/51 Jim Pivarski 4/51 This talk: What is dark matter? The astronomer
More informationThe Dark Side of the Universe: Dark matter in the galaxy and Cosmos
Utah State University DigitalCommons@USU Public Talks Astrophysics 1-18-2011 The Dark Side of the Universe: Dark matter in the galaxy and Cosmos Shane L. Larson Utah State University Follow this and additional
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 informationChapter 22 Lecture. The Cosmic Perspective. Seventh Edition. The Birth of the Universe Pearson Education, Inc.
Chapter 22 Lecture The Cosmic Perspective Seventh Edition The Birth of the Universe The Birth of the Universe 22.1 The Big Bang Theory Our goals for learning: What were conditions like in the early universe?
More informationThe Search for Dark Matter, and Xenon1TP
The Search for Dark Matter, and Xenon1TP by Jamin Rager Hillsdale College Assistant Prof. Rafael Lang Purdue University Dept. of Physics Galaxy NGC 3198 2 Galaxy NGC 3198 Rotation Curves http://bustard.phys.nd.edu/phys171/lectures/dm.html
More informationChapter 22 What do we mean by dark matter and dark energy?
Chapter 22 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 its gravitational influence
More informationIntroduction and Fundamental Observations
Notes for Cosmology course, fall 2005 Introduction and Fundamental Observations Prelude Cosmology is the study of the universe taken as a whole ruthless simplification necessary (e.g. homogeneity)! Cosmology
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 informationToday: Start Ch. 18: Cosmology. Homework # 5 due next Wed. (HW #6 is online)
Today: Start Ch. 18: Cosmology Homework # 5 due next Wed. (HW #6 is online) Dark Matter! A rotation curve is a graph of how fast a something is rotating, as a function of distance from the center.! We
More informationOne of elements driving cosmological evolution is the presence of radiation (photons) Early universe
The Frontier Matter and Antimatter One of elements driving cosmological evolution is the presence of radiation (photons) Early universe Matter and antimatter But we live in universe full of matter -- where
More informationProject Paper May 13, A Selection of Dark Matter Candidates
A688R Holly Sheets Project Paper May 13, 2008 A Selection of Dark Matter Candidates Dark matter was first introduced as a solution to the unexpected shape of our galactic rotation curve; instead of showing
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 informationCMB constraints on dark matter annihilation
CMB constraints on dark matter annihilation Tracy Slatyer, Harvard University NEPPSR 12 August 2009 arxiv:0906.1197 with Nikhil Padmanabhan & Douglas Finkbeiner Dark matter!standard cosmological model:
More informationAstro-2: History of the Universe
Astro-2: History of the Universe Lecture 6; April 30 2013 Lecture 5 - Summary 1 Mass concentrations between us and a given object in the sky distort the image of that object on the sky, acting like magnifying
More informationSpectra of Cosmic Rays
Spectra of Cosmic Rays Flux of relativistic charged particles [nearly exactly isotropic] Particle density Power-Law Energy spectra Exponent (p, Nuclei) : Why power laws? (constraint on the dynamics of
More informationImplications 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 informationComponents of Galaxies: Dark Matter
Components of Galaxies: Dark Matter Dark Matter: Any Form of matter whose existence is inferred solely through its gravitational effects. -B&T, pg 590 Nature of Major Component of Universe Galaxy Formation
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 informationAstr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic
Astr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic Inflation Galaxy Formation 1 Chapter 24: #3 Chapter
More informationThe 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
More informationDark Matter and the DRIFT. Experiment. Why do we believe. How shall we identify it? What is Dark. Matter? in it? C. J. Martoff, Professor of Physics
Dark Matter and the DRIFT Experiment What is Dark Matter? Why do we believe in it? How shall we identify it? C J Martoff, Professor of Physics Physics C056, Astronomy Temple University Spring '03 What
More informationWhat is the Universe Made Of?
What is the Universe Made Of? The case for Dark Matter and Dark Energy, and for what they might be Cliff Burgess What is the Universe Made Of? From best fits to the Concordance Cosmology Courtesy: Ned
More informationOBSERVATIONAL EVIDENCE FOR DARK MATTER AND DARK ENERGY. Marco Roncadelli INFN Pavia (Italy)
OBSERVATIONAL EVIDENCE FOR DARK MATTER AND DARK ENERGY Marco Roncadelli INFN Pavia (Italy) ABSTRACT Assuming KNOWN physical laws, I first discuss OBSERVATIONAL evidence for dark matter in galaxies and
More informationBig Bang Theory PowerPoint
Big Bang Theory PowerPoint Name: # Period: 1 2 3 4 5 6 Recombination Photon Epoch Big Bang Nucleosynthesis Hadron Epoch Hadron Epoch Quark Epoch The Primordial Era Electroweak Epoch Inflationary Epoch
More informationCosmology. Clusters of galaxies. Redshift. Late 1920 s: Hubble plots distances versus velocities of galaxies. λ λ. redshift =
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
More informationAST1100 Lecture Notes
AST1100 Lecture Notes 4 Stellar orbits and dark matter 1 Using Kepler s laws for stars orbiting the center of a galaxy We will now use Kepler s laws of gravitation on much larger scales. We will study
More informationPHY326/426 Dark Matter and the Universe. Dr. Vitaly Kudryavtsev F9b, Tel.:
PHY326/426 Dark Matter and the Universe Dr. Vitaly Kudryavtsev F9b, Tel.: 0114 2224531 v.kudryavtsev@sheffield.ac.uk Indirect searches for dark matter WIMPs Dr. Vitaly Kudryavtsev Dark Matter and the Universe
More informationGravitational Efects and the Motion of Stars
Gravitational Efects and the Motion of Stars On the largest scales (galaxy clusters and larger), strong evidence that the dark matter has to be non-baryonic: Abundances of light elements (hydrogen, helium
More informationDark Side of the Universe
Dark Side of the Universe Bhaskar Dutta Department of Physics & Astronomy Texas A&M University Dark Side of the Universe 1 Content of the Universe 4% The 23% is still unobserved in the laboratory.. (This
More informationThe 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
More informationThe Big Bang Theory, General Timeline. The Planck Era. (Big Bang To 10^-35 Seconds) Inflationary Model Added. (10^-35 to 10^-33 Of A Second)
The Big Bang Theory, General Timeline The Planck Era. (Big Bang To 10^-35 Seconds) The time from the exact moment of the Big Bang until 10^-35 of a second later is referred to as the Planck Era. While
More information