The Dark Matter Problem

Size: px
Start display at page:

Download "The Dark Matter Problem"

Transcription

1 The Dark Matter Problem matter : anything with equation of state w=0 more obvious contribution to matter: baryons (stars, planets, us!) and both Big Bang Nucleosynthesis and WMAP tell us that Ω baryons ~0.05 moreover, most baryons (not all) emit light and are visible, and visible matter (from counting stars and galaxies) provides only Ω visible 0.05 however, dynamical measurement of matter (through gravitational interactions) point to much higher values, an effect observed in very different systems and at very different distance scales WMAP implies Ω total =1, while the Hubble diagram of SN1a imply Ω dark energy ~0.7 so, what is the average density of matter in the Universe today?

2 Using movement to measure mass End Newtonian gravity: GM(r)=v rot 2 r

3 Rotation of spiral galaxies Vera Rubin in the 70 s was the first to show that observation of rotation of disks in their outer parts required a lot of invisible mass End

4 (from

5 (from

6 Invisible mass near the Sun! (Oort, 1932)

7 Evidence from Galaxy Clusters at about the same time End <T>=-1/2 <V TOT >

8 COMA End Milky Way CfA redshift survey

9 clusters of galaxies are the largest structures we know we expect them to contain most of the matter of the Universe their size ranges from 1 to 10 Mpc they contain 50 to 1000 galaxies + hot X-ray emitting gas and large amounts of dark matter COMA cluster today Dark Matter in Clusters is deduced by the temperature of the X-ray emitting gas (assuming hydrostatic equilibrium) in fact, observed temperatures (kt~10 s kev) are much hotter than the ones deduced from the visible mass: moreover, they show an amount of DM about 4-5 times that of baryons this should be true also on Cosmological scales but since Ω baryons ~0.05 this implied Ω DM 0.25 <<1 before SN1a data

10 Gravitational lensing in Clusters

11

12 The Bullet Cluster (smoking gun of DM vs. MOND?) 1E , 56, august 2006 DM weak lensing NB: in MOND lensing should follow baryons, i.e. the blue region should track the red one 3 components in each cluster: gas, stars (red=baryons) and lensing (blue=dark matter) stars pass through, gravitationally slowed gases interact electromagnetically, slowed further dark matter well separated in two regions near the visible galaxies see animation (MOND=Modified Gravity)

13 Evidence for Dark Matter Spiral galaxies rotation curves Clusters & Superclusters Weak gravitational lensing Strong gravitational lensing Galaxy velocities X rays Large scale structure Structure formation CMB anisotropy: WMAP Ω tot =1 Ω dark energy ~0.7 Ω matter ~ 0.27 Ω baryons ~0.05 Ω visible ~0.005 Ω dark matter ~ 0.22

14 The concordance model

15 Apart from being unable to drive galaxy formation (they decouple too late from photons, not enough time for gravitational instabilites to grow) baryons are too few in the Universe in order to explain the dark matter because of nucleosynthesis Observations give 0.6 < h < 0.8 Big Bang nucleosynthesis (deuterium abundance) and cosmic microwave background (WMAP) determine baryon contribution Ω B h , so Ω B 0.04 Ω lum (4 ± 2) (stars, gas, dust) => baryonic dark matter has to exist (maybe as warm intergalactic gas?) But, now we know that Ω M > 0.2, so there has to exist non-baryonic dark matter Lithium underabundant? Fields & Sarkar, 2004

16 A lot of matter in the Universe is dark and non-baryonic P.S.:but also some baryonic DM needed

17 The properties of a good Dark Matter candidate: stable (protected by a conserved quantum number) no charge, no colour (weakly interacting) cold, non dissipative relic abundance compatible to observation* motivated by theory (vs. ad hoc ) subdominant candidates variety is common in Nature may be easier to detect

18 The first place to look for a DM candidate

19 The most trivial solution! We know that neutrinos have mass and that a lot of them should be around us in a neutrino background neutrinos are relativistic at decoupling (hot) so their density is easy to calculate. In fact, one simply has: i.e. the comoving density today is the same as at decoupling. The latter happens at T~MeV when: (particles in equilibrium are photons, neutrinos, electrons and positrons) so that:

20 while: ( ) with g=2. So today s energy density of massive light neutrinos is given by: with: and so: ( )

21 Combining everything together: Easy! as we will see when the particle is non relativistic at decoupling the final result will depend on the details of the decoupling process (microphysics) and is more involved, sometimes MUCH MORE

22 Neutrino Σm v <0.66 ev (WMAP+LSS+SN) LEP: N ν =2.994±0.012 m ν 45 GeV Ω ν h DM searches exclude: 10 GeV m ν 4.7 TeV (similar constraints for sneutrinos and KK-neutrinos) does not work Ω 2 mν νh = 2 1 Ωνh < σannv> HOT 30 ev 91.5 ev Cowsik-McClelland COLD Lee-Weinberg 3 7 GeV mix with sterile component (both for neutrinos and sneutrinos)

23

24 2 early bounds on neutrino mass from cosmology (relic abundance): Cowsik-McClelland bound: m ν < few ev Lee-Weinberg limit: m ν >few GeV

25 Pioneering work on direct DM Homestake mine in late 80s: few GeV<M<few TeV excluded both for neutrinos ad sneutrinos* however, today the sneutrino is not completely dead (rescaling due to relic density not applied to the signal at the time, see later)

26 Neutrinos don t s work also because they are hot dark matter (=relativistic at decoupling, erase density perturbation through free-streaming): density fraction of light neutrinos (from Mark Tegmark home page)

27

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

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 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 information

Brief Introduction to Cosmology

Brief 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 information

Dark Matter. Jaan Einasto Tartu Observatory and ICRANet 16 December Saturday, December 15, 12

Dark Matter. Jaan Einasto Tartu Observatory and ICRANet 16 December Saturday, December 15, 12 Dark Matter Jaan Einasto Tartu Observatory and ICRANet 16 December 2012 Local Dark Matter: invisible matter in the Galaxy in Solar vicinity Global Dark Matter: invisible matter surrounding galaxies Global

More information

Today. Last homework Due next time FINAL EXAM: 8:00 AM TUE Dec. 14 Course Evaluations Open. Modern Cosmology. Big Bang Nucleosynthesis.

Today. 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 information

Decaying Dark Matter, Bulk Viscosity, and Dark Energy

Decaying Dark Matter, Bulk Viscosity, and Dark Energy Decaying Dark Matter, Bulk Viscosity, and Dark Energy Dallas, SMU; April 5, 2010 Outline Outline Standard Views Dark Matter Standard Views of Dark Energy Alternative Views of Dark Energy/Dark Matter Dark

More information

Dark Matter and Dark Energy components chapter 7

Dark Matter and Dark Energy components chapter 7 Dark Matter and Dark Energy components chapter 7 Lecture 3 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,

More information

INTRODUCTION TO DARK MATTER

INTRODUCTION TO DARK MATTER Universität Heidelberg Carl Zeiss Stiftung INTRODUCTION TO DARK MATTER Susanne Westhoff 2nd Colima Winter School on High Energy hysics! January 8-19, 2018 Colima, Mexico GALAXY VELOCITIES IN CLUSTERS Redshift

More information

DARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1

DARK 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 information

A5682: Introduction to Cosmology Course Notes. 12. Dark Matter and Structure Formation

A5682: Introduction to Cosmology Course Notes. 12. Dark Matter and Structure Formation 12. Dark Matter and Structure Formation Reading: Chapter 7 on dark matter. Chapter 11 on structure formation, but don t sweat the mathematical details; we will not have time to cover this material at the

More information

Dark Matter & Dark Energy. Astronomy 1101

Dark 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 information

Project Paper May 13, A Selection of Dark Matter Candidates

Project 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 information

Cosmology: Building the Universe.

Cosmology: 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 information

Components of Galaxies: Dark Matter

Components 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 information

Current status of the ΛCDM structure formation model. Simon White Max Planck Institut für Astrophysik

Current status of the ΛCDM structure formation model. Simon White Max Planck Institut für Astrophysik Current status of the ΛCDM structure formation model Simon White Max Planck Institut für Astrophysik The idea that DM might be a neutral, weakly interacting particle took off around 1980, following a measurement

More information

Astr 102: Introduction to Astronomy. Lecture 16: Cosmic Microwave Background and other evidence for the Big Bang

Astr 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 information

Ta-Pei Cheng PCNY 9/16/2011

Ta-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 information

ASTR 101 General Astronomy: Stars & Galaxies

ASTR 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 information

IoP. An Introduction to the Science of Cosmology. Derek Raine. Ted Thomas. Series in Astronomy and Astrophysics

IoP. An Introduction to the Science of Cosmology. Derek Raine. Ted Thomas. Series in Astronomy and Astrophysics Series in Astronomy and Astrophysics An Introduction to the Science of Cosmology Derek Raine Department of Physics and Astronomy University of Leicester, UK Ted Thomas Department of Physics and Astronomy

More information

Hubble'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.

Hubble'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 information

Astro 406 Lecture 25 Oct. 25, 2013

Astro 406 Lecture 25 Oct. 25, 2013 Astro 406 Lecture 25 Oct. 25, 2013 Announcements: PS 7 due now PS 8 due next Friday ASTR 401: draft due next Monday thanks to the Planetarium-goers alternate makeup activity posted soon Next semester:

More information

Cosmologists dedicate a great deal of effort to determine the density of matter in the universe. Type Ia supernovae observations are consistent with

Cosmologists 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 information

The 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?) 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 information

Astro-2: History of the Universe. Lecture 5; April

Astro-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 information

n=0 l (cos θ) (3) C l a lm 2 (4)

n=0 l (cos θ) (3) C l a lm 2 (4) Cosmic Concordance What does the power spectrum of the CMB tell us about the universe? For that matter, what is a power spectrum? In this lecture we will examine the current data and show that we now have

More information

Modern Physics notes Spring 2005 Paul Fendley Lecture 38

Modern Physics notes Spring 2005 Paul Fendley Lecture 38 Modern Physics notes Spring 2005 Paul Fendley fendley@virginia.edu Lecture 38 Dark matter and energy Cosmic Microwave Background Weinberg, chapters II and III cosmological parameters: Tegmark et al, http://arxiv.org/abs/astro-ph/0310723

More information

Dark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab

Dark 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 information

Concordance Cosmology and Particle Physics. Richard Easther (Yale University)

Concordance Cosmology and Particle Physics. Richard Easther (Yale University) Concordance Cosmology and Particle Physics Richard Easther (Yale University) Concordance Cosmology The standard model for cosmology Simplest model that fits the data Smallest number of free parameters

More information

Dark Energy vs. Dark Matter: Towards a unifying scalar field?

Dark Energy vs. Dark Matter: Towards a unifying scalar field? Dark Energy vs. Dark Matter: Towards a unifying scalar field? Alexandre ARBEY Centre de Recherche Astrophysique de Lyon Institut de Physique Nucléaire de Lyon, March 2nd, 2007. Introduction The Dark Stuff

More information

Galaxies 626. Lecture 3: From the CMBR to the first star

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

More information

Dark matter: evidence and candidates

Dark matter: evidence and candidates .... Dark matter: evidence and candidates Zhao-Huan Yu ( 余钊焕 ) Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, CAS March 14, 2014 Zhao-Huan Yu (IHEP) Dark matter: evidence and

More information

The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004

The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004 The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004 The history of modern cosmology 1917 Static via cosmological constant? (Einstein) 1917 Expansion (Slipher) 1952 Big Bang criticism (Hoyle)

More information

Lecture 19 Nuclear Astrophysics. Baryons, Dark Matter, Dark Energy. Experimental Nuclear Physics PHYS 741

Lecture 19 Nuclear Astrophysics. Baryons, Dark Matter, Dark Energy. Experimental Nuclear Physics PHYS 741 Lecture 19 Nuclear Astrophysics Baryons, Dark Matter, Dark Energy Experimental Nuclear Physics PHYS 741 heeger@wisc.edu References and Figures from: - Haxton, Nuclear Astrophysics - Basdevant, Fundamentals

More information

You may not start to read the questions printed on the subsequent pages until instructed to do so by the Invigilator.

You may not start to read the questions printed on the subsequent pages until instructed to do so by the Invigilator. MATHEMATICAL TRIPOS Part III Friday 8 June 2001 1.30 to 4.30 PAPER 41 PHYSICAL COSMOLOGY Answer any THREE questions. The questions carry equal weight. You may not start to read the questions printed on

More information

Cosmology II: The thermal history of the Universe

Cosmology II: The thermal history of the Universe .. Cosmology II: The thermal history of the Universe Ruth Durrer Département de Physique Théorique et CAP Université de Genève Suisse August 6, 2014 Ruth Durrer (Université de Genève) Cosmology II August

More information

Phys/Astro 689: Lecture 1. Evidence for Dark Matter

Phys/Astro 689: Lecture 1. Evidence for Dark Matter Phys/Astro 689: Lecture 1 Evidence for Dark Matter Why? This class is primarily a consideration of whether Cold Dark Matter theory can be reconciled with galaxy observations. Spoiler: CDM has a small scale

More information

Study Guide for ISP205 Final

Study Guide for ISP205 Final Study Guide for ISP205 Final The final will be 2/3 over the material since midterm 3, to the same level of detail as the midterms. The other 1/3 will be over the material covered on the midterms, mostly

More information

Isotropy and Homogeneity

Isotropy and Homogeneity Cosmic inventory Isotropy and Homogeneity On large scales the Universe is isotropic (looks the same in all directions) and homogeneity (the same average density at all locations. This is determined from

More information

The Early Universe: A Journey into the Past

The 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 information

Evidence for Dark Matter

Evidence for Dark Matter Evidence for Dark Matter We are now going to move on to another of the most important current mysteries in cosmology: dark matter. To set the stage, we will take a census of the mass in the universe, and

More information

The Early Universe: A Journey into the Past

The 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 information

Announcements. Homework. Set 8now open. due late at night Friday, Dec 10 (3AM Saturday Nov. 11) Set 7 answers on course web site.

Announcements. Homework. Set 8now open. due late at night Friday, Dec 10 (3AM Saturday Nov. 11) Set 7 answers on course web site. Homework. Set 8now. due late at night Friday, Dec 10 (3AM Saturday Nov. 11) Set 7 answers on course web site. Review for Final. In class on Thursday. Course Evaluation. https://rateyourclass.msu.edu /

More information

Lab Monday optional: review for Quiz 3. Lab Tuesday optional: review for Quiz 3.

Lab 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 information

Modern Cosmology Solutions 4: LCDM Universe

Modern Cosmology Solutions 4: LCDM Universe Modern Cosmology Solutions 4: LCDM Universe Max Camenzind October 29, 200. LCDM Models The ansatz solves the Friedmann equation, since ȧ = C cosh() Ωm sinh /3 H 0 () () ȧ 2 = C 2 cosh2 () sinh 2/3 () (

More information

Direct Search for Dark Matter

Direct Search for Dark Matter Direct Search for Dark Matter Herbstschule für Hochenergiephysik Maria Laach 2013, September 2013 Institut für Kernphysik, Westfälische Wilhelms-Universität Münster weinheimer@uni-muenster.de - Astrophysical

More information

OBSERVATIONAL 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) 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 information

3 The lives of galaxies

3 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 information

Implications of the Hubble Law: - it is not static, unchanging - Universe had a beginning!! - could not have been expanding forever HUBBLE LAW:

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 information

Cosmology 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 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 information

The 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 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 information

Large Scale Structure After these lectures, you should be able to: Describe the matter power spectrum Explain how and why the peak position depends on

Large Scale Structure After these lectures, you should be able to: Describe the matter power spectrum Explain how and why the peak position depends on Observational cosmology: Large scale structure Filipe B. Abdalla Kathleen Lonsdale Building G.22 http://zuserver2.star.ucl.ac.uk/~hiranya/phas3136/phas3136 Large Scale Structure After these lectures, you

More information

Dark matter and galaxy formation

Dark matter and galaxy formation Dark matter and galaxy formation Galaxy rotation The virial theorem Galaxy masses via K3 Mass-to-light ratios Rotation curves Milky Way Nearby galaxies Dark matter Baryonic or non-baryonic A problem with

More information

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. 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 information

Astro-2: History of the Universe

Astro-2: History of the Universe Astro-2: History of the Universe Lecture 8; May 7 2013 Previously on astro-2 Wherever we look in the sky there is a background of microwaves, the CMB. The CMB is very close to isotropic better than 0.001%

More information

Lecture 37 Cosmology [not on exam] January 16b, 2014

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

More information

AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation!

AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation! AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation! Bring pencil #2 with eraser No use of calculator or any electronic device during the exam We provide the scantrons

More information

The 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 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 information

Cosmological Constraints on Dark Energy via Bulk Viscosity from Decaying Dark Matter

Cosmological Constraints on Dark Energy via Bulk Viscosity from Decaying Dark Matter Cosmological Constraints on Dark Energy via Bulk Viscosity from Decaying Dark Matter Nguyen Quynh Lan Hanoi National University of Education, Vietnam (University of Notre Dame, USA) Rencontres du Vietnam:

More information

Today: 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) 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 information

ASTR 1120 General Astronomy: Stars & Galaxies. OUR Universe: Accelerating Universe

ASTR 1120 General Astronomy: Stars & Galaxies. OUR Universe: Accelerating Universe ASTR 1120 General Astronomy: Stars & Galaxies FINAL: Saturday, Dec 12th, 7:30pm, HERE ALTERNATE FINAL: Monday, Dec 7th, 5:30pm in Muenzinger E131 Last OBSERVING session, Tue, Dec.8th, 7pm Please check

More information

1920s 1990s (from Friedmann to Freedman)

1920s 1990s (from Friedmann to Freedman) 20 th century cosmology 1920s 1990s (from Friedmann to Freedman) theoretical technology available, but no data 20 th century: birth of observational cosmology Hubble s law ~1930 Development of astrophysics

More information

Dark Matter: Finding the Invisible

Dark 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 information

Nucleosíntesis primordial

Nucleosíntesis primordial Tema 5 Nucleosíntesis primordial Asignatura de Física Nuclear Curso académico 2009/2010 Universidad de Santiago de Compostela Big Bang cosmology 1.1 The Universe today The present state of the Universe

More information

VU lecture Introduction to Particle Physics. Thomas Gajdosik, FI & VU. Big Bang (model)

VU lecture Introduction to Particle Physics. Thomas Gajdosik, FI & VU. Big Bang (model) Big Bang (model) What can be seen / measured? basically only light _ (and a few particles: e ±, p, p, ν x ) in different wave lengths: microwave to γ-rays in different intensities (measured in magnitudes)

More information

Lecture 03. The Cosmic Microwave Background

Lecture 03. The Cosmic Microwave Background The Cosmic Microwave Background 1 Photons and Charge Remember the lectures on particle physics Photons are the bosons that transmit EM force Charged particles interact by exchanging photons But since they

More information

FURTHER 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 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 information

Weighing the universe : baryons, dark matter, and dark energy

Weighing the universe : baryons, dark matter, and dark energy Weighing the universe : baryons, dark matter, and dark energy Department of Physics The University of Tokyo Yasushi Suto The 21 st century COE program of Tohoku University International symposium Exploring

More information

The Expanding Universe

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 information

Cosmology. Clusters of galaxies. Redshift. Late 1920 s: Hubble plots distances versus velocities of galaxies. λ λ. redshift =

Cosmology. 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 information

Dark Matter / Dark Energy

Dark Matter / Dark Energy Dark Matter / Dark Energy 2 different things! The first hints of Dark Matter arose with observations of large motions in clusters of galaxies in the 1930 s. The case became compelling in the 1970 s with

More information

Outline. Walls, Filaments, Voids. Cosmic epochs. Jeans length I. Jeans length II. Cosmology AS7009, 2008 Lecture 10. λ =

Outline. Walls, Filaments, Voids. Cosmic epochs. Jeans length I. Jeans length II. Cosmology AS7009, 2008 Lecture 10. λ = Cosmology AS7009, 2008 Lecture 10 Outline Structure formation Jeans length, Jeans mass Structure formation with and without dark matter Cold versus hot dark matter Dissipation The matter power spectrum

More information

We can check experimentally that physical constants such as α have been sensibly constant for the past ~12 billion years

We can check experimentally that physical constants such as α have been sensibly constant for the past ~12 billion years ² ² ² The universe observed ² Relativistic world models ² Reconstructing the thermal history ² Big bang nucleosynthesis ² Dark matter: astrophysical observations ² Dark matter: relic particles ² Dark matter:

More information

3. It is expanding: the galaxies are moving apart, accelerating slightly The mystery of Dark Energy

3. 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 information

Final Exam Study Guide

Final 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 information

Figure 1: The universe in a pie chart [1]

Figure 1: The universe in a pie chart [1] Dark matter Marlene Götz (Jena) Dark matter is a hypothetical form of matter. It has to be postulated to describe phenomenons, which could not be explained by known forms of matter. It has to be assumed

More information

3/6/12! Astro 358/Spring 2012! Galaxies and the Universe! Dark Matter in Spiral Galaxies. Dark Matter in Galaxies!

3/6/12! Astro 358/Spring 2012! Galaxies and the Universe! Dark Matter in Spiral Galaxies. Dark Matter in Galaxies! 3/6/12 Astro 358/Spring 2012 Galaxies and the Universe Dark Matter in Galaxies Figures + Tables for Lectures (Feb 16-Mar 6) Dark Matter in Spiral Galaxies Flat rotation curve of Milky Way at large radii

More information

Lecture 12. Dark Matter. Part II What it could be and what it could do

Lecture 12. Dark Matter. Part II What it could be and what it could do Dark Matter Part II What it could be and what it could do Theories of Dark Matter What makes a good dark matter candidate? Charge/color neutral (doesn't have to be though) Heavy We know KE ~ kev CDM ~

More information

neutrinos (ν) } ν energy ~ K ν + proton e + + neutron! e - + proton neutron + ν Freeze-out temperatures

neutrinos (ν) } ν energy ~ K ν + proton e + + neutron! e - + proton neutron + ν Freeze-out temperatures kt ~ mparticle c 2 neutrinos (ν) kt < mparticle c 2 kt > mparticle c 2 Freeze-out temperatures particle /! T (K) time since BB antiparticle 6x10 e 20 sec 1.2x10 μ 1 sec 1x10 p 10 NOTE: after freeze-out,

More information

AST1100 Lecture Notes

AST1100 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 information

Chapter 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 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 information

Gravitino LSP as Dark Matter in the Constrained MSSM

Gravitino LSP as Dark Matter in the Constrained MSSM Gravitino LSP as Dark Matter in the Constrained MSSM Ki Young Choi The Dark Side of the Universe, Madrid, 20-24 June 2006 Astro-Particle Theory and Cosmology Group The University of Sheffield, UK In collaboration

More information

Dark Matter in Particle Physics

Dark 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 information

Lecture 24: Cosmology: The First Three Minutes. Astronomy 111 Monday November 27, 2017

Lecture 24: Cosmology: The First Three Minutes. Astronomy 111 Monday November 27, 2017 Lecture 24: Cosmology: The First Three Minutes Astronomy 111 Monday November 27, 2017 Reminders Last star party of the semester tomorrow night! Online homework #11 due Monday at 3pm The first three minutes

More information

Analyzing the CMB Brightness Fluctuations. Position of first peak measures curvature universe is flat

Analyzing the CMB Brightness Fluctuations. Position of first peak measures curvature universe is flat Analyzing the CMB Brightness Fluctuations (predicted) 1 st rarefaction Power = Average ( / ) 2 of clouds of given size scale 1 st compression 2 nd compression (deg) Fourier analyze WMAP image: Measures

More information

Particles in the Early Universe

Particles 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 information

Planetarium/Observing: the clock is ticking! Don t forget to fill out your Planetarium/ Observing impression online.

Planetarium/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 information

Solving small scale structure puzzles with. dissipative dark matter

Solving small scale structure puzzles with. dissipative dark matter Solving small scale structure puzzles with. dissipative dark matter Robert Foot, COEPP, University of Melbourne Okinawa, March 2016 Dark matter: why we think it exists Dark matter issues on small scales

More information

Possible sources of very energetic neutrinos. Active Galactic Nuclei

Possible sources of very energetic neutrinos. Active Galactic Nuclei Possible sources of very energetic neutrinos Active Galactic Nuclei 1 What might we learn from astrophysical neutrinos? Neutrinos not attenuated/absorbed Information about central engines of astrophysical

More information

WOLFGANG KLASSEN DARK MATTER

WOLFGANG KLASSEN DARK MATTER 1 WOLFGANG KLASSEN DARK MATTER "Hubble Maps the Cosmic Web of "Clumpy" Dark Matter in 3-D" (Press release). NASA. 7 January 2007. DARK MATTER 2 CONTENTS 1.Relating Mass and Light Tulley-Fisher relation

More information

Modern Cosmology / Scott Dodelson Contents

Modern Cosmology / Scott Dodelson Contents Modern Cosmology / Scott Dodelson Contents The Standard Model and Beyond p. 1 The Expanding Universe p. 1 The Hubble Diagram p. 7 Big Bang Nucleosynthesis p. 9 The Cosmic Microwave Background p. 13 Beyond

More information

Dark Matter and Cosmic Structure Formation

Dark Matter and Cosmic Structure Formation Dark Matter and Cosmic Structure Formation Prof. Luke A. Corwin PHYS 792 South Dakota School of Mines & Technology Jan. 23, 2014 (W2-2) L. Corwin, PHYS 792 (SDSM&T) DM & Cosmic Structure Jan. 23, 2014

More information

ASTROPHYSICAL PROPERTIES OF MIRROR DARK MATTER

ASTROPHYSICAL PROPERTIES OF MIRROR DARK MATTER 16 December 2011 ASTROPHYSICAL PROPERTIES OF MIRROR DARK MATTER Paolo Ciarcelluti Motivation of this research We are now in the ERA OF PRECISION COSMOLOGY and... Motivation of this research We are now

More information

Introduction to Cosmology

Introduction to Cosmology Introduction to Cosmology Subir Sarkar CERN Summer training Programme, 22-28 July 2008 Seeing the edge of the Universe: From speculation to science Constructing the Universe: The history of the Universe:

More information

What is the Dark Matter? William Shepherd Niels Bohr International Academy Johannes Gutenberg University Mainz

What is the Dark Matter? William Shepherd Niels Bohr International Academy Johannes Gutenberg University Mainz What is the Dark Matter? William Shepherd Niels Bohr International Academy Johannes Gutenberg University Mainz Outline Evidence for the existence of dark matter Motion of visible matter Cosmological evidence

More information

Formation of the Universe. What evidence supports current scientific theory?

Formation 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 information

Cosmology - Redshift and Radiation ASTR 2120 Sarazin

Cosmology - Redshift and Radiation ASTR 2120 Sarazin Cosmology - Redshift and Radiation ASTR 2120 Sarazin Test #1 Monday, February 26, 11-11:50 am ASTR 265 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other

More information

Cosmology. Jörn Wilms Department of Physics University of Warwick.

Cosmology. 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 information

Introduction. How did the universe evolve to what it is today?

Introduction. 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 information

Chapter 29. The Hubble Expansion

Chapter 29. The Hubble Expansion Chapter 29 The Hubble Expansion The observational characteristics of the Universe coupled with theoretical interpretation to be discussed further in subsequent chapters, allow us to formulate a standard

More information

Particle Cosmology. V.A. Rubakov. Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University

Particle Cosmology. V.A. Rubakov. Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University Particle Cosmology V.A. Rubakov Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University Topics Basics of Hot Big Bang cosmology Dark matter: WIMPs Axions Warm

More information

The Dark Matter Puzzle and a Supersymmetric Solution. Andrew Box UH Physics

The Dark Matter Puzzle and a Supersymmetric Solution. Andrew Box UH Physics The Dark Matter Puzzle and a Supersymmetric Solution Andrew Box UH Physics Outline What is the Dark Matter (DM) problem? How can we solve it? What is Supersymmetry (SUSY)? One possible SUSY solution How

More information