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

Size: px
Start display at page:

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

Transcription

1 Dark Matter Part II What it could be and what it could do

2 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 ~ GeV or heavier Non-baryonic Fall out of larger theory Natural production mechanism e.g. WIMP miracle More theories than you can count! Let's discuss a few of them 2

3 Old News: MACHOs Massive Compact Halo Objects Jupiter-like planets, brown dwarf stars Extra normal matter that doesn't emit light But MACHOs are baryons! Doesn't this disagree with WMAP? MACHO searches were conducted about the same time that the CMB measurements were made Look for MACHOs via gravitational lensing Micro-lensing of starlight from within the milky way Look for brightening of star as MACHO passes in front of it Galactic survey to look for MACHOs in the milky way Some MACHOs were found Not enough to constitute DM Consistent with WMAP result that DM is non-baryonic! 3

4 Sterile Neutrinos We know about 3 types of neutrinos Could there be a fourth type? The full answer will be discussed in neutrino lectures Short answer, yes, but it must be sterile! Doesn't participate in weak interactions Only accessible via oscillations Usually heavy (~ kev) Not quite cold, but warm DM candidate 4

5 Axions Remember CP violation? C = charge congugation P = parity (invert coordinates, like looking in mirror) CP symmetry means that under inversion of charge and parity, physics is unchanged Does an electron behave the same as a positron when viewed in a mirror? CP violation: processes which do not obey this symmetry CP violation observed in weak interactions Never observed in strong interactions But remember Noether's theorem: Symmetry Conserved quantity No such symmetry in strong interaction Strong CP problem Add axial symmetry to strong interaction Resulting particle is the axion Would solve strong CP problem Could also be DM Huge parameter space for axion coupling and mass Subset gives correct DM density ADMX Experiment Search for axion dark matter No discovery yet Not ruled out either 5

6 WIMPs Recall the WIMP Miracle Weak-scale cross section gives correct abundance Many, many theories give WIMPs Extensions to the SM often have new physics just beyond our reach Electroweak scale New particles and new interactions New forces or extensions of existing ones Natural framework for CDM Heavy (e.g. cold) particles Scaling of WIMP miracle: Relic density roughly scales with Smaller cross section but larger mass gives same relic density 6

7 SUSY Remember our old friend SUSY Doubling of SM Fermion Boson symmetry Lightest SUSY Particle (LSP) Naturally neutral Neutralino: SUSY is by far the most popular framework for physics beyond the SM, and DM A lot of flexibility Answers many shortcomings of SM By no means the only possibility for WIMP DM 7

8 Composite Dark Matter DM could be composite Made up of constituent particles Like baryons consist of quarks One example: DM consists of 4 fundamental particles Each carries both weak and electrical charge But the DM particle is electrically neutral Couples through Z, H exchange Many other models: Different numbers of constituents Different properties EM, weak, strong interactions New interactions Always globally neutral (like neutron) Come from adding a new symmetry to SM 8

9 Mirror Dark Matter Mirror copy of normal particle physics All known particles have a copy in the mirror sector Same physics in the mirror sector as normal sector The two sectors are connected by a photon mixing Consistent with WIMP miracle High density allows freezeout as with other WIMPs Mixing is small (ε ~ 10-9) Characteristics: More dynamic physics available in DM halos Bullet cluster and non-bullet cluster like collisions Dominantly an EM interaction But strongly suppressed by ε 9

10 Compact Dimensions: Kaluza Klein Particles Compact extra dimension Periodic boundary Think of a loop Compact, ~ TeV-1 (10-21 m) Quantized excitations Shows up as effective mass ~ TeV particles In Kaluza Klein theory, the lowest mode is stable Invoke a symmetry to protect KK number Orthogonality: New dimension (w) orthogonal to x, y, z Welcome to the fourth dimension 10

11 WIMP Miracle and DM Detection The WIMP Miracle predicts three types of interactions DM annihilation DM production DM scattering We look for all three experimentally! 11

12 WIMP Scattering Let's start with a few assumptions: Cold Dark Matter exists and consists of SUSY WIMPs with m ~ 100 GeV The WIMP miracle tells us DM should interact with normal matter! Our galaxy is immersed in a WIMP halo with density ~ 0.3 GeV/cm3 The WIMP velocity distribution is roughly understood (details later) WIMPs and matter have weak scale interaction How do we determine the interaction rate in a WIMP detector? We can follow general scattering theory New physics only shows up in the cross section (in most cases) We can ignore the details, and calculate the rate for a given cross section 12

13 Scattering Theory In quantum mechanics, you will study scattering theory Probability (or rate) of interaction In general, it can be written in this form Two things to deal with: Velocity integral Differential cross section R = scattering rate ρ0 = 0.3 GeV/cm3 is the local dark matter density mx and mn are the WIMP and Nucleon masses respectively v is the WIMP speed f(v) is the 1D WIMP speed distribution S is the elastic WIMP-nucleon cross section q is the momentum transfer 13

14 Some Useful Substitutions Reduced mass: Energy transferred: At low momentum transfer: σ0 is the cross section at zero momentum transfer F2(Q) is the nuclear form factor Integrating over all possible velocities, the differential rate can be written as: Three terms to deal with: Velocity integral Cross section Form factor 14

15 Details of the Velocity Minimum velocity: bound by kinematics Two cases for maximum velocity: Simple model: vmax = Realistic model: vmax = vesc WIMPs greater than vesc are not gravitationally bound Different measurements exist for the escape velocity in the Milky Way 496 < vesc < 655 km/s Earth-Sun motion: The sun moves around the galactic center at v0 = 220 km/s The earth moves with or against the sun motion Annual modulation of relative WIMP velocity distribution 15

16 Simplest Model: Ignore vesc and vearth Maxwellian distribution: Velocity integral: What does this mean for the WIMP scattering rate? Consider F2(Q) = 1 (true for light WIMPs): General feature: Exponential Energy Spectrum! This is a global feature, all additional terms only modify this slightly 16

17 More Realistic Model: Include Earth-Sun Motion Recall: The 1D Boltzmann distribution has two terms (derivable from 3D distribution) With this form and still ignoring the escape velocity, the velocity integral is: General feature: Exponential Energy Spectrum! This is a global feature, all additional terms only modify this slightly 17

18 The Full Solution Re-evaluating the previous integral with finite vesc And the differential rate can be written as: vmin is a function of Q ve is a function of cos(t) 18

19 Features of the Velocity Integral Exponential behavior predicts high rate at low recoil energy Experiments must be sensitive to few kev Earth-Sun motion creates modulation in rate Modulation in total number of events May ultimately allow for probing our own DM Halo Escape velocity truncates rate at high E More complicated velocity distributions can be considered (streamers, motion or structure in Halo, etc) 19

20 Form Factor Describes how a wave overlaps with nuclear structure How much nuclear structure do you see Recall the DeBroglie wavelength Long wavelength sees nucleus as one blob Short wavelength resolves nuclear sub-structure 20

21 Computing the Form Factor The nuclear form factor is the Fourier transform of the matter density in the nucleus Need to know matter density inside nucleus Nuclear physics Many different form factors used Most agree to a large extent 21

22 Example of Form Factor Woods-Saxon form factor Treat the nucleus as a hard, uniform sphere, but with blurry edges j1(x) is a spherical bessel function q is the momentum transfer R1 is related to the nuclear radius R s is the skin depth of the nuclear edge 22

23 Features of the Form Factor Suppresses high momentum exchange Poles at certain momentum exchange: Destructive interference Form factor 0 Rate 0 Goes to 1 as q goes to 0 No effect when no resolution of nuclear structure! 23

24 Cross Section The cross section at zero momentum transfer is: # protons # neutrons Proton coupling Neutron coupling Let's make an assumption: fp = fn Maybe that's not too crazy, we're looking for SUSY WIMPs Ignoring form factor effects, the rate should scale with A

25 The Final Event Rate Plugging in all the numbers, one gets a differential rate for each WIMP mass, cross section and target material Features of this plot: Differential Rate Unit (dru) Events / kg / kev / day A2 dependence Heavy target is better (at low E) Form factor large nucleus has pole at low E Incredibly low rate! (few events / year) experimental challenge Mχ = 100 GeV, σ = cm2 25

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

Kaluza-Klein Dark Matter

Kaluza-Klein Dark Matter Kaluza-Klein Dark Matter Hsin-Chia Cheng UC Davis Pre-SUSY06 Workshop Complementary between Dark Matter Searches and Collider Experiments Introduction Dark matter is the best evidence for physics beyond

More information

Lecture 03. The Standard Model of Particle Physics. Part III Extensions of the Standard Model

Lecture 03. The Standard Model of Particle Physics. Part III Extensions of the Standard Model Lecture 03 The Standard Model of Particle Physics Part III Extensions of the Standard Model Where the SM Works Excellent description of 3 of the 4 fundamental forces Explains nuclear structure, quark confinement,

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

2. The evolution and structure of the universe is governed by General Relativity (GR).

2. 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 information

Overview of Dark Matter models. Kai Schmidt-Hoberg

Overview 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 information

PHY323:Lecture 11 SUSY and UED Higgs and Supersymmetry The Neutralino Extra Dimensions How WIMPs interact

PHY323:Lecture 11 SUSY and UED Higgs and Supersymmetry The Neutralino Extra Dimensions How WIMPs interact PHY323:Lecture 11 SUSY and UED Higgs and Supersymmetry The Neutralino Extra Dimensions How WIMPs interact Candidates for Dark Matter III The New Particle Zoo Here are a few of the candidates on a plot

More information

The Search for Dark Matter. Jim Musser

The 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 information

November 24, Scalar Dark Matter from Grand Unified Theories. T. Daniel Brennan. Standard Model. Dark Matter. GUTs. Babu- Mohapatra Model

November 24, Scalar Dark Matter from Grand Unified Theories. T. Daniel Brennan. Standard Model. Dark Matter. GUTs. Babu- Mohapatra Model Scalar from November 24, 2014 1 2 3 4 5 What is the? Gauge theory that explains strong weak, and electromagnetic forces SU(3) C SU(2) W U(1) Y Each generation (3) has 2 quark flavors (each comes in one

More information

The Story of Wino Dark matter

The Story of Wino Dark matter The Story of Wino Dark matter Varun Vaidya Dept. of Physics, CMU DIS 2015 Based on the work with M. Baumgart and I. Rothstein, 1409.4415 (PRL) & 1412.8698 (JHEP) Evidence for dark matter Rotation curves

More information

LHC searches for dark matter.! Uli Haisch

LHC searches for dark matter.! Uli Haisch LHC searches for dark matter! Uli Haisch Evidence for dark matter Velocity Observed / 1 p r Disk 10 5 ly Radius Galaxy rotation curves Evidence for dark matter Bullet cluster Mass density contours 10 7

More information

It is possible for a couple of elliptical galaxies to collide and become a spiral and for two spiral galaxies to collide and form an elliptical.

It is possible for a couple of elliptical galaxies to collide and become a spiral and for two spiral galaxies to collide and form an elliptical. 7/16 Ellipticals: 1. Very little gas and dust an no star formation. 2. Composed of old stars. 3. Masses range from hundreds of thousands to 10's of trillions of solar masses. 4. Sizes range from 3000 ly

More information

Lecture 14. Dark Matter. Part IV Indirect Detection Methods

Lecture 14. Dark Matter. Part IV Indirect Detection Methods Dark Matter Part IV Indirect Detection Methods WIMP Miracle Again Weak scale cross section Produces the correct relic abundance Three interactions possible with DM and normal matter DM Production DM Annihilation

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

PHY326/426:Lecture 11

PHY326/426:Lecture 11 PHY326/426:Lecture 11 Towards WIMP direct detection WIMP Cross Sections and Recoil Rates (1) Introduction to SUSY dark matter WIMP-nucleon collision kinematics Recoil energy in the CM frame Probability

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

Dark Matter Searches. Marijke Haffke University of Zürich

Dark 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 information

Development of a New Paradigm

Development of a New Paradigm P599 Seminar, April 9, 2014 Development of a New Paradigm for Direct Dark Matter Detection Jason Rose / UTK (working with Dr. Kamyshkov) Dark Matter Recap Evidence: Galactic Rotation Curves Gravitational

More information

Week 3 - Part 2 Recombination and Dark Matter. Joel Primack

Week 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 information

Collider Searches for Dark Matter

Collider Searches for Dark Matter Collider Searches for Dark Matter AMELIA BRENNAN COEPP-CAASTRO WORKSHOP 1 ST MARCH 2013 Introduction Enough introductions to dark matter (see yesterday) Even though we don t know if DM interacts with SM,

More information

Chapter 12. Dark Matter

Chapter 12. Dark Matter Karl-Heinz Kampert Univ. Wuppertal 128 Chapter 12 Dark Matter Karl-Heinz Kampert Univ. Wuppertal Baryonic Dark Matter Brightness & Rotation Curve of NGC3198 Brightness Rotation Curve measured expected

More information

Made of? What is the Universe. What is the Universe made of? Made of? We are stardust!!! Element Abundances

Made of? What is the Universe. What is the Universe made of? Made of? We are stardust!!! Element Abundances Made of? Dr Risa H Wechsler Hubble Fellow" Enrico Fermi Fellow University of Chicago Lecture Plan Lecture Two" April #& The Story of Galaxy Formation in Our Universe: Kavli Inst for Cosmological Physics"

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

COLD DARK MATTER DETECTION VIA THE LSP-NUCLEUS ELASTIC SCATTERING 1

COLD DARK MATTER DETECTION VIA THE LSP-NUCLEUS ELASTIC SCATTERING 1 COLD DARK MATTER DETECTION VIA THE LSP-NUCLEUS ELASTIC SCATTERING 1 J.D. VERGADOS and T.S. KOSMAS Theoretical Physics Section, University of Ioannina, GR 451 1, Greece Abstract The momentum transfer dependence

More information

components Particle Astrophysics, chapter 7

components Particle Astrophysics, chapter 7 Dark matter and dark energy components Particle Astrophysics, chapter 7 Overview lecture 3 Observation of dark matter as gravitational ti effects Rotation curves galaxies, mass/light ratios in galaxies

More information

MICROPHYSICS AND THE DARK UNIVERSE

MICROPHYSICS AND THE DARK UNIVERSE MICROPHYSICS AND THE DARK UNIVERSE Jonathan Feng University of California, Irvine CAP Congress 20 June 2007 20 June 07 Feng 1 WHAT IS THE UNIVERSE MADE OF? Recently there have been remarkable advances

More information

Astronomy 182: Origin and Evolution of the Universe

Astronomy 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 information

Dark matter: summary

Dark 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 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

Dark 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) 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 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

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

Beyond the standard model? From last time. What does the SM say? Grand Unified Theories. Unifications: now and the future

Beyond the standard model? From last time. What does the SM say? Grand Unified Theories. Unifications: now and the future From last time Quantum field theory is a relativistic quantum theory of fields and interactions. Fermions make up matter, and bosons mediate the forces by particle exchange. Lots of particles, lots of

More information

Dark matter in split extended supersymmetry

Dark matter in split extended supersymmetry Dark matter in split extended supersymmetry Vienna 2 nd December 2006 Alessio Provenza (SISSA/ISAS) based on AP, M. Quiros (IFAE) and P. Ullio (SISSA/ISAS) hep ph/0609059 Dark matter: experimental clues

More information

The Standard Model of particle physics and beyond

The Standard Model of particle physics and beyond The Standard Model of particle physics and beyond - Lecture 3: Beyond the Standard Model Avelino Vicente IFIC CSIC / U. Valencia Physics and astrophysics of cosmic rays in space Milano September 2016 1

More information

IMPLICATIONS OF PARTICLE PHYSICS FOR COSMOLOGY

IMPLICATIONS OF PARTICLE PHYSICS FOR COSMOLOGY IMPLICATIONS OF PARTICLE PHYSICS FOR COSMOLOGY Jonathan Feng University of California, Irvine 28-29 July 2005 PiTP, IAS, Princeton 28-29 July 05 Feng 1 Graphic: N. Graf OVERVIEW This Program anticipates

More information

Distinguishing Dark Matter Candidates from Direct Detection Experiments

Distinguishing Dark Matter Candidates from Direct Detection Experiments Distinguishing Dark Matter Candidates from Direct Detection Experiments Chung-Lin Shan Department of Physics, National Cheng Kung University International Workshop on DM, DE and Matter-Antimatter Asymmetry

More information

Dennis 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 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 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

WIMPs and superwimps. Jonathan Feng UC Irvine. MIT Particle Theory Seminar 17 March 2003

WIMPs and superwimps. Jonathan Feng UC Irvine. MIT Particle Theory Seminar 17 March 2003 WIMPs and superwimps Jonathan Feng UC Irvine MIT Particle Theory Seminar 17 March 2003 Dark Matter The dawn (mid-morning?) of precision cosmology: Ω DM = 0.23 ± 0.04 Ω total = 1.02 ± 0.02 Ω baryon = 0.044

More information

Lecture 03. The Standard Model of Particle Physics. Part II The Higgs Boson Properties of the SM

Lecture 03. The Standard Model of Particle Physics. Part II The Higgs Boson Properties of the SM Lecture 03 The Standard Model of Particle Physics Part II The Higgs Boson Properties of the SM The Standard Model So far we talked about all the particles except the Higgs If we know what the particles

More information

The Yang and Yin of Neutrinos

The Yang and Yin of Neutrinos The Yang and Yin of Neutrinos Ernest Ma Physics and Astronomy Department University of California Riverside, CA 92521, USA The Yang and Yin of Neutrinos (2018) back to start 1 Contents Introduction The

More information

M. Lattanzi. 12 th Marcel Grossmann Meeting Paris, 17 July 2009

M. Lattanzi. 12 th Marcel Grossmann Meeting Paris, 17 July 2009 M. Lattanzi ICRA and Dip. di Fisica - Università di Roma La Sapienza In collaboration with L. Pieri (IAP, Paris) and J. Silk (Oxford) Based on ML, Silk, PRD 79, 083523 (2009) and Pieri, ML, Silk, MNRAS

More information

Dark Side of the Universe

Dark 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 information

The Dark Matter Problem

The Dark Matter Problem 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

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

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

The Mystery of Dark Matter

The Mystery of Dark Matter The Mystery of Dark Matter Maxim Perelstein, LEPP/Cornell U. CIPT Fall Workshop, Ithaca NY, September 28 2013 Introduction Last Fall workshop focused on physics of the very small - elementary particles

More information

Signatures of clumpy dark matter in the global 21 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:

Signatures of clumpy dark matter in the global 21 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv: Signatures of clumpy dark matter in the global 2 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:0808.088 Daniel Grin Ay. Journal Club /23/2009 /8 Signatures of clumpy dark matter in

More information

The Search for Dark Matter, and Xenon1TP

The 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 information

Inert Doublet Model and DAMA:

Inert Doublet Model and DAMA: Inert Doublet Model and DAMA: elastic and/or inelastic Dark Matter candidates C.A., FS. Ling, M.H.G. Tytgat arxiv:0907.0430 Chiara Arina TAUP 2009 - July 1/5 Service de Physique Theorique 1 Universite

More information

Searching for sneutrinos at the bottom of the MSSM spectrum

Searching for sneutrinos at the bottom of the MSSM spectrum Searching for sneutrinos at the bottom of the MSSM spectrum Arindam Chatterjee Harish-Chandra Research Insitute, Allahabad In collaboration with Narendra Sahu; Nabarun Chakraborty, Biswarup Mukhopadhyay

More information

Dark Matter WIMP and SuperWIMP

Dark Matter WIMP and SuperWIMP Dark Matter WIMP and SuperWIMP Shufang Su U. of Arizona S. Su Dark Matters Outline Dark matter evidence New physics and dark matter WIMP candidates: neutralino LSP in MSSM direct/indirect DM searches,

More information

The Building Blocks of Nature

The Building Blocks of Nature The Building Blocks of Nature PCES 15.1 Schematic picture of constituents of an atom, & rough length scales. The size quoted for the nucleus here (10-14 m) is too large- a single nucleon has size 10-15

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

Overview. The quest of Particle Physics research is to understand the fundamental particles of nature and their interactions.

Overview. The quest of Particle Physics research is to understand the fundamental particles of nature and their interactions. Overview The quest of Particle Physics research is to understand the fundamental particles of nature and their interactions. Our understanding is about to take a giant leap.. the Large Hadron Collider

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

Particle Physics Lecture 1 : Introduction Fall 2015 Seon-Hee Seo

Particle Physics Lecture 1 : Introduction Fall 2015 Seon-Hee Seo Particle Physics Lecture 1 : Introduction Fall 2015 Seon-Hee Seo Particle Physics Fall 2015 1 Course Overview Lecture 1: Introduction, Decay Rates and Cross Sections Lecture 2: The Dirac Equation and Spin

More information

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

THE DARK UNIVERSE. Jonathan Feng Department of Physics and Astronomy. UCI Distinguished Faculty Lecture 26 October 2004

THE DARK UNIVERSE. Jonathan Feng Department of Physics and Astronomy. UCI Distinguished Faculty Lecture 26 October 2004 THE DARK UNIVERSE Jonathan Feng Department of Physics and Astronomy UCI Distinguished Faculty Lecture 26 October 2004 What is the universe made of? An age old question, but we live at a particularly interesting

More information

Dark Matter Decay and Cosmic Rays

Dark Matter Decay and Cosmic Rays Dark Matter Decay and Cosmic Rays Christoph Weniger Deutsches Elektronen Synchrotron DESY in collaboration with A. Ibarra, A. Ringwald and D. Tran see arxiv:0903.3625 (accepted by JCAP) and arxiv:0906.1571

More information

Whither WIMP Dark Matter Search? Pijushpani Bhattacharjee AstroParticle Physics & Cosmology Division Saha Institute of Nuclear Physics Kolkata

Whither WIMP Dark Matter Search? Pijushpani Bhattacharjee AstroParticle Physics & Cosmology Division Saha Institute of Nuclear Physics Kolkata Whither WIMP Dark Matter Search? AstroParticle Physics & Cosmology Division Saha Institute of Nuclear Physics Kolkata 1/51 2/51 Planck 2015 Parameters of the Universe 3/51 Discovery of Dark Matter Fritz

More information

DARK MATTERS. Jonathan Feng University of California, Irvine. 2 June 2005 UCSC Colloquium

DARK MATTERS. Jonathan Feng University of California, Irvine. 2 June 2005 UCSC Colloquium DARK MATTERS Jonathan Feng University of California, Irvine 2 June 2005 UCSC Colloquium 2 June 05 Graphic: Feng N. Graf 1 WHAT IS THE UNIVERSE MADE OF? An age old question, but Recently there have been

More information

Thermal decoupling of WIMPs

Thermal decoupling of WIMPs PPC 2010, Torino, 12-15 July 2010 A link between particle physics properties and the small-scale structure of (dark) matter Outlook Chemical vs kinetic decoupling of WIMPs Kinetic decoupling from first

More information

DARK MATTER MEETS THE SUSY FLAVOR PROBLEM

DARK MATTER MEETS THE SUSY FLAVOR PROBLEM DARK MATTER MEETS THE SUSY FLAVOR PROBLEM Work with Manoj Kaplinghat, Jason Kumar, John Learned, Arvind Rajaraman, Louie Strigari, Fumihiro Takayama, Huitzu Tu, Haibo Yu Jonathan Feng University of California,

More information

Cosmological Constraint on the Minimal Universal Extra Dimension Model

Cosmological Constraint on the Minimal Universal Extra Dimension Model Cosmological Constraint on the Minimal Universal Extra Dimension Model Mitsuru Kakizaki (Bonn University) September 7, 2007 @ KIAS In collaboration with Shigeki Matsumoto (Tohoku Univ.) Yoshio Sato (Saitama

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 4 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

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

Outline. Charged Leptonic Weak Interaction. Charged Weak Interactions of Quarks. Neutral Weak Interaction. Electroweak Unification

Outline. Charged Leptonic Weak Interaction. Charged Weak Interactions of Quarks. Neutral Weak Interaction. Electroweak Unification Weak Interactions Outline Charged Leptonic Weak Interaction Decay of the Muon Decay of the Neutron Decay of the Pion Charged Weak Interactions of Quarks Cabibbo-GIM Mechanism Cabibbo-Kobayashi-Maskawa

More information

The Linear Collider and the Preposterous Universe

The Linear Collider and the Preposterous Universe The Linear Collider and the Preposterous Universe Sean Carroll, University of Chicago 5% Ordinary Matter 25% Dark Matter 70% Dark Energy Why do these components dominate our universe? Would an Apollonian

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

Origin of the Universe - 2 ASTR 2120 Sarazin. What does it all mean?

Origin of the Universe - 2 ASTR 2120 Sarazin. What does it all mean? Origin of the Universe - 2 ASTR 2120 Sarazin What does it all mean? Fundamental Questions in Cosmology 1. Why did the Big Bang occur? 2. Why is the Universe old? 3. Why is the Universe made of matter?

More information

The first one second of the early universe and physics beyond the Standard Model

The first one second of the early universe and physics beyond the Standard Model The first one second of the early universe and physics beyond the Standard Model Koichi Hamaguchi (University of Tokyo) @ Colloquium at Yonsei University, November 9th, 2016. Credit: X-ray: NASA/CXC/CfA/M.Markevitch

More information

WIMP Velocity Distribution and Mass from Direct Detection Experiments

WIMP Velocity Distribution and Mass from Direct Detection Experiments WIMP Velocity Distribution and Mass from Direct Detection Experiments Manuel Drees Bonn University WIMP Distribution and Mass p. 1/33 Contents 1 Introduction WIMP Distribution and Mass p. 2/33 Contents

More information

Discovery Physics at the Large Hadron Collider

Discovery Physics at the Large Hadron Collider + / 2 GeV N evt 4 10 3 10 2 10 CMS 2010 Preliminary s=7 TeV -1 L dt = 35 pb R > 0.15 R > 0.20 R > 0.25 R > 0.30 R > 0.35 R > 0.40 R > 0.45 R > 0.50 10 1 100 150 200 250 300 350 400 [GeV] M R Discovery

More information

Solar and atmospheric neutrinos as background for direct dark matter searches

Solar and atmospheric neutrinos as background for direct dark matter searches Solar and atmospheric neutrinos as background for direct dark matter searches Achim Gütlein TU-München Joined seminar on neutrinos and dark matter.0.0 utline Direct Dark Matter Search eutrinos as background

More information

1 Introduction. 1.1 The Standard Model of particle physics The fundamental particles

1 Introduction. 1.1 The Standard Model of particle physics The fundamental particles 1 Introduction The purpose of this chapter is to provide a brief introduction to the Standard Model of particle physics. In particular, it gives an overview of the fundamental particles and the relationship

More information

The Uncertainty Principle and the Quarks

The Uncertainty Principle and the Quarks The Uncertainty Principle and the Quarks Andrei Gritsan Johns Hopkins University August, 2007 JHU Quarknet Meeting Outline The Uncertainty Principle quantum mechanics with elementary particles The Quarks

More information

Physics 214 Experimental Particle Physics. Lecture 1 What to expect.

Physics 214 Experimental Particle Physics. Lecture 1 What to expect. Physics 214 Experimental Particle Physics Lecture 1 What to expect. We ll start with a grand tour. I do not expect you to understand this tour in detail. Instead, think of it as an orientation to which

More information

Spectra of Cosmic Rays

Spectra 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 information

DISCRETE SYMMETRIES IN NUCLEAR AND PARTICLE PHYSICS. Parity PHYS NUCLEAR AND PARTICLE PHYSICS

DISCRETE SYMMETRIES IN NUCLEAR AND PARTICLE PHYSICS. Parity PHYS NUCLEAR AND PARTICLE PHYSICS PHYS 30121 NUCLEAR AND PARTICLE PHYSICS DISCRETE SYMMETRIES IN NUCLEAR AND PARTICLE PHYSICS Discrete symmetries are ones that do not depend on any continuous parameter. The classic example is reflection

More information

Asymmetric Sneutrino Dark Matter

Asymmetric Sneutrino Dark Matter Asymmetric Sneutrino Dark Matter Stephen West Oxford University Asymmetric Sneutrino Dark Matter and the Ω b /Ω dm Puzzle; hep-ph/0410114, PLB, Dan Hooper, John March- Russell, and SW from earlier work,

More information

Outline. Charged Leptonic Weak Interaction. Charged Weak Interactions of Quarks. Neutral Weak Interaction. Electroweak Unification

Outline. Charged Leptonic Weak Interaction. Charged Weak Interactions of Quarks. Neutral Weak Interaction. Electroweak Unification Weak Interactions Outline Charged Leptonic Weak Interaction Decay of the Muon Decay of the Neutron Decay of the Pion Charged Weak Interactions of Quarks Cabibbo-GIM Mechanism Cabibbo-Kobayashi-Maskawa

More information

Relating the Baryon Asymmetry to WIMP Miracle Dark Matter

Relating the Baryon Asymmetry to WIMP Miracle Dark Matter Brussels 20/4/12 Relating the Baryon Asymmetry to WIMP Miracle Dark Matter PRD 84 (2011) 103514 (arxiv:1108.4653) + PRD 83 (2011) 083509 (arxiv:1009.3227) John McDonald, LMS Consortium for Fundamental

More information

Dark matter at LHC (Mostly ATLAS) Ian Hinchliffe LBNL

Dark matter at LHC (Mostly ATLAS) Ian Hinchliffe LBNL Dark matter at LHC (Mostly ATLAS) Ian Hinchliffe LBNL 1 Dark matter at LHC 2 Two classes of searches Model dependent: dependent on other new particles Higgs to invisible Supersymmetry Model independent

More information

OVERVIEW: Dark Matter

OVERVIEW: Dark Matter DM-Stat: Statistical Challenges in the Search for Dark Matter OVERVIEW: Dark Matter Bradley J. Kavanagh GRAPPA Institute, University of Amsterdam b.j.kavanagh@uva.nl @BradleyKavanagh DM-Stat: Statistical

More information

Cosmological Constraint on the Minimal Universal Extra Dimension Model

Cosmological Constraint on the Minimal Universal Extra Dimension Model Cosmological Constraint on the Minimal Universal Extra Dimension Model Mitsuru Kakizaki (Bonn Univ. & ICRR, Univ. of Tokyo) 20 September, 2006 @ SISSA In collaboration with Shigeki Matsumoto (KEK) Yoshio

More information

UNIVERSITÀ DEGLI STUDI DI MILANO Facoltà di Scienze e Tecnologie Corso di Laurea Magistrale in Fisica

UNIVERSITÀ DEGLI STUDI DI MILANO Facoltà di Scienze e Tecnologie Corso di Laurea Magistrale in Fisica UNIVERSITÀ DEGLI STUDI DI MILANO Facoltà di Scienze e Tecnologie Corso di Laurea Magistrale in Fisica Search for Dark Matter direct production in the mono-photon plus missing energy channel in pp collisions

More information

Cosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity

Cosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity Cosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity Masaki Asano The Graduate University for Advanced Studies Collaborated with Shigeki Matsumoto Nobuchika Okada Yasuhiro

More information

Neutrinos and DM (Galactic)

Neutrinos and DM (Galactic) Neutrinos and DM (Galactic) ArXiv:0905.4764 ArXiv:0907.238 ArXiv: 0911.5188 ArXiv:0912.0512 Matt Buckley, Katherine Freese, Dan Hooper, Sourav K. Mandal, Hitoshi Murayama, and Pearl Sandick Basic Result

More information

Dark Matter: What is it?

Dark 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 information

Open Questions in Particle Physics. Carlos Wagner Physics Department, EFI and KICP, Univ. of Chicago HEP Division, Argonne National Laboratory

Open Questions in Particle Physics. Carlos Wagner Physics Department, EFI and KICP, Univ. of Chicago HEP Division, Argonne National Laboratory Open Questions in Particle Physics Carlos Wagner Physics Department, EFI and KICP, Univ. of Chicago HEP Division, Argonne National Laboratory Society of Physics Students, Univ. of Chicago, Nov. 21, 2016

More information

Wesley Smith, U. Wisconsin, January 21, Physics 301: Introduction - 1

Wesley Smith, U. Wisconsin, January 21, Physics 301: Introduction - 1 Wesley Smith, U. Wisconsin, January 21, 2014 Physics 301: Introduction - 1 Physics 301: Physics Today Prof. Wesley Smith, wsmith@hep.wisc.edu Undergraduate Physics Colloquium! Discussions of current research

More information

Neutrino Anomalies & CEνNS

Neutrino Anomalies & CEνNS Neutrino Anomalies & CEνNS André de Gouvêa University PIRE Workshop, COFI February 6 7, 2017 Something Funny Happened on the Way to the 21st Century ν Flavor Oscillations Neutrino oscillation experiments

More information

Physics 214 Experimental Particle Physics. Lecture 1 What to expect.

Physics 214 Experimental Particle Physics. Lecture 1 What to expect. Physics 214 Experimental Particle Physics Lecture 1 What to expect. We ll start with a grand tour. I do not expect you to understand this tour in detail. Instead, think of it as an orientation to which

More information

Measuring Dark Matter Properties with High-Energy Colliders

Measuring Dark Matter Properties with High-Energy Colliders Measuring Dark Matter Properties with High-Energy Colliders The Dark Matter Problem The energy density of the universe is mostly unidentified Baryons: 5% Dark Matter: 20% Dark Energy: 75% The dark matter

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

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

First detection of dark matter How Much Dark Matter is There?

First detection of dark matter How Much Dark Matter is There? Galaxies AS7007, 2012 Lecture 3: Dark matter in galaxies Outline I What is dark matter? How much dark matter is there? How do we know it exists? Dark matter candidates The Cold Dark Matter (CDM) model

More information

Cosmological Signatures of a Mirror Twin Higgs

Cosmological Signatures of a Mirror Twin Higgs Cosmological Signatures of a Mirror Twin Higgs Zackaria Chacko University of Maryland, College Park Curtin, Geller & Tsai Introduction The Twin Higgs framework is a promising approach to the naturalness

More information