Big-Bang nucleosynthesis, early Universe and relic particles. Alexandre Arbey. Moriond Cosmology La Thuile, Italy March 23rd, 2018

Size: px
Start display at page:

Download "Big-Bang nucleosynthesis, early Universe and relic particles. Alexandre Arbey. Moriond Cosmology La Thuile, Italy March 23rd, 2018"

Transcription

1 Big-Bang nucleosynthesis, early Universe and relic particles Alexandre Arbey Lyon U. & CERN TH Moriond Cosmology 2018 La Thuile, Italy March 23rd, 2018

2 Introduction Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

3 What happened before recombination? Quantum gravity? Branes? Other gravitation theories? Ination Topological defects (cosmic strings, magnetic monopoles, domain walls,...)? Primordial Black Holes? Leptogenesis Baryogenesis Particle-antiparticle asymmetry QCD-dominated plasma Relic particle freeze-out/in Big-Bang nucleosynthesis Big-Bang nucleosynthesis is the oldest epoch which leads to direct observations. Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

4 Dark matter: thermal relics Hypothesis: dark matter made of thermal relics. Thermal relics Stable, massive and weakly interacting particles Particles in thermal equilibrium in the early Universe Below the freeze-out temperature ( GeV), suppressed interactions with the thermal bath Annihilation/co-annihilation of the relic particles Out-of-equilibrium description through Boltzmann equations Good particle physics candidates should have the observed cold dark matter density Standard particle physics candidates are in reach of the LHC and dark matter detection experiments For illustrative purposes: dark matter composed of the MSSM lightest neutralinos. Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

5 MSSM neutralino Minimal Supersymmetric extension of the Standard Model (MSSM) More than 100 free parameters Provided R-parity is conserved, sparticles produced in pairs The lightest sparticle is stable 4 neutralinos and 2 charginos: supersymmetric partners of the Higgs (h, H, A, H ± ) and vector bosons (γ, Z, W ± ) The lightest neutralino is a suitable dark matter candidate Lightest neutralino χ 0 1 χ Mixed state of bino/wino/higgsino (photino/zino/higgsino) if mostly bino, very weakly interacting if mostly wino, accompanied by one chargino close in mass if mostly higgsino, accompanied by one chargino and another neutralino close in mass if very mixed, more strongly interacting Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

6 MSSM neutralino Minimal Supersymmetric extension of the Standard Model (MSSM) More than 100 free parameters Provided R-parity is conserved, sparticles produced in pairs The lightest sparticle is stable 4 neutralinos and 2 charginos: supersymmetric partners of the Higgs (h, H, A, H ± ) and vector bosons (γ, Z, W ± ) The lightest neutralino is a suitable dark matter candidate Lightest neutralino χ 0 1 χ Mixed state of bino/wino/higgsino (photino/zino/higgsino) if mostly bino, very weakly interacting if mostly wino, accompanied by one chargino close in mass if mostly higgsino, accompanied by one chargino and another neutralino close in mass if very mixed, more strongly interacting Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

7 Relic density: standard calculation In the Standard Model of Cosmology: before and at nucleosynthesis time, the expansion is dominated by radiation H 2 = 8πG/3 ρ rad the evolution of the number density of all supersymmetric particles follows the Boltzmann equation dn dt = 3Hn σ e v (n2 neq) 2 the time and temperature are related through: ds rad = 3Hs dt rad Thermal average of eective cross section (K 1,2 : modied Bessel functions): ( ) s dp 0 e pe 2 W ek 1 T σ e v = [ m1 4T g i m 2 ( i mi ) ] 2 i g 1 m1 2 K 2 T where: (ij: coannihilating SUSY particles / kl: SM outgoing particles) dw e d cos θ = p ij p kl 2 32πp ijkl e S kl s M(ij kl) helicities diagrams Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

8 Neutralino relic density Very precise measurements of cold dark matter density by Planck (+ others) (2015): Ω ch 2 = ± AA, M. Boudaud, F. Mahmoudi, G. Robbins, arxiv: Binos generally have a too large relic density, except when close in mass to other (co-annihilating) sparticles. Heavy winos and higgsinos can have naturally a correct relic density. The Planck results lead to very strong constraints on supersymmetry. Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

9 Relic density: sensitivity to the cosmological model Caveat! Many unobservable phenomena could have happened during the pre-bbn era. Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

10 Relic density: inuence of a modied expansion rate For example, the expansion rate can be modied. We can parametrize the modication by adding a dark density ρ D : H 2 = 8πG/3 (ρ rad + ρ D ) with ρ D (T ) = ρ D (T BBN )(T /T BBN ) n D n D = 4: radiation-like behaviour n D = 6: behaviour of a scalar eld dominated by its kinetic term n D > 6: decaying scalar eld where κ D = ρ D (T BBN )/ρ γ(t BBN ) Big-Bang Nucleosynthesis (BBN) occurs at T MeV and can impose strong limits on this kind of models, since it may be aected by the presence of a dark density. Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

11 Big-Bang Nucleosynthesis: inuence of a modied expansion rate Deuterium fraction Helium fraction Accepted regions below the lines. Observationally: Y P = ± , 2 H/H = (2.527 ± 0.030) Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

12 Relic density: inuence of a modied expansion rate Pure bino (667 GeV, Ω std h 2 = 22.5) Pure higgsino (510 GeV, Ω std h 2 = ) Relic density mainly increased, possibly by several orders of magnitude. Planck 2015: Ω ch 2 = ± Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

13 Relic density: inuence of entropy injection The entropy content of the Universe can also be altered! Modied relation between time, expansion rate and temperature! Possible parametrisation: where with ds rad dt = 3Hs rad + Σ D Σ D (T ) = Σ D (T BBN )(T /T BBN ) n D n D 5 7: entropy evolution of a decaying scalar eld κ D = Σ D (T BBN )/Σ e γ (T BBN ) Σ e γ (T BBN ) = 1 8π 3 M P 5 T BBN 2 s γ(t BBN ) This modication can push the relic density in the other direction! Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

14 Big-Bang Nucleosynthesis: inuence of entropy injection Deuterium fraction Helium fraction Accepted regions below the lines. Observationally: Y P = ± , 2 H/H = (2.527 ± 0.030) Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

15 Relic density: inuence of entropy injection Pure bino (667 GeV, Ω std h 2 = 22.5) Pure higgsino (510 GeV, Ω std h 2 = ) Relic density decreased or increased, possibly by several orders of magnitude. Planck 2015: Ω ch 2 = ± Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

16 AlterBBN v2.0 (beta1) Calculation of BBN abundances in alternative cosmologies Authors: Alexandre Arbey, Kevin Hickerson and Espen Jenssen Website: Features of AlterBBN Open source code written in C. High readability, user friendly. Fast calculation of the abundance of the elements. 26 elements, nuclear network of 100 processes. Dierent cosmological scenarios (reheating, dark energy, WIMP,...). Automatic calculation of the errors and correlations. Parallel routines for faster correlation calculation. New manual to be released soon! AA, Comput.Phys.Commun. 183 (2012) 1822, arxiv: [astro-ph.co] Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

17 SuperIso Relic v4.0 (beta1) Calculation of avour physics and dark matter observables Authors: Alexandre Arbey, Farvah Nazila Mahmoudi and Glenn Robbins Website: Features of SuperIso Relic Open source code written in C (particle physics amplitudes in Fortran). Calculation of relic density, and direct and indirect detection observables and observability Particle physics models: MSSM and NMSSM currently included Generalisation towards other models ongoing: link with FeynRules and automatical calculation of the amplitudes. Dierent cosmological scenarios. Linked with AlterBBN. Contains SuperIso, for the calculation of avour physics observables. New manual to be released soon! AA, F. Mahmoudi, Comput.Phys.Commun. 181 (2010) 1277, arxiv: [hep-ph] Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

18 Conclusion and perspectives Conclusions Dark matter particles may be strongly aected by the possible phenomena in the early Universe. Big-Bang Nucleosynthesis can help setting limits on the possible deviations. If dark matter particles are discovered, scenarios leading to too large or too small relic densities should not be disregarded. Results rather general, valid also for non-susy scenarios and non-wimps. Perspectives Further improvments in AlterBBN v2.0 and SuperIso Relic v4.0. Detailed manuals will appear soon. Other cosmological scenarios can be implemented. Generic version of SuperIso Relic will be released soon. Do not hesitate to suggest new features, scenarios,... Feedback is welcome if you use the codes! Alexandre Arbey Moriond Cosmology 2018 March 23rd, / 16

BSM physics and Dark Matter

BSM physics and Dark Matter BSM physics and Dark Matter Andrea Mammarella University of Debrecen 26-11-2013 1 Introduction and motivation 2 Dark Matter 3 MiAUMSSM 4 Dark Matter in the MiAUMSSM 5 Conclusion Introduction and motivation

More information

Supersymmetric dark matter with low reheating temperature of the Universe

Supersymmetric dark matter with low reheating temperature of the Universe Supersymmetric dark matter with low reheating temperature of the Universe Sebastian Trojanowski National Center for Nuclear Research, Warsaw COSMO 204 Chicago, August 29, 204 L. Roszkowski, ST, K. Turzyński

More information

The Influence of DE on the Expansion Rate of the Universe and its Effects on DM Relic Abundance

The Influence of DE on the Expansion Rate of the Universe and its Effects on DM Relic Abundance The Influence of DE on the Expansion Rate of the Universe and its Effects on DM Relic Abundance Esteban Jimenez Texas A&M University XI International Conference on Interconnections Between Particle Physics

More information

Dark matter and LHC: complementarities and limitations

Dark matter and LHC: complementarities and limitations Dark matter and LHC: complementarities and limitations,1,2, F. Mahmoudi 1,2,3, A. Arbey 1,2,3, M. Boudaud 4 1 Univ Lyon, Univ Lyon 1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574,

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

Supersymmetry in Cosmology

Supersymmetry in Cosmology Supersymmetry in Cosmology Raghavan Rangarajan Ahmedabad University raghavan@ahduni.edu.in OUTLINE THE GRAVITINO PROBLEM SUSY FLAT DIRECTIONS AND THEIR COSMOLOGIAL IMPLICATIONS SUSY DARK MATTER SUMMARY

More information

Making Dark Matter. Manuel Drees. Bonn University & Bethe Center for Theoretical Physics. Making Dark Matter p. 1/35

Making Dark Matter. Manuel Drees. Bonn University & Bethe Center for Theoretical Physics. Making Dark Matter p. 1/35 Making Dark Matter Manuel Drees Bonn University & Bethe Center for Theoretical Physics Making Dark Matter p. 1/35 Contents 1 Introduction: The need for DM Making Dark Matter p. 2/35 Contents 1 Introduction:

More information

Astroparticle Physics and the LC

Astroparticle Physics and the LC Astroparticle Physics and the LC Manuel Drees Bonn University Astroparticle Physics p. 1/32 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/32 Contents 1) Introduction:

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

Big Bang Nucleosynthesis

Big Bang Nucleosynthesis Big Bang Nucleosynthesis George Gamow (1904-1968) 5 t dec ~10 yr T dec 0.26 ev Neutrons-protons inter-converting processes At the equilibrium: Equilibrium holds until 0 t ~14 Gyr Freeze-out temperature

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

Non-Thermal Dark Matter from Moduli Decay. Bhaskar Dutta. Texas A&M University

Non-Thermal Dark Matter from Moduli Decay. Bhaskar Dutta. Texas A&M University Non-Thermal Dark Matter rom Moduli Decay Bhaskar Dutta Texas A&M University Allahverdi, Dutta, Sinha, PRD87 (2013) 075024, PRDD86 (2012) 095016, PRD83 (2011) 083502, PRD82 (2010) 035004 Allahverdi, Dutta,

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

Theory Group. Masahiro Kawasaki

Theory Group. Masahiro Kawasaki Theory Group Masahiro Kawasaki Current members of theory group Staffs Masahiro Kawasaki (2004~) cosmology Masahiro Ibe (2011~) particle physics Postdoctoral Fellows Shuichiro Yokoyama Shohei Sugiyama Daisuke

More information

Dark Matter from Non-Standard Cosmology

Dark Matter from Non-Standard Cosmology Dark Matter from Non-Standard Cosmology Bhaskar Dutta Texas A&M University Miami 2016 December 16, 2016 1 Some Outstanding Issues Questions 1. Dark Matter content ( is 27%) 2. Electroweak Scale 3. Baryon

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

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

Physics of the hot universe!

Physics of the hot universe! Cosmology Winter School 5/12/2011! Lecture 2:! Physics of the hot universe! Jean-Philippe UZAN! The standard cosmological models! a 0!! Eq. state! Scaling Scale factor! radiation! w=1/3! a -4! t 1/2! Matter

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

Astroparticle Physics at Colliders

Astroparticle Physics at Colliders Astroparticle Physics at Colliders Manuel Drees Bonn University Astroparticle Physics p. 1/29 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/29 Contents 1) Introduction:

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

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

Hot Big Bang model: early Universe and history of matter

Hot Big Bang model: early Universe and history of matter Hot Big Bang model: early Universe and history of matter nitial soup with elementary particles and radiation in thermal equilibrium. adiation dominated era (recall energy density grows faster than matter

More information

Search for SUperSYmmetry SUSY

Search for SUperSYmmetry SUSY PART 3 Search for SUperSYmmetry SUSY SUPERSYMMETRY Symmetry between fermions (matter) and bosons (forces) for each particle p with spin s, there exists a SUSY partner p~ with spin s-1/2. q ~ g (s=1)

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

Dark Matter Abundance in Brane Cosmology

Dark Matter Abundance in Brane Cosmology Dark Matter Abundance in Brane Cosmology Takeshi Nihei Department of Physics, College of Science and Technology, Nihon University, -8-4, Kanda-Surugadai, Chiyoda-ku, Tokyo -838, Japan Nobuchika Okada Theory

More information

Cosmology/DM - I. Konstantin Matchev

Cosmology/DM - I. Konstantin Matchev Cosmology/DM - I Konstantin Matchev What Do We Do? Trying to answer the really big questions: 1. What is the Universe made of?... 5. Can the laws of Physics be unified? 16. What is the cause of the terrible

More information

Axino Phenomenology in the Kim-Nilles mechanism

Axino Phenomenology in the Kim-Nilles mechanism CP3, SDU, Odense, 11 Aug. 2014 Axino Phenomenology in the Kim-Nilles mechanism Eung Jin Chun Outline Introduction to strong CP problem & axion. KSVZ & DFSZ axion models. Supersymmetric axion models and

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

Kaluza-Klein Theories - basic idea. Fig. from B. Greene, 00

Kaluza-Klein Theories - basic idea. Fig. from B. Greene, 00 Kaluza-Klein Theories - basic idea Fig. from B. Greene, 00 Kaluza-Klein Theories - basic idea mued mass spectrum Figure 3.2: (Taken from [46]). The full spectrum of the UED model at the first KK level,

More information

Cosmology. Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation

Cosmology. Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation Cosmology Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation Energy density versus scale factor z=1/a-1 Early times,

More information

Particle Physics and Cosmology II: Dark Matter

Particle Physics and Cosmology II: Dark Matter Particle Physics and Cosmology II: Dark Matter Mark Trodden Center for Particle Cosmology University of Pennsylvania Second Lecture Puerto Vallarta Mexico 1/13/2011 Problems of Modern Cosmology Is cosmic

More information

Gravitinos, Reheating and the Matter-Antimatter Asymmetry of the Universe

Gravitinos, Reheating and the Matter-Antimatter Asymmetry of the Universe Gravitinos, Reheating and the Matter-Antimatter Asymmetry of the Universe Raghavan Rangarajan Physical Research Laboratory Ahmedabad with N. Sahu, A. Sarkar, N. Mahajan OUTLINE THE MATTER-ANTIMATTER ASYMMETRY

More information

The Matter-Antimatter Asymmetry and New Interactions

The Matter-Antimatter Asymmetry and New Interactions The Matter-Antimatter Asymmetry and New Interactions The baryon (matter) asymmetry The Sakharov conditions Possible mechanisms A new very weak interaction Recent Reviews M. Trodden, Electroweak baryogenesis,

More information

Lecture 18 - Beyond the Standard Model

Lecture 18 - Beyond the Standard Model Lecture 18 - Beyond the Standard Model Why is the Standard Model incomplete? Grand Unification Baryon and Lepton Number Violation More Higgs Bosons? Supersymmetry (SUSY) Experimental signatures for SUSY

More information

Learning from WIMPs. Manuel Drees. Bonn University. Learning from WIMPs p. 1/29

Learning from WIMPs. Manuel Drees. Bonn University. Learning from WIMPs p. 1/29 Learning from WIMPs Manuel Drees Bonn University Learning from WIMPs p. 1/29 Contents 1 Introduction Learning from WIMPs p. 2/29 Contents 1 Introduction 2 Learning about the early Universe Learning from

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

Physics at e + e - Linear Colliders. 4. Supersymmetric particles. M. E. Peskin March, 2002

Physics at e + e - Linear Colliders. 4. Supersymmetric particles. M. E. Peskin March, 2002 Physics at e + e - Linear Colliders 4. Supersymmetric particles M. E. Peskin March, 2002 In this final lecture, I would like to discuss supersymmetry at the LC. Supersymmetry is not a part of the Standard

More information

I V E R S U N. The Hot Big Bang I T Y T H E O F E. Andrew Liddle R G. Image: NASA/WMAP Science Team

I V E R S U N. The Hot Big Bang I T Y T H E O F E. Andrew Liddle R G. Image: NASA/WMAP Science Team The Hot Big Bang Andrew Liddle T H E O F E U N D I I V E R S N U B R G I T Y H Image: NASA/WMAP Science Team The Standard Model The discovery of the Higgs particle completes the Standard Model of Particle

More information

7 Relic particles from the early universe

7 Relic particles from the early universe 7 Relic particles from the early universe 7.1 Neutrino density today (14 December 2009) We have now collected the ingredients required to calculate the density of relic particles surviving from the early

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

Week 3: Thermal History of the Universe

Week 3: Thermal History of the Universe Week 3: Thermal History of the Universe Cosmology, Ay127, Spring 2008 April 21, 2008 1 Brief Overview Before moving on, let s review some of the high points in the history of the Universe: T 10 4 ev, t

More information

Possible Connections in Colliders, Dark Matter, and Dark Energy

Possible Connections in Colliders, Dark Matter, and Dark Energy Possible Connections in Colliders, Dark Matter, and Dark Energy 0704.3285 [hep-ph] 0706.2375 [hep-ph] Daniel Chung (U. Wisconsin Madison) Collaborators: L. Everett, K. Kong, K. Matchev Quiz Which of the

More information

The Early Universe. Overview: The Early Universe. Accelerators recreate the early universe. Simple Friedmann equation for the radiation era:

The Early Universe. Overview: The Early Universe. Accelerators recreate the early universe. Simple Friedmann equation for the radiation era: The Early Universe Notes based on Teaching Company lectures, and associated undergraduate text with some additional material added. ) From µs to s: quark confinement; particle freezout. 2) From s to 3

More information

COSMOLOGY AND GRAVITATIONAL WAVES. Chiara Caprini (APC)

COSMOLOGY AND GRAVITATIONAL WAVES. Chiara Caprini (APC) COSMOLOGY AND GRAVITATIONAL WAVES Chiara Caprini (APC) the direct detection of GW by the LIGO interferometers has opened a new era in Astronomy - we now have a new messenger bringing complementary informations

More information

Stau Pair Production At The ILC Tohoku University Senior Presentation Tran Vuong Tung

Stau Pair Production At The ILC Tohoku University Senior Presentation Tran Vuong Tung e + Z*/γ τ + e - τ Stau Pair Production At The ILC Tohoku University Senior Presentation Tran Vuong Tung 1 Outline Introduction of the International Linear Collider (ILC) Introduction of (g μ -2) in the

More information

Inflation, Gravity Waves, and Dark Matter. Qaisar Shafi

Inflation, Gravity Waves, and Dark Matter. Qaisar Shafi Inflation, Gravity Waves, and Dark Matter Qaisar Shafi Bartol Research Institute Department of Physics and Astronomy University of Delaware Feb 2015 University of Virginia Charlottesville, VA Units ћ =

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

Supersymmetry at the LHC

Supersymmetry at the LHC Supersymmetry at the LHC What is supersymmetry? Present data & SUSY SUSY at the LHC C. Balázs, L. Cooper, D. Carter, D. Kahawala C. Balázs, Monash U. Melbourne SUSY@LHC.nb Seattle, 23 Sep 2008 page 1/25

More information

Physics 662. Particle Physics Phenomenology. February 21, Physics 662, lecture 13 1

Physics 662. Particle Physics Phenomenology. February 21, Physics 662, lecture 13 1 Physics 662 Particle Physics Phenomenology February 21, 2002 Physics 662, lecture 13 1 Physics Beyond the Standard Model Supersymmetry Grand Unified Theories: the SU(5) GUT Unification energy and weak

More information

Dark Matter II. Marco Cirelli. (CNRS IPhT Saclay) December th TRR Winter School - Passo del Tonale. Reviews on Dark Matter: NewDark

Dark Matter II. Marco Cirelli. (CNRS IPhT Saclay) December th TRR Winter School - Passo del Tonale. Reviews on Dark Matter: NewDark 10-14 December 2012 6 th TRR Winter School - Passo del Tonale Dark Matter II Marco Cirelli (CNRS IPhT Saclay) in collaboration with: A.Strumia (Pisa) N.Fornengo (Torino) M.Tamburini (Pisa) R.Franceschini

More information

THERMAL HISTORY OF THE UNIVERSE

THERMAL HISTORY OF THE UNIVERSE M. Pettini: Introduction to Cosmology Lecture 7 THERMAL HISTORY OF THE UNIVERSE The Universe today is bathed in an all-pervasive radiation field, the Cosmic Microwave Background (CMB) which we introduced

More information

PAMELA from Dark Matter Annihilations to Vector Leptons

PAMELA from Dark Matter Annihilations to Vector Leptons PAMELA from Dark Matter Annihilations to Vector Leptons phalendj@umich.edu With Aaron Pierce and Neal Weiner University of Michigan LHC and Dark Matter Workshop 2009 University of Michigan Outline PAMELA

More information

arxiv: v2 [hep-ph] 8 Dec 2009

arxiv: v2 [hep-ph] 8 Dec 2009 OUTP-09-18-P, UCB-PTH-09/32 Freeze-In Production of FIMP Dark Matter Lawrence J. Hall a, Karsten Jedamzik b, John March-Russell c and Stephen M. West d,e arxiv:0911.1120v2 [hep-ph] 8 Dec 2009 a Department

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

SUSY Phenomenology & Experimental searches

SUSY Phenomenology & Experimental searches SUSY Phenomenology & Experimental searches Slides available at: Alex Tapper http://www.hep.ph.ic.ac.uk/~tapper/lecture.html Objectives - Know what Supersymmetry (SUSY) is - Understand qualitatively the

More information

Production of WIMPS in early Universe

Production of WIMPS in early Universe Production of WIMPS in early Universe Anjishnu Bandyopadhyay Universität Bonn July 5, 2013 Anjishnu Bandyopadhyay Production of WIMPS in early Universe 1 / 30 1 2 Generalized Equation Equation for relics

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

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

Is SUSY still alive? Dmitri Kazakov JINR

Is SUSY still alive? Dmitri Kazakov JINR 2 1 0 2 The l o o h c S n a e p o r Eu y g r e n E h g i of H s c i s y PAnhjou, France 2 1 0 2 e n 6 19 Ju Is SUSY still alive? Dmitri Kazakov JINR 1 1 Why do we love SUSY? Unifying various spins SUSY

More information

THE STATUS OF NEUTRALINO DARK MATTER

THE STATUS OF NEUTRALINO DARK MATTER THE STATUS OF NEUTRALINO DARK MATTER BIBHUSHAN SHAKYA CORNELL UNIVERSITY CETUP 2013 Workshop June 25, 2013 Based on hep-ph 1208.0833, 1107.5048 with Maxim Perelstein, hep-ph 1209.2427 The favorite / most

More information

A model of the basic interactions between elementary particles is defined by the following three ingredients:

A model of the basic interactions between elementary particles is defined by the following three ingredients: I. THE STANDARD MODEL A model of the basic interactions between elementary particles is defined by the following three ingredients:. The symmetries of the Lagrangian; 2. The representations of fermions

More information

AlterBBN: A program for calculating the BBN abundances of the elements in alternative cosmologies

AlterBBN: A program for calculating the BBN abundances of the elements in alternative cosmologies CERN-PH-TH/2011-135 LYCEN 2011-06 AlterBBN: A program for calculating the BBN abundances of the elements in alternative cosmologies Alexandre Arbey Université de Lyon, France; Université Lyon 1, CNRS/IN2P3,

More information

About the format of the literature report

About the format of the literature report About the format of the literature report Minimum 3 pages! Suggested structure: Introduction Main text Discussion Conclusion References Use bracket-number (e.g. [3]) or author-year (e.g. Zackrisson et

More information

Direct Detection Rates of Neutralino WIMP in MSSM

Direct Detection Rates of Neutralino WIMP in MSSM Direct Detection Rates of Neutralino WIMP in MSSM Yeong Gyun Kim a, 1 Takeshi Nihei b, Leszek Roszkowski a, and Roberto Ruiz de Austri c a Department of Physics, Lancaster University, Lancaster LA1 4YB,

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

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

Search for exotic process with space experiments

Search for exotic process with space experiments Search for exotic process with space experiments Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata Rencontres de Moriond, Very High Energy Phenomena in the Universe Les Arc, 20-27

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

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

Chapter 27 The Early Universe Pearson Education, Inc.

Chapter 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 information

An Introduction to Particle Physics

An Introduction to Particle Physics An Introduction to Particle Physics The Universe started with a Big Bang The Universe started with a Big Bang What is our Universe made of? Particle physics aims to understand Elementary (fundamental)

More information

Superheavy Thermal Dark Matter

Superheavy Thermal Dark Matter Superheavy Thermal Dark Matter 13th April 2018 University of Illinois at Chicago Work /w Joe Bramante [1701.05859] & Saleh Hamdan [1710.03758] 1/18 Introduction Xenon1T Unitarity 2/18 Superheavy Dark Matter

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

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

Scalar field dark matter and the Higgs field

Scalar field dark matter and the Higgs field Scalar field dark matter and the Higgs field Catarina M. Cosme in collaboration with João Rosa and Orfeu Bertolami Phys. Lett., B759:1-8, 2016 COSMO-17, Paris Diderot University, 29 August 2017 Outline

More information

Creating Matter-Antimatter Asymmetry from Dark Matter Annihilations in Scotogenic Scenarios

Creating Matter-Antimatter Asymmetry from Dark Matter Annihilations in Scotogenic Scenarios Creating Matter-Antimatter Asymmetry from Dark Matter Annihilations in Scotogenic Scenarios Based on arxiv:1806.04689 with A Dasgupta, S K Kang (SeoulTech) Debasish Borah Indian Institute of Technology

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

The Lightest Higgs Boson and Relic Neutralino in the MSSM with CP Violation

The Lightest Higgs Boson and Relic Neutralino in the MSSM with CP Violation The Lightest Higgs Boson and Relic Neutralino in the MSSM with CP Violation Stefano Scopel Korea Institute of Advanced Study (based on: J. S. Lee, S. Scopel, PRD75, 075001 (2007)) PPP7, Taipei, Taiwan,

More information

Introduction Motivation WIMP models. WIMP models. Sebastian Belkner. University of Bonn - University of Cologne. June 24, 2016

Introduction Motivation WIMP models. WIMP models. Sebastian Belkner. University of Bonn - University of Cologne. June 24, 2016 WIMP models Sebastian Belkner University of Bonn - University of Cologne June 24, 2016 1 / 27 A brief history of the universe 2 / 27 Outline 1 Motivation On galactic scales On cosmological scales 2 WIMP

More information

RECENT PROGRESS IN SUSY DARK MATTER

RECENT PROGRESS IN SUSY DARK MATTER RECENT PROGRESS IN SUSY DARK MATTER Jonathan Feng University of California, Irvine 12 April 2006 Texas A&M Mitchell Symposium 12 Apr 06 Graphic: Feng N. Graf 1 Supersymmetric dark matter has been around

More information

Moduli-induced axion problem

Moduli-induced axion problem Moduli-induced axion problem Kazunori Nakayama (University of Tokyo) T.Higaki, KN, F.Takahashi, JHEP1307,005 (2013) [1304.7987] SUSY2013 @ ICTP, Trieste, Italy (2013/8/26) What we have shown : Kahler

More information

Earlier in time, all the matter must have been squeezed more tightly together and a lot hotter AT R=0 have the Big Bang

Earlier in time, all the matter must have been squeezed more tightly together and a lot hotter AT R=0 have the Big Bang Re-cap from last lecture Discovery of the CMB- logic From Hubble s observations, we know the Universe is expanding This can be understood theoretically in terms of solutions of GR equations Earlier in

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

Baryon-Dark Matter Coincidence. Bhaskar Dutta. Texas A&M University

Baryon-Dark Matter Coincidence. Bhaskar Dutta. Texas A&M University Baryon-Dark Matter Coincidence Bhaskar Dutta Texas A&M University Based on work in Collaboration with Rouzbeh Allahverdi and Kuver Sinha Phys.Rev. D83 (2011) 083502, Phys.Rev. D82 (2010) 035004 Miami 2011

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

Beyond the WIMP Alternative dark matter candidates. Riccardo Catena. Chalmers University

Beyond the WIMP Alternative dark matter candidates. Riccardo Catena. Chalmers University Beyond the WIMP Alternative dark matter candidates Riccardo Catena Chalmers University April 3, 2017 Outline WIMPs and the thermal production mechanism Generalized WIMPs Other candidates / production mechanisms

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

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

Par$cle physics Boost Factors

Par$cle physics Boost Factors Par$cle physics Boost Factors Junji Hisano (ICRR, Univ. of Tokyo) TANGO in PARIS Tes$ng Astropar$cle with the New GeV/TeV Observa$ons May 4 th 6 th, 2009 Ins$tut d'astrophysique de Paris, France Contents

More information

arxiv: v1 [hep-ph] 12 Nov 2012

arxiv: v1 [hep-ph] 12 Nov 2012 CERN-PH-TH/2012-308 Light neutralino dark matter in MSSM arxiv:1211.2795v1 [hep-ph] 12 Nov 2012 CERN Theory Division, CH-1211 Geneva 23, Switzerland Clermont Université, Université Blaise Pascal, CNRS/IN2P3,

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

Big Bang Nucleosynthesis and Particle Physics

Big Bang Nucleosynthesis and Particle Physics New Generation Quantum Theory -Particle Physics, Cosmology and Chemistry- Kyoto University Mar.7-9 2016 Big Bang Nucleosynthesis and Particle Physics Masahiro Kawasaki (ICRR & Kavli IPMU, University of

More information

CMB & Light Degrees of Freedom

CMB & Light Degrees of Freedom CMB & Light Degrees of Freedom Joel Meyers Canadian Institute for Theoretical Astrophysics SLAC Summer Institute 2017 Cosmic Opportunities August 21, 2017 Image Credits: Planck, ANL Light Relics What and

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

Twin Higgs Theories. Z. Chacko, University of Arizona. H.S Goh & R. Harnik; Y. Nomura, M. Papucci & G. Perez

Twin Higgs Theories. Z. Chacko, University of Arizona. H.S Goh & R. Harnik; Y. Nomura, M. Papucci & G. Perez Twin Higgs Theories Z. Chacko, University of Arizona H.S Goh & R. Harnik; Y. Nomura, M. Papucci & G. Perez Precision electroweak data are in excellent agreement with the Standard Model with a Higgs mass

More information

Interconnection between Particle Physics and Cosmology at the LHC

Interconnection between Particle Physics and Cosmology at the LHC Interconnection between Particle Physics and Cosmology at the LHC Selections from the Cosmo Secret Cube Catalogue Transformer Cube Standard Model Cube PPC Cube Premiere Props Teruki Kamon Mitchell Institute

More information

Calculation of Momentum Distribution Function of a Non-Thermal Fermionic Dark Matter

Calculation of Momentum Distribution Function of a Non-Thermal Fermionic Dark Matter Calculation of Momentum Distribution Function of a Non-Thermal Fermionic Dark Matter, March 8, 2017. arxiv:1612.02793, with Anirban Biswas. Aritra Gupta Why Non-Thermal? 1 / 31 The most widely studied

More information

How high could SUSY go?

How high could SUSY go? How high could SUSY go? Luc Darmé LPTHE (Paris), UPMC November 24, 2015 Based on works realised in collaboration with K. Benakli, M. Goodsell and P. Slavich (1312.5220, 1508.02534 and 1511.02044) Introduction

More information

String Theory in the LHC Era

String Theory in the LHC Era String Theory in the LHC Era J Marsano (marsano@uchicago.edu) 1 String Theory in the LHC Era 1. Electromagnetism and Special Relativity 2. The Quantum World 3. Why do we need the Higgs? 4. The Standard

More information