1. Electric Dipole Moments, the LHC, and the Origin of Matter M.J. Ramsey-Musolf Wisconsin-Madison http://www.physics.wisc.edu/groups/particle-theory/ NPAC Theoretical Nuclear, Particle, Astrophysics & Cosmology MIT LNS Colloquium, March 2011

2. The Origin & History of Matter Standard Model Universe EW Symmetry Breaking: Higgs ? BSM Universe QCD: n+p! nuclei QCD: q+g! n,p… Astro: stars, galaxies,.. How did we go from nothing to something ? e + + e - !  q + q ! 

3. The Origin & History of Matter ? Baryogenesis: When? CPV? SUSY? Neutrinos? EW Baryogenesis: testable w/ EDMs + colliders Leptogenesis: less testable, look for ingredients w/ s Can new TeV scale physics explain the abundance of matter ? If so, how will we know ? What are the quantitative implications of new EDM experiments & LHC searches for the Higgs and new particles for explaining the origin of Y B &  CDM ?

4. The Origin of Matter ? Baryogenesis: When? CPV? SUSY? Neutrinos? EW Baryogenesis: testable w/ EDMs + colliders Leptogenesis: less testable, look for ingredients w/ s Can new TeV scale physics explain the abundance of matter ? If so, how will we know ? What are the quantitative implications of new EDM experiments & LHC searches for the Higgs and new particles for explaining the origin of Y B ? PRD 71: 075010 (2005) PRD 73: 115009 (2006) JHEP 0607:002 (2006 ) PRD 78:075009 (2008) PRL 102:061301 (2009) PLB 673: 95 (2009) JHEP 0912:067 (2009) PRD 81:063506 (2010) JHEP 1001:002 (2010) PRD 81: 103503 (2010) JHEP 1008:062 (2010) D. Chung Wisconsin V. Cirigliano LANL B. Garbrecht Aachen M. Gonzalez-Alonso Wisconsin C. Lee MIT Y. Li BNL T. Liu UC Santa Barbara S. Profumo UC Santa Cruz J. Shiu IPMU S. Tulin TRIUMF Baryogenesis & EDMs PRD 75: 037701 (2007) JHEP 0807:010 (2007) PRD 77: 035005 (2008) PRD79: 015018 (2009) PRD79: 055024 (2009) JHEP 1001:053 (2010) arXiv: 1101.4665 [hep-ph] Higgs Pheno & EWPT V. BargerWisconsin P. Fileviez PerezWisconsin M. GonderingerWisconsin P. LangackerIAS H. LimWisconsin M. McCaskeyKansas D. O’ConnellIAS H. PatelWisconsin S. ProfumoUC Santa Cruz G. ShaugnessyANL/Northwestern K. WangIPMU M. WiseCaltech

5. Outline I.Baryogenesis: General Features II.Computing Y B systematically: progress & challenges (today’s theory talk by V. Cirigliano) III.Illustrative phenomenology in MSSM: EDMs & the LHC IV.EW Phase Transition: Higgs & New Scalars

6. I. Baryogenesis: General Features

7. Baryogenesis: Ingredients Anomalous B-violating processesPrevent washout by inverse processes Sakharov Criteria B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 SM Sphalerons:  SM CKM CPV:  SM EWPT:  EDMs LHC: Scalars

8. EW Baryogenesis: Standard Model Weak Scale Baryogenesis B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 Anomalous Processes Different vacua:  (B+L)=  N CS Kuzmin, Rubakov, Shaposhnikov McLerran,… Sphaleron Transitions

9. EW Baryogenesis: Standard Model Weak Scale Baryogenesis B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 Increasing m h 1st order2nd order CP-violation too weak No EWPT Shaposhnikov

10. Electroweak Baryogenesis Baryogenesis: When? CPV? SUSY? Neutrinos? EW symmetric universe Bubbles of broken EW symmetry EW phase transition

11. Baryogenesis: New Electroweak Physics Weak Scale Baryogenesis B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 Unbroken phase Broken phase CP Violation Topological transitions 1st order phase transition Is it viable? Can experiment constrain it? How reliably can we compute it? Theoretical Issues: Strength of phase transition (Higgs sector) Bubble dynamics (numerical) Transport at phase boundary (non-eq QFT) EDMs: many-body physics & QCD

12. II. Computing Y B

13. Systematic Baryogenesis Goal: Derive dependence of Y B on parameters L new systematically (controlled approximations) Parameters in L new Bubble & PT dynamics CPV phases Departure from equilibrium Earliest work: QM scattering & stat mech New developments: non-equilibrium QFT Develop methods with Minimal Supersymmetric SM but more generally applicable

14. Systematic Baryogenesis Goal: Derive dependence of Y B on parameters L new systematically (controlled approximations) Parameters in L new Bubble & PT dynamics CPV phases Departure from equilibrium Earliest work: QM scattering & stat mech New developments: non-equilibrium QFT Scale Hierarchy: Fast, but not too fast Hot, but not too hot Dense, but not too dense  d =  v w (k /  << 1  p =  p /  << 1   =  / T << 1 Thermal, but not too dissipative Plural, but not too flavored  coll =  coll /  << 1  osc =  / T << 1 Work to lowest, non- trivial order in  ’s Error is O (  ) ~ 0.1 Cirigliano, Lee, R-M,Tulin

15. Baryogenesis: CPV & Transport Weak Scale Baryogenesis B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 Unbroken phase Broken phase CP Violation & Transport Also Cirigliano, Lee, R-M, Tulin F WS (x) ->0 deep inside bubble n L produced in wall & diffuses in front

16. Baryogenesis: CPV & Transport Weak Scale Baryogenesis B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 Unbroken phase Broken phase CP Violation & Transport Transport: A Competition CPV Chem Eq R-M et al Diffusion Also Cirigliano, Lee, R-M, Tulin Coupled set of (~30) quantum Boltzmann equations Thanks: B. Garbrecht

17. Baryogenesis: CPV & Transport Weak Scale Baryogenesis B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 Unbroken phase Broken phase CP Violation & Transport Transport: A Competition CPV Chem Eq R-M et al Diffusion Also Cirigliano, Lee, R-M, Tulin Coupled set of (~30) quantum Boltzmann equations Thanks: B. Garbrecht Topological transitions MSSM: Chung, Garbrecht, R-M, Tulin ‘09 Bubble interior Bubble exterior Details of spectrum & int impt: Chung, Garbrecht, R-M, Tulin ‘08 LH leptons LH quarks LH fermions

18. Baryogenesis: CPV & Transport Weak Scale Baryogenesis B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 Unbroken phase Broken phase CP Violation & Transport Transport: A Competition CPV Chem Eq R-M et al Diffusion Also Cirigliano, Lee, R-M, Tulin Coupled set of (~30) quantum Boltzmann equations EDM searches: How strong was the CPV “kick” ? Thanks: B. Garbrecht Topological transitions MSSM: Chung, Garbrecht, R-M, Tulin ‘09 Bubble interior Bubble exterior CPV LH leptons LH quarks LH fermions CPV Sources: Compute finite-T Greens fns in presence of spacetime varying, complex mass matrix (CPV flavor oscillations) & thermalizing reactions Approx solutions Exact solution for time-varying, spatially homogeneous background (Cirigliano, Lee, R-M, Tulin ‘09) Full solution: in progress

19. Key Results: MSSM Resonant Higgsino-Gaugino scattering dominates S CPV S CPV

20. CP-cons particle number changing processes Chung,Garbrecht, R-M, Tulin: PRL 102:061301 (2009) Small tan  negligible Y b,  effects tan  =20: impt Y b,  effects (g  -2) Detailed information from precision tests & LHC needed Key Results: MSSM & Beyond

21. III. Phenomenology: EDMs, LHC, & Y B

22. EDMs: New CPV? SM “background” well below new CPV expectations New expts: 10 2 to 10 3 more sensitive CPV needed for BAU? Mass Scale Sensitivity sin  CP ~ 1 ! M > 5000 GeV M < 500 GeV ! sin  CP < 10 -2 3.1 x 10 -29

23. EDMs: Complementary Searches Electron Improvements of 10 2 to 10 3 Neutron Neutral Atoms Deuteron QCD

24. EDMs: Strongly Interacting Systems Electron Neutron Neutral Atoms Deuteron QCD P-,T-odd  NN

25. EDMs: Schiff Moments Electron Improvements of 10 2 to 10 3 Neutron Neutral Atoms Deuteron QCD Nuclear Schiff Moment Nuclear EDM: Screened in atoms Schiff Screening Atomic effect from nuclear finite size: Schiff moment

26. EDMs in SUSY One-loop EDM: q, l, n…Chromo-EDM: q, n… Dominant in nuclei & atoms 40 new CPV phases  j = arg (  M j b * )  A = arg (A f M j ) Universality Assumption     Common  A

27. One Loop EDMs & Baryogenesis T ~ T EW Resonant Non-resonant Cirigliano, Lee, Tulin, R-M Future d e d n d A

28. EDM Interpretation: MSSM at 2 Loop  A = arg (A f M j ) Li, Profumo, R-M 09 2-loop: Non-universal Phases  j = arg (  M j b * ) Decouple in heavy sfermion regime ATLAS Exclusion: mSUGRA/CMSSM arXiv: 1102.5290

29. EDMs & EWB: Non-universal phases Arg(  M 1 b * ) = Arg(  M 2 b * ) / Weak dependence of d e, d n on Arg(  M 1 b * ) Res   EWB not compatible with d n Res & non-res   EWB compatible with future d n, light m A, & moderate tan  Li, Profumo, R-M: PLB 673:95 (2009)

30. MSSM Baryogenesis: EDMs & LHC baryogenesis Present d e LEP II exclProspective d n Cirigliano, Profumo, R-M  + -driven EWB  0 -driven EWB 10 -28 LHC reach

31. EDMs: What We May Learn Present n-EDM limit Proposed n-EDM limit Matter-Antimatter Asymmetry in the Universe: Theory: How robust ? Can EDMs & LHC kill EW baryogenesis ? “n-EDM has killed more theories than any other single experiment” ? MSSM

32. IV. EW Phase Transition: Higgs & New Scalars Was there a first order EWPT leading to bubble nucleation? If BSM physics (CPV + particle transfer) generated a large initial Y B, did nature preserve it inside the bubbles ?

33. EW Phase Transition: New Scalars 1st order2nd order LEP EWWG Increasing m h m h >114.4 GeV or ~ 90 GeV (SUSY) Computed E SM : m H < 70 GeV Need So that  sphaleron is not too fast V Eff (T) : ++ “Strong” 1 st order EWPT Preserve Y B initial Bubble nucleation

34. Baryon Number Preservation ~  F(  ) Final baryon asymmetry Initial baryon asymmetry ln S ~ A(T C ) e  “Washout factor”

35. EW Phase Transition: New Scalars 1st order2nd order LEP EWWG Increasing m h m h >114.4 GeV or ~ 90 GeV (SUSY) Computed E SM : m H < 70 GeV Need So that  sphaleron is not too fast E MSSM ~ 10 E pert SM : m H < 120 GeV Stop loops in V Eff Light RH stop w/ special Non-doublet Higgs (w / wo SUSY) MixingDecay

36. MSSM: Color Breaking Vacua Deeper minima may develop along stop direction Carena et al (2008): color- neutral EW vacuum is metastable for appropriate MSSM parameters Two-loop analysis of V EFF in effective theory

37. The Simplest Extension Model Independent Parameters: v 0, x 0, 0, a 1, a 2, b 3, b 4 H-S Mixing H 1 ! H 2 H 2 Mass matrix Stable S (dark matter?) Tree-level Z 2 symmetry: a 1 =b 3 =0 to prevent s-h mixing and one-loop s hh x 0 =0 to prevent h-s mixing xSM EWPT:  Signal Reduction Factor ProductionDecay Simplest extension of the SM scalar sector: add one real scalar S (SM singlet) Two Higgs mass eigenstates at “low” (LHC) energy: mixed doublet-singlet More flexibility pattern of symmetry breaking at high T Can achieve 1 st order EWPT and evade LEP SM Higgs mass bounds LHC: Signal Reduction Factor ProductionDecay sin 2  O’Connel, R-M, Wise: Profumo, R-M, Shaugnessy: Barger, Langacker, McCaskey, R-M Shaugnessy: PRD 75: 037701 (2007) JHEP 0807:010 (2007) PRD 77: 035005 (2008) PRD79: 015018 (2009) Model EWPT LHC & DM

38. Finite Temperature Potential What is the pattern of symmetry breaking ? What are conditions on the couplings in V(H,S) so that /T > 1 at T C ?

39. LHC Phenomenology Signatures EWPO compatible m 2 > 2 m 1 m 1 > 2 m 2 LHC: reduced BR(h SM) Signal Reduction Factor ProductionDecay Light: all models Black: LEP allowed Scan: EWPT-viable model parameters LHC exotic final states: 4b-jets,  + 2 b-jets… EWPO comp w/ a 1 =0=b 3 LHC: reduced BR(h SM)

40. Complex Singlet: LHC Discovery Barger, Langacker, McCaskey, R-M, Shaugnessy Traditional search: CMSInvisible search: ATLAS Single component case (x 0 = 0) EWPT

41. Baryon Number Preservation: Open Theory Issues ~ Final baryon asymmetry Initial baryon asymmetry Gauge Dep Freq of sph unstable mode Fluct Det ratio Duration of EWPT Y B init & entropy dilution H. Patel & MRM, arXiv: 1101.4665

42. Ongoing Theoretical Work EWPT with scalars in higher- dim reps of SU(2) Nuclear Schiff Moment Nuclear EDM: Screened in atoms Computationally tractable operator accounting for nuclear correlations (Liu, Haxton, R-M, Timmermans…) Chung, Garbrecht, R-M, Tulin ‘09 Bubble interior Bubble exterior CPV CPV sources: resum vevs to all orders & consistently solve for non-eq Green’s functions Apply our tools to candidates for the “new Standard Model” Learn what expts teach us about the origin of matter

43. Summary I.Baryonic Matter & Electroweak Baryogenesis II. Dark Matter Can TeV scale new physics explain the abundance of matter ? Highly interdisciplinary problem Precision, sensitivity… Precision: details of the interactions and spectrum essential Energy: multi-TeV mass reach may be needed Astro/Cosmo: relic , e +, GW… Theory: Non-equilibrium & finite-T QFT, model- building, many-body & nonperturbative QCD, collider phenomenology…

44. Back Matter

45. Fast, but not too fast Hot, but not too hot Dense, but not too dense  d =  v w (k /  << 1  p =  p /  << 1   =  / T << 1 Thermal, but not too dissipative Plural, but not too flavored  coll =  coll /  << 1  osc =  / T << 1 ATLAS Exclusion: mSUGRA/CMSSM arXiv: 1102.5290

46. “Strong” 1 st order EWPT Preserve Y B initial Bubble nucleation

47. The Simplest Extension Model Independent Parameters: v 0, x 0, 0, a 1, a 2, b 3, b 4 H-S Mixing H 1 ! H 2 H 2 Mass matrix Stable S (dark matter?) Tree-level Z 2 symmetry: a 1 =b 3 =0 to prevent s-h mixing and one-loop s hh x 0 =0 to prevent h-s mixing xSM EWPT:  Signal Reduction Factor ProductionDecay sin 2 

48. MSSM EDMs: Leading Contributions Electron Neutron Neutral Atoms Deuteron q, l EDMChromo- EDM Weinberg 3 gluon

49. EDMs & Schiff Moments One-loop EDM: q, l, n…Chromo-EDM: q, n… Dominant in nuclei & atoms Engel & de Jesus: Enhanced isoscalar sensitivity (  QCD ) Schiff Moment in 199 Hg Nuclear & hadron structure

50. EDMs: QCD & Many-Body Theory Electron Improvements of 10 2 to 10 3 Neutron Neutral Atoms Deuteron QCD Nuclear Schiff Moment Nuclear EDM: Screened in atoms Schiff Screening Atomic effect from nuclear finite size: Schiff moment Liu et al: New formulation of Schiff operator + … Role of nuclear correlations

51. Non-minimal Solutions (SUSY) Nature of DM & its interactions Origin of the BAU Gauge hierarchy EWPO & m H Origin of m “Minimal” : 105 new parameters        Additional complications: Why is  ~ M weak ? Why little flavor & CPV ? Origin of params in L soft ? M SUSY < TeV (hierarchy) Bino-Higgsino-like LSP (DM) Light RH stop ( m < 125 GeV) M 1 ~     

52. Minimal Solutions (non-SUSY) Nature of DM & its interactions Origin of the BAU Gauge hierarchy EWPO & m H Origin of m      Extra ScalarsExtra Fermions     

53. EWPT & DM: New Scalars Gauge Interactions No Gauge Interactions Simplest: 1 new dof Next Simplest: 2 new dof Focus: Key parameters for cosmo & LHC pheno Complex Singlet (cxSM): DM, BAU, and m H / EWPO H-S Mixing, Reduced BRs, &  SI Real Singlet (xSM): DM or BAU-m H / EWPO BAU: H-S Mixing & Reduced BRs DM: Reduced BRs &  SI Simplest: 3 new dof (2HDM: 4 new dof) Real Triplet  SM)  DM or BAU (EWPT) DM: Charged track &  SI BAU:  or bb  ;  Br(H!  )

54. LHC Phenomenology Signatures EWPO compatible m 2 > 2 m 1 m 1 > 2 m 2 LHC: reduced BR(h SM) Signal Reduction Factor ProductionDecay CMS 30 fb -1  SM-like Singlet-like SM-like SM-like w/ H 2 ->H 1 H 1 or Singlet-like ~ EWB Viable Light: all models Black: LEP allowed Scan: EWPT-viable model parameters LHC exotic final states: 4b-jets,  + 2 b-jets… EWPO comp w/ a 1 =0=b 3 LHC: reduced BR(h SM) Probing   : WBF H ! ZZ! 4 l H ! WW! 2j l Early LHC discovery possible Determine  as low as ~ 0.5

55. Illustrative Study: MSSM Neutralino Mass Matrix M1M1 -- M2M2 -m Z cos  sin  W m Z cos  cos  W m Z sin  sin  W -m Z sin  sin  W 0 0 0 0 -- -m Z cos  sin  W m Z cos  cos  W m Z sin  sin  W -m Z sin  sin  W M N = Chargino Mass Matrix M2M2  M C = T << T EW : mixing of H,W to     ~~ ~~ T ~T EW : scattering of H,W from background field ~~ T ~ T EW CPV Resonant CPV: M 1,2 ~  sin    Arg(  M 1 b * ) = Arg(  M 2 b * )

56. Quantum Transport & Baryogenesis Particle Propagation: Beyond familiar (Peskin) QFT LILI Assumptions: 1.Evolution is adiabatic 2.Spectrum is non-degenerate 3.Density is zero Electroweak Baryogenesis 1.Evolution is non-adiabatic: v wall > 0 -> decoherence 2.Spectrum is degenerate: T > 0 -> Quasiparticles mix 3.Density is non-zero

57. + - =+ + … + LILI Generalized Green F’ns Spectral degeneracies Non-adiabaticity Non-equilibrium T>0 Evolution

58. Quantum Transport & Baryogenesis Electroweak Baryogenesis 1.Evolution is non-adiabatic: v wall > 0 -> decoherence 2.Spectrum is degenerate: T > 0 -> Quasiparticles mix 3.Density is non-zero Scale Hierarchy: Fast, but not too fast Hot, but not too hot Dense, but not too dense  d =  v w (k /  << 1  p =  p /  << 1   =  / T << 1 Work to lowest, non- trivial order in  ’s Error is O (  ) ~ 0.1 Cirigliano, Lee, R-M Systematically derive transport eq’s from L new Competing Dynamics CPV Ch eq Cirigliano, Lee,Tulin, R-M

59. Complex Singlet: EWB & DM? Barger, Langacker, McCaskey, R-M Shaugnessy Key features for EWPT & DM: (1)Softly broken global U(1) (2)Closes under renormalization (3)SSB leading to two fields: S that mixes w/ h and A is stable (DM) Controls  CDM & EWPT No domain walls DM mass

60. Complex Singlet: EWB & DM Barger, Langacker, McCaskey, R-M, Shaugnessy  2 controls  CDM & EWPT M H1 = 120 GeV, M H2 =250 GeV, x 0 =100 GeV

61. Complex Singlet: Direct Detection Barger, Langacker, McCaskey, R-M, Shaugnessy Two component case (x 0 =0) Little sensitivity of scaled  SI to  

62. EDMs & EWB: Universal Phases Arg(  M 1 b * ) = Arg(  M 2 b * ) Lower panels: entropy rescaling Present & prospective d e constraints Cirigliano, Li, Profumo, R-M 0910.4589  + -driven EWB  0 -driven EWB

63. EDMs in SUSY One-loop EDM: q, l, n…Chromo-EDM: q, n… Dominant in nuclei & atoms Two-loop EDM only: no chromo-EDMWeinberg: small matrix el’s Decouple in largelimit

64. EDMs in SUSY: Full Two-Loop Higgs Boson Masses Li, Profumo, R-M: PRD 78:075009 (2008) WH Loops dominate for neutron & comparable to  H,  A for electron m A =300 GeV,  =300 GeV, M 2 =2M 1 =290 GeV

65. Key Results: MSSM & Beyond 3. Three-body interactions (typically) drive particle number transfer 4. RH b (s)quark and tau (s)lepton Yukawa interactions critical Y b,  (susy) / Y b,  (sm) = tan  Presence of light sbottoms and staus can quench Y B or change its sign our  Y previous  Y  g H tLtL tLtL tRtR Chung, Garbrecht, R-M, Tulin ‘08

66. Key Results: MSSM & Beyond, cont. 5. Superpartners are generally in equilibrium: “superequilibrium” Supergauge interactions Chain of Yukawa interactions No supergauge No 3rd gen sleptons Full results Exact supereq Chung, Garbrecht, R-M, Tulin ‘09

67. Illustrative Study: MSSM Supergauge Interactions Particle Number Changing Reactions: Yukawa Interactions Dominant in SM Enhanced for moderate tan  “Superequilibrium”: Chung, Garbrecht, R-M, Tulin ‘09 Bubble interior Bubble exterior CPV

68. Quantum Transport Equations =+ + … + Expand in  d,p,  Currents CP violating sources Links CP violation in Higgs and baryon sectors Chiral Relaxation Strong sphalerons Producing n L = 0 S CPV  M,  H,  Y,  SS From S-D Equations: S CPV  M,  H,  Y … Riotto, Carena et al, R-M et al, Konstandin et al R-M et al Objectives: Determine param dep of S CPV and all  s and not just that of S CPV Develop general methods for any model with new CPV Quantify theor uncertainties Approximations Neglect O (   ) terms Others under scrutiny R-M, Chung, Tulin, Garbrecht, Lee, Cirigliano  Y >> other rates? (No) Majorana fermions ? (densities decouple) Particle-sparticle eq? (usually) Vev resummation ?

69. EDMs: Theory Electron Improvements of 10 2 to 10 3 Neutron Neutral Atoms Deuteron QCD Nuclear Schiff Moment Nuclear EDM: Screened in atoms Neutron EDM from LQCD: Two approaches: Expand in  & average over topological sectors (Blum et al, Shintani et al) Compute  E for spin up/down nucleon in background E field (Shintani et al) m N =2.2 GeV QCD SR (Pospelov et al) Hadronic couplings Pospelov et al: PCAC + had models & QCD SR ChPT for d n : van Kolck et al Schiff Screening Atomic effect from nuclear finite size: Schiff moment

70. EDMs & Schiff Moments One-loop EDM: q, l, n…Chromo-EDM: q, n… Dominant in nuclei & atoms Engel & de Jesus: Reduced isoscalar sensitivity (  QCD ) Schiff Moment in 199 Hg Nuclear & hadron structure Liu et al: New formulation of Schiff operator + … New nuclear calc’s needed

71. Dark Matter: Future Experiments Cirigliano, Profumo, R-M Assumes    CDM

72. Dark Matter: Neutrinos in the Sun SUGRA: M 2 ~ 2M 1 AMSB: M 1 ~ 3M 2 Neutralino-driven baryogenesis

73. Dark Matter: Relic Abundance SUGRA: M 2 ~ 2M 1 AMSB: M 1 ~ 3M 2 LEP II Exclusion suppressed too fast Neutralino-driven baryogenesis Non-thermal  

74. Phenomenology: EWPO Electroweak Precision Observables (EWPO) Oblique parameters Similar for S,U… SM: global fit favors light scalar (m h ~ 85 GeV)

75. Phenomenology: EWPO cont’d Electroweak Precision Observables (EWPO) Oblique parameters Global fit (GAPP) Fix m H =114 GeV & fit S,T,U Require O(m 1, m 2, sin  ) - O SM to lie inside 95% CL ellipse

76. SUSY Baryogenesis & Colliders Prospective d e Present d e Prospective d e LHC reach Present d e Prospective d e LHC reach ILC reach

77. Symmetry Breaking Two Cases for at high T: V min = 0 V min = V 0 < 0

78. Electroweak Symmetry Breaking Critical Temperature LEP allowed models: T C ~ 100 GeV |V 0 | / T C 4 << 1

79. Extending the Higgs Sector GUTs: SU(5) example + L soft SUSY Beyond the MSSM       Fileviez Perez, Patel, R-M Ando, Barger, Langacker, Profumo, R-M, Shaugnessy, Tulin