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Electroweak Phase Transition, Scalar Dark Matter, & the LHC

Electroweak Phase Transition, Scalar Dark Matter, & the LHC. M.J. Ramsey-Musolf Wisconsin-Madison. NPAC. Theoretical Nuclear, Particle, Astrophysics & Cosmology. http://www.physics.wisc.edu/groups/particle-theory/. TNT Colloquium, November 2012. Recent Work.

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Electroweak Phase Transition, Scalar Dark Matter, & the LHC

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  1. Electroweak Phase Transition, Scalar Dark Matter, & the LHC M.J. Ramsey-Musolf Wisconsin-Madison NPAC Theoretical Nuclear, Particle, Astrophysics & Cosmology http://www.physics.wisc.edu/groups/particle-theory/ TNT Colloquium, November 2012

  2. Recent Work • M. Gonderinger, Y. Li, H. Patel, & MRM, arXiv:1202.1316 • M. Buckley & MRM JHEP 1109 (2011) 094 • H. Patel & MRM, JHEP 1107 (2011) 029 • C. Wainwright, S. Profumo, MRM Phys Rev. D84 (2011) 023521 • M. Gonderinger, H. Lim, & MRM, Phys. Rev. D86 (2012) 043511 • W. Chao, M. Gonderinger, & MRM, arXiv:1210.0491 Earlier Work • D. O’Connell, MRM, & M.B. Wise, PR D75 (2007) 037701 • S. Profumo, MRM, & G. Shaugnessy, JHEP 0708 (2007) 010 • V. Barger, P. Langacker, M. McCaskey, MRM, & G. Shaugnessy, PR D77 (2008) 035005, D79 (2009) 015018 • P. Fileviez-Perez, H. Patel, MRM & K. Wang, PR D79 (2009) 055024

  3. Stuart J. Freedman

  4. Outline Intro & Motivation EWPT & General Features Three minimal extensions of the Standard Model scalar sector ( How will we know it’s a scalar ? ) ( Theoretical issues )

  5. I. Intro & Motivation

  6. Scalar Fields in Cosmology What role do scalar fields play (if any) in the physics of the early universe ?

  7. Standard Model Hidden Sector (DM) Dark Matter Portals

  8. Scalar Fields & the Higgs Portal

  9. Scalar fields are theoretically problematic m2 ~ 2 Scalar Fields in Particle Physics Scalar fields are a simple Has a fundamental scalar finally been discovered ? If so, is it telling us anything about  ?

  10. Remarkable agreement with EWPO Tension: EWPO + Direct Searches EWPO: data favor a “light” SM-like Higgs scalar What is the BSM Energy Scale  ?

  11. Remarkable agreement with EWPO Agreement w/ SM at ~ 10-3 level:ONP = c / 2 Barbieri & Strumia ‘99 ~ 10 TeV generically What is the BSM Energy Scale  ?

  12. Scalar fields are theoretically problematic m2 ~ 2 Scalar Fields in Particle Physics Scalar fields are a simple Must BSM ~ TeV to maintain a weak scale scalar ? EWPO: for new interactions coupling to gauge bosons or fermions, BSM >> TeV

  13. Scalar fields are theoretically problematic m2 ~ 2 Scalar Fields in Particle Physics Scalar fields are a simple Must BSM ~ TeV to maintain a weak scale scalar ? Perhaps new weak scale physics couples only to scalar sector: “Higgs portal”

  14. Problem Theory Exp’t Scalar Fields in Cosmology • Inflation • Dark Energy • Dark Matter • Phase transitions

  15. EW Symmetry Breaking: Higgs ? QCD: q+g! n,p… Astro: stars, galaxies,.. New Scalars ? Standard Model Universe QCD: n+p! nuclei Scalar Fields & Cosmic History

  16. EW Symmetry Breaking: Higgs ? QCD: q+g! n,p… Astro: stars, galaxies,.. New Scalars ? Standard Model Universe • Flatness • Isotropy • Homogeneity Scalar Field: Inflaton Reheat “Slow roll” QCD: n+p! nuclei Scalar Fields & Inflation

  17. CDM • Supernovae • BAO Cosmological constant ? > 0 Scalar Field: Quintessence ? Scalar Fields & Dark Energy ?

  18. Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation? • BBN ( t ~ 100 s ) • CMB ( t ~ 105 y ) Scalar Fields & the Origin of Matter ?

  19. Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation? Electroweak Phase Transition ? New Scalars • BBN ( t ~ 100 s ) • CMB ( t ~ 105 y ) Scalar Fields & the Origin of Matter ?

  20. Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation? Electroweak Phase Transition ? New Scalars • Rotation curves • Lensing • Bullet clusters Darkogenesis: When? SUSY? Neutrinos? Axions ? YB related ? Scalar Fields & the Origin of Matter ? ?

  21. Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation? Electroweak Phase Transition ? New Scalars: CDM ? • Rotation curves • Lensing • Bullet clusters Darkogenesis: When? SUSY? Neutrinos? Axions ? YB related ? Scalar Fields & the Origin of Matter ? ?

  22. ?  ?  ?  ? Scalar Fields in Cosmology Problem Theory Exp’t • Inflation • Dark Energy • Dark Matter • Phase transitions

  23. Problem Theory Exp’t  • Inflation • Dark Energy • Dark Matter • Phase transitions ?  ?  ?  ? Scalar Fields in Cosmology Could experimental discovery of a fundamental scalar point to early universe scalar field dynamics?

  24. Scalar Fields in Cosmology Problem Theory Exp’t • Inflation • Dark Energy • Dark Matter • Phase transitions  ?  ?  ?  ? Focus of this talk, but perhaps part of larger role of scalar fields in early universe

  25. Questions for this Talk: • Was there a cosmic phase transition at T ~ 100 GeV ? • Did it have the characteristics needed for successful electroweak baryogenesis and/or production of gravity waves? • Are its dynamics coupled to dark matter ? • What are the experimental signatures ? • How robust is the underlying theory ?

  26. II. General Features

  27. * Tree level L = (D y D- V() Quantum corrections V() ) VEFF(,T) • T=0 : Coleman-Weinberg (RG improved) • T>0 : Finite-T effective potential * Many applications: Effective action Effective Potential

  28. 1st order 2nd order Increasingmh New scalars EW Phase Transition: New Scalars

  29. 1st order 2nd order Increasingmh Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars New scalars

  30. 1st order 2nd order Increasingmh Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT New scalars

  31. 1st order 2nd order Increasingmh Bubble nucleation EWSB Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT New scalars

  32. 1st order 2nd order Increasingmh Bubble nucleation Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT New scalars YB : CPV & EW sphalerons EWSB

  33. 1st order 2nd order Increasingmh Bubble nucleation Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT New scalars YB : diffuses into interiors EWSB

  34. 1st order 2nd order Quench EW sph Increasingmh Preserve YBinitial Bubble nucleation Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT New scalars YB : diffuses into interiors EWSB

  35. 1st order 2nd order Increasingmh Preserve YBinitial Bubble nucleation Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT Quench EW sph New scalars YB : diffuses into interiors EWSB TC , Esph, Stunnel F()

  36. 1st order 2nd order Detonation & turbulence Increasingmh Bubble nucleation EWSB BaryogenesisGravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT New scalars

  37. 1st order 2nd order Increasingmh Bubble nucleation BaryogenesisGravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT Detonation & turbulence New scalars EWSB GW Spectra: Q & tEW F()

  38. 1st order 2nd order Increasingmh Bubble nucleation BaryogenesisGravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT Detonation & turbulence nMSSM New scalars EWSB Q tEW GW Spectra: Q & tEW F()

  39. 1st order 2nd order Increasingmh Bubble nucleation BaryogenesisGravity WavesScalar DM ? LHC Searches ? EW Phase Transition: New Scalars “Strong” 1st order EWPT YB preservation, detonation & turbulence New scalars EWSB TC , Esph, Stunnel Q & tEW F()

  40. Higgs Boson Searches

  41. LHC Observation LHC Exclusion LEP, Tevatron, & ATLAS Exclusion Non-SM Higgs(es) ? SM Higgs properties ? SM Higgs? • SM “background” well below new CPV expectations • New expts: 102 to 103 more sensitive • CPV needed for BAU? Precision Tests

  42. Thermal DM: WIMP Direct detection: Spin-indep DM-nucleus scattering  A  SM  A  SM Dark Matter:  & SI

  43. Extension DOF EWPT DM   1  1   2  ?  3 III. Simplest Scalar Extensions Real singlet Real singlet Complex Singlet Real Triplet May be low-energy remnants of UV complete theory & illustrative of generic features

  44. Extension DOF EWPT DM   1  1   2  ?  3 Higgs Portal: Simple Scalar Extensions Real singlet Real singlet Complex Singlet Real Triplet May be low-energy remnants of UV complete theory & illustrative of generic features

  45. Stable S (dark matter?) • Tree-level Z2 symmetry: a1=b3=0 to prevent s-h mixing and one-loop s hh • x0 =0 to prevent h-s mixing Mass matrix H-S Mixing H1 !H2H2 EWPT: a1,2 = 0 & <S> = 0 DM: a1 = 0 & <S> = 0 / / Signal Reduction Factor Independent Parameters: v0, x0, l0, a1, a2, b3, b4 xSM EWPT:  Production Decay The Simplest Extension Model Simplest extension of the SM scalar sector: add one real scalar S (SM singlet) O’Connel, R-M, Wise; Profumo, R-M, Shaugnessy; Barger, Langacker, McCaskey, R-M Shaugnessy; He, Li, Li, Tandean, Tsai; Petraki & Kusenko; Gonderinger, Li, Patel, R-M; Cline, Laporte, Yamashita; Ham, Jeong, Oh; Espinosa, Quiros; Konstandin & Ashoorioon…

  46. Stable S (dark matter?) • Tree-level Z2 symmetry: a1=b3=0 to prevent s-h mixing and one-loop s hh • x0 =0 to prevent h-s mixing Mass matrix H-S Mixing H1 !H2H2 Raise barrier Lower TC : a2 < 0 Signal Reduction Factor Independent Parameters: v0, x0, l0, a1, a2, b3, b4 xSM EWPT:  Production Decay The Simplest Extension Model EWPT Scenario

  47. Finite Temperature Potential Multiple fields & new interactions: novel patters of symmetry breaking, lower TC , greater super-cooling, “stronger 1st order EWPT”

  48. Stable S (dark matter?) • Tree-level Z2 symmetry: a1=b3=0 to prevent s-h mixing and one-loop s hh • x0 =0 to prevent h-s mixing Mass matrix H-S Mixing H1 !H2H2 Signal Reduction Factor Mixing Independent Parameters: v0, x0, l0, a1, a2, b3, b4 Modified BRs Two mixed (singlet-doublet) states w/ reduced SM branching ratios xSM EWPT:  Production Decay The Simplest Extension Model Low energy phenomenology Raise barrier Lower TC

  49. Mixed States h1 = cosh + sins h2 = -sinh + coss

  50. LHC exotic final states: 4b-jets, gg + 2 b-jets… Light: all models Black: LEP allowed LHC: reduced BR(h SM) Scan: EWPT-viable model parameters m2 > 2 m1 m1 > 2 m2 Signal Reduction Factor Production Decay EWPT & LHC Phenomenology Signatures Profumo, R-M, Shaugnessy

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