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Scalar Dark Matter and the Higgs Portal

Scalar Dark Matter and the Higgs Portal. M.J. Ramsey-Musolf Wisconsin-Madison. NPAC. Theoretical Nuclear, Particle, Astrophysics & Cosmology. http://www.physics.wisc.edu/groups/particle-theory/. SSNuDM, Shanghai, September 2012. Outline. Dark Matter Portals Why the Higgs portal?

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Scalar Dark Matter and the Higgs Portal

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  1. Scalar Dark Matter and the Higgs Portal M.J. Ramsey-Musolf Wisconsin-Madison NPAC Theoretical Nuclear, Particle, Astrophysics & Cosmology http://www.physics.wisc.edu/groups/particle-theory/ SSNuDM, Shanghai, September 2012

  2. Outline Dark Matter Portals Why the Higgs portal? Why scalar dark matter ? Simplest examples: scalar DM & LHC Long-range dark forces • Supersymmetry as an illustration • Theoretical progress & challenges • Our work

  3. Standard Model Hidden Sector (DM) I. Dark Matter Portals

  4. BSM Physics: EFT Framework Thanks: Adam Ritz EFT: Integrate out heavy DOF & retain only light DOF w/ M << 

  5. Portals Thanks: Adam Ritz

  6. “dark photons” Classifying Portals Thanks: Adam Ritz

  7. Mediator mass Classifying Portals ! scalar DM ! fermionic DM Thanks: Adam Ritz

  8. Classifying Portals Thanks: Adam Ritz

  9. II. Why the Higgs Portal ?

  10. Higgs Boson Searches

  11. Higgs Boson Searches SM Higgs?

  12. 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

  13. 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  ?

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

  15. 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  ?

  16. 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

  17. 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 ?

  18. 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”

  19.  ? III. Why scalar dark matter ?

  20. Scalar Fields & Early Universe

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

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

  23. EW Symmetry Breaking: Higgs ? QCD: q+g! n,p… Astro: stars, galaxies,.. New Forces ? Standard Model Universe QCD: n+p! nuclei Symmetries & Cosmic History

  24. EW Symmetry Breaking: Higgs ? New Forces ? Standard Model Universe SUSY ? GUTS ? Extra Dims ? ~ WL Terascale Symmetries & Cosmic History WR NR WL* Puzzles the Standard Model can’t solve Origin of matter Unification & gravity Weak scale stability Neutrinos

  25. 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

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

  27. Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation? Scalar Fields & the Origin of Matter ?

  28. Baryogenesis: When? CPV? SUSY? Neutrinos? Non-equilibrium dynamics or CPT violation? Electroweak Phase Transition ? New Scalars Scalar Fields & the Origin of Matter ?

  29. 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 ? ?

  30. 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 ? ?

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

  32. 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?

  33. 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

  34. Electroweak Phase Transition

  35. 1st order 2nd order Increasingmh New scalars EW Phase Transition: New Scalars

  36. 1st order 2nd order Increasingmh Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars New scalars

  37. 1st order 2nd order Increasingmh Baryogenesis Gravity Waves Scalar DM LHC Searches EW Phase Transition: New Scalars “Strong” 1st order EWPT New scalars

  38. 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

  39. 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

  40. 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

  41. 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()

  42. 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()

  43. 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()

  44. 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

  45. 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()

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

  47. IV. Simple examples

  48. 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

  49. 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…

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