Higgs Portal & Cosmology: Theory Overview

Transcription

1 Higgs Portal & Cosmology: Theory Overview M.J. Ramsey-Musolf U Mass Amherst Higgs Portal WS May 2014! 1

2 The Origin of Matter Baryons Cosmic Energy Budget Dark Matter 27 % 5 % 68 % Dark Energy

3 The Origin of Matter Baryons Cosmic Energy Budget Dark Matter 27 % 5 % 68 % Dark Energy Explaining the origin, identity, and relative fractions of the cosmic energy budget is one of the most compelling motivations for physics beyond the Standard Model

4 Symmetries & Cosmic History

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

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

7 Symmetries & Cosmic History What is the nature of the EW phase transition? EW Symmetry Breaking: Higgs Standard Model Universe QCD: q+g! n,p QCD: n+p! nuclei Astro: stars, galaxies,..

8 Symmetries & Cosmic History What is the nature of the EW phase transition?! Origin of matter? EW Symmetry Breaking: Higgs Standard Model Universe QCD: q+g! n,p QCD: n+p! nuclei Astro: stars, galaxies,..

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

10 What is the Origin of Matter Baryogenesis: When? CPV? SUSY? Neutrinos?

11 What is the Origin of Matter? Baryogenesis: When? CPV? SUSY? Neutrinos?

12 What is the Origin of Matter? EW Baryogenesis: testable w/ EDMs + colliders Baryogenesis: When? CPV? SUSY? Neutrinos? Leptogenesis: less testable, look for ingredients w/ νs

13 What is the Origin of Matter Baryogenesis: When? CPV? SUSY? Neutrinos?? Leptogenesis: less testable, look for ingredients w/ νs EW Baryogenesis: testable w/ EDMs + colliders Other Scenarios: GUT baryogenesis Affleck-Dine Asymmetric DM Post sphaleron

14 What is the Origin of Matter Baryogenesis: When? CPV? SUSY? Neutrinos?? Leptogenesis: less testable, look for ingredients w/ νs EW Baryogenesis: testable w/ EDMs + colliders Other Scenarios: GUT baryogenesis Affleck-Dine Asymmetric DM Post sphaleron

15 Symmetries & the Origin of Matter? Baryogenesis: When? CPV? SUSY? Neutrinos? Leptogenesis: less testable, look for ingredients w/ νs EW Baryogenesis: testable w/ EDMs + colliders Can new TeV scale physics explain the abundance of matter? If so, how will we know?

16 Questions for This Workshop What happened ~ 10ps after the Big Bang?

17 Questions for This Workshop What happened ~ 10ps after the Big Bang? Single step (cross over) transition? More d.o.f. with a richer pattern of EWSB? Single or multiple steps? First or second order? Coupled to origin of matter?

18 Questions for This Workshop What happened ~ 10ps after the Big Bang? Single step (cross over) transition? More d.o.f. with a richer pattern of EWSB? Single or multiple steps? First or second order? Coupled to origin of matter? What are collider signatures that could provide clues? Modified Higgs properties (production, decays) New states

19 Recent Developments: BICEP2 CMB B-mode observation! Evidence for primordial gravitational radiation associated with inflation Discovery of BEH-like boson! Paradigm of symmetry-breaking in particle physics driven by a fundamental scalar likely correct Non-observation (so far) of physics beyond Supersymmetry the Standard Model as an at illustration the LHC Theoretical progress & challenges Our work

20 Recent Results Discovery of BEH-like scalar at the LHC Non-observation (so far) of sub-tev particles at LHC

21 Recent Results Discovery of BEH-like scalar at the LHC Idea of φ-driven spontaneous EW symmetry breaking is likely correct Non-observation (so far) of sub-tev particles at LHC

22 Recent Results Discovery of BEH-like scalar at the LHC Idea of φ-driven spontaneous EW symmetry breaking is likely correct Non-observation (so far) of sub-tev particles at LHC Sub-TeV BSM spectrum is compressed Sub-TeV BSM is purely EW or Higgs portal BSM physics lies at very different mass scale

23 Outline Portals & the Early Universe Why the Higgs Portal Scalar Fields in Particle Physics & Cosmology General Considerations Illustrative Higgs Portals: Simplest Extensions

24 I. Portals & Early Universe Standard Model Hidden Sector : DM, early universe dynamics (EWPT)

25 Two approaches: Portals Specific model (MSSM.) Model independent

26 Model Independent Portals Vector portal ( dark photons ) Neutrino portal Axion portal Higgs portal Higher dimensional op s portal

27 Model Independent Portals Vector portal ( dark photons ) Neutrino portal Axion portal Higgs portal Higher dimensional op s portal

28 Model Independent Portals Vector portal ( dark photons ) Neutrino portal Axion portal Higgs portal Higher dimensional op s portal

29 Higgs Portal: DM Renormalizable Z 2 symmetric Dimensionless coupling φ (DM): singlet or charged under SU(2) L x U(1) Y

30 Higgs Portal: Phase Transitions + Renormalizable Z 2 symmetric Dimensionless coupling φ (DM): singlet or charged under SU(2) L x U(1) Y

31 Higgs Portal: Higher Dim Op s + Renormalizable Z 2 symmetric Dimensionless coupling χ (DM): singlet or charged under SU(2) L x U(1) Y

32 II. Why the Higgs Portal?

33 Preserving EW Min Stable EW Vacuum? V EFF EW vacuum top loops ϕ sets m H top loops

34 Stable EW Vacuum? Preserving EW Min Funnel plot V EFF EW vacuum top loops perturbativity ϕ sets m H top loops

35 Stable EW Vacuum? Preserving EW Min Funnel plot V EFF EW vacuum top loops perturbativity SM stability & pert vity naïve stability scale Λ ϕ sets m H top loops

36 Stable EW Vacuum? Preserving EW Min Funnel plot V EFF EW vacuum top loops perturbativity SM stability & pert vity naïve stability scale Λ ϕ m H SM unstable above ~ TeV sets m H top loops

37 Stable EW Vacuum? Preserving EW Min Funnel plot V EFF EW vacuum top loops perturbativity SM stability & pert vity naïve stability scale Λ ϕ m H SM unstable above ~ TeV sets m H top loops Higgs portal interactions! more robust stability?

38 What is the BSM Energy Scale Λ? Barbieri & Strumia 99 ~ 10-3 agreement with EWPO BSM: O BSM = c / Λ 2! Λ ~ 10 TeV EWPO: data favor a light SM-like Higgs scalar LHC: so far no sub- TeV BSM physics Higgs Portal: new low scale d.o.f.?

39 III. Scalar Fields in Particle Physics & Cosmology ϕ?

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

41 Scalar Fields in Cosmology Problem Theory Exp t Inflation Dark Energy Dark Matter Phase transitions

42 Scalar Fields in Cosmology Problem Theory Exp t Inflation Dark Energy Dark Matter Phase transitions

43 Scalar Fields in Cosmology Problem Theory Exp t Inflation Dark Energy Dark Matter Phase transitions????

44 Scalar Fields in Cosmology Problem Theory Exp t Inflation Dark Energy Dark Matter Phase transitions Could experimental discovery of additional scalars point to early universe scalar field dynamics? Are there signatures in modified Higgs properties, new states, or EW precision tests?????

45 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

46 IV. General Considerations

47 Thermal DM: Ω CDM & σ SI XENON 100 LUX Thermal DM: WIMP Direct detection: Spin-indep DM-nucleus scattering χ SM χ A χ SM χ A

48 Thermal DM: Ω CDM & σ SI CDMS 2013 K McCarthy APS 13? Thermal DM: WIMP Direct detection: Spin-indep DM-nucleus scattering χ SM χ A χ SM χ A

49 EWPT & EW Baryogenesis

50 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order φ φ

51 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order φ φ Increasing m h

52 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order φ φ Increasing m h New scalars

53 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order Strong 1 st order EWPT φ φ Increasing m h Baryogenesis Gravity Waves Scalar DM LHC Searches New scalars

54 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order Strong 1 st order EWPT φ φ Bubble nucleation Increasing m h Baryogenesis Gravity Waves Scalar DM LHC Searches New scalars EWSB

55 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order Strong 1 st order EWPT φ φ Bubble nucleation Increasing m h New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches Y B : CPV & EW sphalerons EWSB A λ

56 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order Strong 1 st order EWPT φ φ Bubble nucleation Increasing m h New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches Y B : CPV & EW sphalerons BSM EWSB A λ

57 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order Strong 1 st order EWPT φ φ Bubble nucleation Increasing m h New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches Y B : diffuses into interiors EWSB A λ

58 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order Strong 1 st order EWPT Preserve Y B initial Bubble nucleation φ φ Quench EW sph Increasing m h New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches Y B : diffuses into interiors EWSB

59 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order Strong 1 st order EWPT Preserve Y B initial Bubble nucleation φ φ Quench EW sph Increasing m h New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches Y B : diffuses into interiors EWSB

60 EW Phase Transition: Gravity waves F 1st order F 2nd order Strong 1 st order EWPT Detonation & turbulence Bubble nucleation φ φ Increasing m h nmssm New scalars Baryogenesis ΔQ Gravity Waves Scalar DM LHC Searches Δt EW GW Spectra: ΔQ & Δt EW EWSB F(φ)

61 EW Phase Transition: New Scalars & CPV F 1st order F 2nd order Strong 1 st order EWPT Preserve Y B initial Bubble nucleation φ φ Quench EW sph Increasing m h New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches Y B : diffuses into interiors EWSB

62 Electroweak Phase Transition

63 EW Phase Transition: St d Model F 1st order F 2nd order Lattice: Endpoint φ Increasing m h φ v S td Model: 1 st order EWPT requires light Higgs

64 EW Phase Transition: New Scalars F 1st order F 2nd order Lattice: Laine, Rummukainen φ φ CCB Vac Increasing m h New scalars 1 st order EWPT MSSM: Light RH stops PT: Carena et al, Decreasing RH stop mass

65 EW Phase Transition: MSSM F 1st order F 2nd order φ φ CCB vac Increasing m h New scalars MSSM: Light RH stops Carena et al 2008: Higgs phase metastable

66 EW Phase Transition: MSSM F 1st order F 2nd order φ φ CCB vac Increasing m h New scalars MSSM: Light RH stops Carena et al 2008: Higgs phase metastable

67 EW Phase Transition: MSSM F 1st order F 2nd order φ φ CCB vac Increasing m h New scalars MSSM: Light RH stops CMS PAS SUS Carena et al 2008: Higgs phase metastable

68 EW Phase Transition: Higgs Portal F 1st order F 2nd order < φ > φ φ Increasing m h New scalars +

69 EW Phase Transition: Higgs Portal F 1st order F 2nd order < φ > φ φ Increasing m h New scalars + Renormalizable φ : singlet or charged under SU(2) L x U(1) Y Generic features of full theory (NMSSM, GUTS ) More robust vacuum stability Novel patterns of SSB

70 EW Phase Transition: Higgs Portal F 1st order F 2nd order < φ > φ φ Increasing m h New scalars + Renormalizable φ : singlet or charged under SU(2) L x U(1) Y Generic features of full theory (NMSSM, GUTS ) More robust vacuum stability Novel patterns of SSB

71 Higgs Portal: Simple Scalar Extensions Extension DOF EWPT DM Real singlet Real singlet Complex Singlet Real Triplet May be low-energy remnants of UV complete theory & illustrative of generic features

72 Higgs Portal: Simple Scalar Extensions Extension DOF EWPT DM Real singlet Real singlet Complex Singlet Real Triplet May be low-energy remnants of UV complete theory & illustrative of generic features (NMSSM, GUTs, Hidden Valley.)

73 Higgs Portal: Simple Scalar Extensions Extension DOF EWPT DM Real singlet Real singlet Complex Singlet Real Triplet May be low-energy remnants of UV complete theory & illustrative of generic features (NMSSM, GUTs, Hidden Valley.)

74 The Simplest Extension Model Simplest Signal extension Reduction of the Factor SM scalar Tree-level sector: Z 2 symmetry: add one a 1 real =b 3 =0 scalar to S (SM singlet) Stable S (dark matter?) H-S Mixing prevent s-h mixing and one-loop s Mass matrix " M 2 = $ # 2 µ hs 2% " h 1 % 2 ' $ 2 µ s & # h 2 & ' = " $ sinθ / # cosθ / Independent Parameters: µ h 2 2 µ hs v 0, x 0, λ 0, a 1, a 2, b 3, b 4 hh x 0 =0 to prevent h-s mixing xsm EWPT: Production Decay EWPT: a 1,2 = 0 & <S> = 0 DM: a 1 = 0 & <S> = 0 cosθ %" sinθ& ' h% $ # s ' & H 1! H 2 H 2 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

75 The Simplest Extension, Cont d Mass matrix M 2 = " $ # µ h 2 2 µ hs 2 µ hs 2% 2 ' 2 µ s & " $ # h 1 h 2 % & ' = " $ sinθ # cosθ cosθ % sinθ& ' " h % $ # s ' & x 0 = <S>

76 The Simplest Extension, Cont d Mass matrix h 1,2 M 2 = " $ # µ h 2 2 µ hs 2 γ µ hs 2% 2 ' γ 2 µ s & " $ # h 1 % h j h 2 & ' = " $ sinθ # cosθ h k b b cosθ % sinθ& ' " h % γ h k $ # s ' γ& x 0 = <S> New topologies

77 The Simplest Extension, Cont d Mass matrix h 1,2 M 2 = " $ # µ h 2 2 µ hs 2 γ µ hs 2% 2 ' γ 2 µ s & " $ # h 1 % h j h 2 & ' = " $ sinθ # cosθ h k b b cosθ % sinθ& ' " h % γ h k $ # s ' γ& x 0 = <S> Stable S (dark matter) Tree-level Z 2 symmetry: a 1 =0 to prevent s-h mixing and one-loop s x 0 =0 to prevent h-s mixing & s! hh hh

78 The Simplest Extension Model Stable S (dark matter?) Signal Reduction Factor DM Scenario Tree-level Z H-S Mixing 2 symmetry: a 1 =b 3 =0 to prevent s-h mixing and one-loop s hh H 1! H 2 H 2 x 0 =0 to prevent h-s mixing xsm EWPT: Production Decay Mass matrix " M 2 = $ # µ h 2 2 µ hs 2 µ hs 2% 2 ' 2 µ s & " $ # h 1 h 2 % & ' = " $ sinθ # cosθ cosθ %" sinθ& ' h% $ # s ' &

79 The Simplest Extension Model Stable S (dark matter?) Signal Reduction Factor DM Scenario Tree-level Z H-S Mixing 2 symmetry: a 1 =b 3 =0 to prevent s-h mixing and one-loop s hh H 1! H 2 H 2 x 0 =0 to prevent h-s mixing xsm EWPT: Production Decay Mass matrix " M 2 = $ # 2 µ hs 2% " h 1 % 2 ' $ 2 µ s & # h 2 & ' = " sinθ Ω cosθ %" $ # cosθ sinθ& ' h% DM & σ SI $ # s ' & Independent Parameters: µ h 2 2 µ hs v 0, x 0, λ 0, a 1, a 2, b 3, b 4 + +

80 DM Phenomenology Relic Density He, Li, Li, Tandean, Tsai Direct Detection Barger, Langacker, McCaskey, R-M, Shaugnessy He, Li, Li, Tandean, Tsai

81 New Scalars EW Vacuum Stability Preserving EW Min Funnel plot SM stability & pert vity V EFF EW vacuum top loops perturbativity naïve stability scale Λ ϕ m H DM-H coupling top loops Gonderinger, Li, Patel, R-M; Gonderinger, Lim, R-M

82 New Scalars EW Vacuum Stability Preserving EW Min Funnel plot SM stability & pert vity V EFF EW vacuum top loops perturbativity naïve stability scale Λ ϕ m H SM + singlet: stable but non-pertur tive DM-H coupling top loops Gonderinger, Li, Patel, R-M; Gonderinger, Lim, R-M

83 LHC & Higgs Phenomenology LHC discovery potential Signal Reduction Factor Production Decay

84 LHC & Higgs Phenomenology LHC discovery potential Signal Reduction Factor Production Decay V 1j < 1: mixed states h j New decays: h 2! h 1 h 1

85 LHC & Higgs Phenomenology LHC discovery potential Signal Reduction Factor Production Decay V 1j < 1: mixed states h j New decays: h 2! h 1 h 1 Dark matter: no mixing! states are h,s New decays h! SS (invisible!) possible

86 LHC & Higgs Phenomenology LHC discovery potential Invisible decays Signal Reduction Factor He, Li, Li, Tandean, Tsai Production Decay Dijet azimuthal distribution h j Γ (h!ss)=0 A A Invis search Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld 00)

87 LHC & Higgs Phenomenology LHC discovery potential Invisible decays Signal Reduction Factor He, Li, Li, Tandean, Tsai Production Decay Dijet azimuthal distribution Jets + E T h j A A Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld 00)

88 LHC & Higgs Phenomenology LHC discovery potential Invisible decays Signal Reduction Factor ATLAS He, Li, Li, Tandean, Tsai Production Decay Dijet azimuthal distribution h j A A Look for azimuthal shape change of primary jets (Eboli & Zeppenfeld 00)

89 Real Singlet: EWPT Model Stable S (dark matter?) Signal Reduction Factor Tree-level Z H-S Mixing 2 symmetry: a 1 =b 3 =0 to prevent s-h mixing and one-loop s hh H 1! H 2 H 2 x 0 =0 to prevent h-s mixing xsm EWPT: Production Decay Mass matrix " M 2 = $ # µ h 2 2 µ hs 2 µ hs 2% 2 ' 2 µ s & " $ # h 1 h 2 % & ' = " $ sinθ # cosθ cosθ %" sinθ& ' h% $ # s ' &

90 Real Singlet: EWPT Model Stable S (dark matter?) Signal Reduction Factor Tree-level Z H-S Mixing 2 symmetry: a 1 =b 3 =0 to prevent s-h mixing and one-loop s hh H 1! H 2 H 2 x 0 =0 to prevent h-s mixing xsm EWPT: Production Decay Mass matrix 2 2 Raise " µ barrier M 2 = h µ hs 2% $ 2 2 ' # 2 µ s & µ hs " $ # h 1 h 2 % & ' = " sinθ Lower cosθ T %" $ # cosθ sinθ& ' $ h% C # s ' &

91 Real Singlet: EWPT Model Stable S (dark matter?) Signal Low energy Reduction phenomenology Factor Tree-level Z H-S Mixing 2 symmetry: a 1 =b 3 =0 to prevent s-h mixing and one-loop s hh H 1! H 2 H 2 x 0 =0 to prevent h-s mixing xsm EWPT: Production Decay Mass matrix 2 2 Raise " µ barrier M 2 = h µ hs 2% " h 1 % $ 2 2 ' $ # µ hs 2 µ s & # h 2 & ' = " sinθ Lower cosθ T %" $ # cosθ sinθ& ' h% C $ s ' # & Independent Parameters: Mixing v 0, x 0, λ 0, a 1, a 2, b 3, b Modified BRs 4 Two mixed (singlet-doublet) states w/ reduced SM branching ratios

92 EWPT & LHC Phenomenology Signatures m 2 > 2 m 1 Scan: EWPT-viable model parameters Light: all models Black: LEP allowed m 1 > 2 m 2 Profumo, R-M, Shaugnessy 07

93 EWPT & LHC Phenomenology Signatures m 2 > 2 m 1 b LHC exotic final h Scan: EWPT-viable 1 h b states: 2 4b-jets, model parameters h 1 γγ + 2 b-jets γ γ Mixed States: Precision $ ILC Scan: EWPT-viable model parameters Light: all models Black: LEP allowed h 2 h 1 h 2 m 1 > 2 m 2 LHC: reduced BR(h SM) Profumo, R-M, Shaugnessy 07

94 EWPT & LHC Phenomenology Signatures m 2 > 2 m 1 b LHC exotic final h Scan: EWPT-viable 1 h b states: 2 4b-jets, model parameters h 1 γγ + 2 b-jets γ γ Mixed States: Precision $ ILC Scan: EWPT-viable model parameters Light: all models Black: LEP allowed h 2 h 1 h 2 m 1 > 2 m 2 LHC: reduced BR(h SM) Signal Reduction Factor Profumo, R-M, Shaugnessy 07 Production Decay

95 EWPT: Resonant Di-Higgs Production Signatures m 2 > 2 m 1 b LHC exotic final h Scan: EWPT-viable 1 h b states: 2 4b-jets, model parameters h 1 τ + γγ + 2 b-jets τ - Mixed States: Precision $ ILC Scan: EWPT-viable model parameters Light: all models Black: LEP allowed m 2 = 270 GeV un-boosted m 2 = 370 GeV boosted m 1 > 2 m 2 bbτ + τ - : discovery with ~ 100 fb -1 in τ lep τ had channel R-M & No, arxiv:

96 EWPT: Resonant Di-Higgs Production Signatures m 2 > 2 m 1 b LHC exotic final h Scan: EWPT-viable 1 h b states: 2 4b-jets, model parameters h 1 τ + γγ + 2 b-jets τ - Mixed States: Precision $ ILC Scan: EWPT-viable model parameters Light: all models Black: LEP allowed m 2 = 270 GeV un-boosted m 2 = 370 GeV boosted m 1 > 2 m 2 σ) dσ/dm Signal (m 2 Signal (m 2 = 270 GeV) = 370 GeV) Z bb t t Z jj bbτ + τ - : discovery with ~ 100 fb -1 in τ lep τ had channel (1/ h 2 h 1 h 1 t t Zb b Zjj b bτ lep τ had b blτ had b bτ lep τ had b bτ lep τ had jjτ lep τ had Event selection (see section V.C) R bb > 2.1, P T,b1 > 45 GeV, P T,b2 > 30 GeV h 1 -mass: 90 GeV <m bb < 140 GeV Collinear x 1,x 2 Cuts R lτ > m l T < 30 GeV h 1 -mass: 110 GeV <m coll ττ < 150 GeV ET miss < 50 GeV h 2 -mass: 230 GeV <m coll bbττ < 300 GeV σ) dσ/dm (1/ m coll τ τ (GeV) Signal (m 2 Signal (m 2 = 270 GeV) = 370 GeV) Z bb t t Z jj R-M & No, arxiv: mbbτ coll τ (GeV)

97 EWPT & LHC Phenomenology Signatures m 2 > 2 m 1 Mixed States: Precision $ ILC Scan: EWPT-viable model parameters Light: all models Black: LEP allowed m 1 > 2 m 2 Profumo, R-M, Shaugnessy 07

98 Higgs Portal: Simple Scalar Extensions Extension DOF EWPT DM Real singlet Real singlet Complex Singlet Real Triplet Back up slides May be low-energy remnants of UV complete theory & illustrative of generic features

99 Complex Singlet: EWB & DM? Barger, Langacker, McCaskey, R-M Shaugnessy Spontaneously & softly broken global U(1) < S > = 0 Controls Ω CDM, T C, & H-S mixing Gives non-zero M A

100 Complex Singlet: EWB & DM? Barger, Langacker, McCaskey, R-M Shaugnessy Consequences: Three scalars: h 1, h 2 : mixtures of h & S A : dark matter Phenomenology: Produce h 1, h 2 w/ reduced σ Reduce BR (h j! SM) Observation of BR (invis) Possible obs of σ SI

101 Higgs Portal: Simple Scalar Extensions Extension DOF EWPT DM Real singlet Real singlet Complex Singlet Real Triplet Simplest non-trivial EW multiplet

102 Real Triplet Σ 0, Σ +, Σ - ~ ( 1, 3, 0 ) Fileviez-Perez, Patel, Wang, R-M: PRD 79: (2009); [hep-ph] EWPT: a 1,2 = / 0 & <Σ 0 > = / 0 DM & EWPT: a 1 = 0 & <Σ 0 > = 0

103 Real Triplet Σ 0, Σ +, Σ - ~ ( 1, 3, 0 ) Fileviez-Perez, Patel, Wang, R-M: PRD 79: (2009); [hep-ph] EWPT: a 1,2 = / 0 & <Σ 0 > = / 0 DM & EWPT: a 1 = 0 & <Σ 0 > = 0 Small: ρ-param

104 Real Triplet: DM Σ 0, Σ +, Σ - ~ ( 1, 3, 0 ) Fileviez-Perez, Patel, Wang, R-M: PRD 79: (2009); [hep-ph] EWPT: a 1,2 = / 0 & <Σ 0 > = / 0 DM & EWPT: a 1 = 0 & <Σ 0 > = 0 Small: ρ-param

105 EW Phase Transition: Higgs Portal F 1st order F 2nd order <Σ 0 > φ φ Increasing m h New scalars Quench sphalerons Small entropy dilution Real Triplet Σ ~ (1,3,0) Two-step EWPT & dark matter Patel, R-M: arxiv ; Fileviez-Perez, Patel, RM, Wang Baryogenesis Σ dark matter

106 Higgs Diphoton Decays LHC: H! γγ h j h j Σ + SM background D γ well below new CPV expectations D γ New expts: 10 2 to 10 3 more sensitive CPV needed for BAU? Post Moriond 2013 h j D D Fileviez-Perez, Patel, Wang, R-M: PRD 79: (2009); [hep-ph]

107 Real Triplet: EWPT Σ 0, Σ +, Σ - ~ ( 1, 3, 0 ) H. Patel & R-M, /hepph (2012) Two-step EWSB 1. Break SU(2) L x U(1) Y w/ Σ vev 2. Transition to Higgs phase w/ small or zero Σ vev EWB favorable

108 Real Triplet: EWPT Σ 0, Σ +, Σ - ~ ( 1, 3, 0 ) H. Patel & R-M, /hepph (2012) Two-step EWSB 1. Break SU(2) L x U(1) Y w/ Σ vev 2. Transition to Higgs phase w/ small or zero Σ vev EWB favorable

109 Real Triplet : DM Search Mass splitting due to EW symmetry breaking: M ± M 0 4 M W Σ +! Σ 0 + π + (soft) Generalizes to higher dim EW multiplets

110 Real Triplet : DM Search Basic signature: Charged track disappearing after ~ 5 cm qq W ±* H ± H 2 qq Z *,γ * H + H Trigger: Monojet (ISR) + large E T SM Background: QCD jz and jw w/ Z!νν & W!lν Fileviez-Perez, Patel, Wang, R-M: PRD 79: (2009); [hep-ph]

111 Real Triplet : DM Search Basic signature: Charged track disappearing after ~ 5 cm qq W ±* H ± H 2 qq Z *,γ * H + H Trigger: Monojet (ISR) + large E T SM Background: QCD jz and jw w/ Z!νν & W!lν Cuts: large E T hard jet One 5cm track Fileviez-Perez, Patel, Wang, R-M: PRD 79: (2009); [hep-ph]

112 EW Phase Transition: Higgs Portal F 1st order F 2nd order Do good symmetries today need to be good symmetries in the early Universe? φ φ Increasing m h New scalars Patel, R-M, Wise: PRD 88 (2013)

113 Symmetry Breaking & Restoration F 1st order F 2nd order Do good symmetries today need to be good symmetries in the early Universe? φ Increasing m h φ Rochelle salt: KNaC 4 H 4 O 6 4H 2 0 J. Valasek New scalars Piezoelectricity Increasing T!

114 EW Phase Transition: Higgs Portal F 1st order F 2nd order Do good symmetries today need to be good symmetries in the early Universe? No φ Increasing m h New scalars φ O(n) x O(n): Weinberg (1974) SU(5), CP : Dvali, Mohapatra, Senjanovic ( 79, 80 s, 90 s) Cline, Moore, Servant et al (1999) EM: Langacker & Pi (1980) SU(3) C : Patel, R-M, Wise: PRD 88 (2013) Patel, R-M, Wise: PRD 88 (2013)

115 EW Phase Transition: Higgs Portal F 1st order F 2nd order Do good symmetries today need to be good symmetries in the early Universe? No φ Increasing m h New scalars Colored Scalars Color breaking & restoration φ O(n) x O(n): Weinberg (1974) SU(5), CP : Dvali, Mohapatra, Senjanovic ( 79, 80 s, 90 s) Cline, Moore, Servant et al (1999) EM: Langacker & Pi (1980) SU(3) C : Patel, R-M, Wise: PRD 88 (2013) Patel, R-M, Wise: PRD 88 (2013)

116 Color Breaking & Restoration Two illustrative cases: H. Patel, R-M, Wise (2013) Extension DOF EWPT DM Color triplet scalar 6 Color triplet + singlet 7..

117 Color Breaking & Restoration Two illustrative cases: H. Patel, R-M, Wise (2013) Extension DOF EWPT DM Color triplet scalar 6 Color triplet + singlet 7.. Spontaneous B violation

118 EW Phase Transition: Higgs Portal F 1st order F 2nd order 1. Break SU(3) C φ φ Increasing m h 2. Restore SU(3) C New scalars Colored Scalars (triplet) Color breaking & restoration 1. Break SU(3) C 2. Restore SU(3) C Patel, R-M, Wise: PRD 88 (2013)

119 Summary: Workshop Questions What happened ~ 10ps after the Big Bang? Single step (cross over) transition? More d.o.f. with a richer pattern of EWSB? Single or multiple steps? First or second order? Coupled to origin of matter? What are collider signatures that could provide clues? Modified Higgs properties (production, decays) New states

120 Back Up Slides

121 Ingredients for Baryogenesis Standard Model BSM B violation (sphalerons) C & CP violation Out-of-equilibrium or CPT violation

122 Ingredients for Baryogenesis Scenarios: leptogenesis, EW baryogenesis, Afflek- Dine, asymmetric DM, cold baryogenesis, postsphaleron baryogenesis Standard Model BSM B violation (sphalerons) C & CP violation Out-of-equilibrium or CPT violation

123 Ingredients for Baryogenesis Scenarios: leptogenesis, EW baryogenesis, Afflek- Dine, asymmetric DM, cold baryogenesis, postsphaleron baryogenesis Testable Standard Model BSM B violation (sphalerons) C & CP violation Out-of-equilibrium or CPT violation

124 Baryon Number Preservation Washout factor ln S ~ A(T C ) e ζ ζ = F(ϕ) Two qtys of interest: T C from V eff E sph from Γ eff

125 Daisy Resummation Convergence of PT: going beyond expansion Light stop scenario Patel & R-M 11 Csikor 00 For given T, increasingly negative increases difference between two minima Increased ΔV! Lowered T C

126 DM Phenomenology Relic Density He, Li, Li, Tandean, Tsai Higgs pole S H - f S f Direct Detection Barger, Langacker, McCaskey, R-M, Shaugnessy He, Li, Li, Tandean, Tsai

127 Real Triplet: EWPT Σ 0, Σ +, Σ - ~ ( 1, 3, 0 ) H. Patel & R-M, /hepph (2012) Two-step EWSB 1. Break SU(2) L x U(1) Y w/ Σ vev 2. Transition to Higgs phase w/ small or zero Σ vev

128 Real Triplet: EWPT Σ 0, Σ +, Σ - ~ ( 1, 3, 0 ) H. Patel & R-M, /hepph (2012) Two-step EWSB

129 Real Triplet: EWPT Σ 0, Σ +, Σ - ~ ( 1, 3, 0 ) H. Patel & R-M, /hepph (2012) Two-step EWSB 1. Break SU(2) L x U(1) Y w/ Σ vev 2. Transition to Higgs phase w/ small or zero Σ vev

130 Color Breaking & Restoration Two illustrative cases: H. Patel, R-M, Wise (2013) Extension DOF EWPT DM Color triplet scalar 6 Color triplet + singlet 7.. Light : special flavor structure Spontaneous B violation

131 Color Breaking & Restoration Two illustrative cases: H. Patel, R-M, Wise (2013) Extension DOF EWPT DM Color triplet scalar 6 Color triplet + singlet 7.. heavy: generic flavor structure Spontaneous B violation

132 SM + Color Triplet H. Patel, R-M, Wise (2013) Decays: C! <C> = υ C : B violation

133 SM + Color Triplet H. Patel, R-M, Wise (2013) Upper bound on m C :

134 SM + Color Triplet + Singlet H. Patel, R-M, Wise (2013) Heavier colored scalar

135 Higgs Decays: All Channels ATLAS Preliminary W,Z H bb -1 s = 7 TeV: Ldt = 4.7 fb -1 s = 8 TeV: Ldt = 13 fb H ττ -1 s = 7 TeV: Ldt = 4.6 fb -1 s = 8 TeV: Ldt = 13 fb (*) H WW H γγ s = 7 TeV: Ldt = 4.8 fb s = 8 TeV: Ldt = 20.7 fb (*) H ZZ lνlν -1 s = 7 TeV: Ldt = 4.6 fb -1 s = 8 TeV: Ldt = 20.7 fb 4l -1 s = 7 TeV: Ldt = 4.6 fb -1 s = 8 TeV: Ldt = 20.7 fb -1-1 m H = GeV Combined -1 s = 7 TeV: Ldt = fb -1 s = 8 TeV: Ldt = fb µ = 1.30 ± Signal strength (µ)

136 Theoretical Issues Gauge-dependence in V EFF (ϕ, T ) V EFF (ϕ, T )! V EFF (ϕ, T ; ξ ) Ongoing research: approaches for carrying out tractable, GI computations H. Patel & MRM, JHEP 1107 (2011) 029 C. Wainwright, S. Profumo, MRM Phys Rev. D84 (2011) H. Gonderinger, H. Lim, & MRM, arxiv:

137 Origin of Gauge Dependence Effective Action Source term: Not GI Effective Potential

138 Nielsen Identities Identity: Extremal configurations: Effective potential:

139 Baryon Number Preservation Washout factor ln S ~ A(T C ) e ζ ζ = F(ϕ) Two qtys of interest: T C from V eff E sph from Γ eff

140 Baryon Number Preservation: Pert Theory ζ = F(ϕ) Conventional treatments ~ Gauge Dep Baryon number preservation criterion (BNPC) H. Patel & MRM, JHEP 1107 (2011) 029

141 Baryon Number Preservation: Pert Theory ζ = F(ϕ) Conventional treatments ~ Gauge Dep GI T C from hbar exp, V eff (φ + φ), or Hamiltonian formulation Use GI scale in E sph computation Baryon number preservation criterion (BNPC) H. Patel & MRM, JHEP 1107 (2011) 029

142 Nielsen Identities: Application to T C Critical Temperature V eff (ϕ min, T C ) = V eff (0, T C ) Fukuda & Kugo 74: T=0 V EFF Laine 95 : 3D high-t Eff Theory Patel & R-M 11: Full high T Theory Apply consistently order-by-order in Implement minimization order-by-order (defines φ n )

143 Obtaining a GI T C Patel & R-M 11 Track evolution of minima with T using expansion n=1 n=2 n=3 Track evolution of different minima with T using Illustrative results in SM: Full φ