Lecture V: Electric Dipole Moments and the Baryon Asymmetry M.J. Ramsey-Musolf U Mass Amherst http://www.physics.umass.edu/acfi/ ACFI EDM School November 2016

Lecture V Outline General Considerations Electroweak Baryogenesis Electroweak Phase Transition CPV & EDMs

I. General Considerations

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

Symmetries & Cosmic History EW Symmetry Breaking: Higgs Standard Model Universe 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

Symmetries & Cosmic History EW Symmetry Breaking: Higgs BSM Physics? Standard Model Universe 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

Symmetries & Cosmic History EW Symmetry Breaking: Higgs Standard Model Universe How did we go from nothing to something ? 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

Cosmic Baryon Asymmetry Cosmic Microwave Bcknd: Shape of anisotropies depends on YB Big Bang Nucleosynthesis: Light element abundances depend on YB

Cosmic Baryon Asymmetry Big Bang Nucleosynthesis: Light element abundances depend on YB

Cosmic Baryon Asymmetry Cosmic Microwave Bcknd: Shape of anisotropies depends on YB

Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? ? C: Charge Conjugation P: Parity 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

Cosmic Baryon Asymmetry One number ! BSM Physics

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

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

Cosmic Baryon Asymmetry One number ! IIII IIII IIII … Explanations BARYOGENESIS THEORIES Theory

Cosmic Baryon Asymmetry One number ! IIII IIII IIII … Explanations Experiment can help: BARYOGENESIS THEORIES Discover ingredients Falsify candidates Theory

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

Ingredients for Baryogenesis Scenarios: leptogenesis, EW baryogenesis, Afflek-Dine, asymmetric DM, cold baryogenesis, post-sphaleron baryogenesis… Ingredients? Standard Model BSM    B violation (sphalerons) C & CP violation Out-of-equilibrium or CPT violation

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

Baryogenesis Scenarios 1012 Standard thermal lepto 109 Affleck Dine Energy Scale (GeV) Electroweak, resonant lepto, WIMPY baryo, ARS lepto… 10 2 10-1 Post-sphaleron, cold…

Baryogenesis Scenarios 1012 Standard thermal lepto 109 Affleck Dine Energy Scale (GeV) Electroweak, resonant lepto, WIMPY baryo, ARS lepto… 10 2 10-1 Post-sphaleron, cold… Most directly testable

Baryogenesis Scenarios Discover (some) ingredients & possibly falsify 1012 Standard thermal lepto 109 Affleck Dine Energy Scale (GeV) Electroweak, resonant lepto, WIMPY baryo, ARS lepto… 10 2 10-1 Post-sphaleron, cold… Most directly testable

Baryogenesis Scenarios Discover (some) ingredients & possibly falsify 1012 Standard thermal lepto 109 Affleck Dine Energy Scale (GeV) EDMs ! Electroweak, resonant lepto, WIMPY baryo, ARS lepto… 10 2 10-1 Post-sphaleron, cold… Most directly testable

Electroweak Baryogenesis Was YB generated in conjunction with electroweak symmetry-breaking?

Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? EW Baryogenesis: testable w/ EDMs + colliders Leptogenesis: look for ingred’s w/ s: DBD,  osc 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

II. Electroweak Baryogenesis

Electroweak Baryogenesis Ingredients Baryon number violation Strong first order electroweak phase transition Effective CPV

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

Electroweak Baryogenesis Ingredients Baryon number violation Strong first order electroweak phase transition Effective CPV

Electroweak Sphalerons Sphaleron Configuration

Electroweak Sphalerons Sphaleron Configuration D (B+L) / NF Anomaly

Electroweak Baryogenesis Ingredients Baryon number violation Strong first order electroweak phase transition Effective CPV

Symmetries & Cosmic History EW Symmetry Breaking: Higgs What is the nature of the EW phase transition ? Standard Model Universe 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: n+p! nuclei QCD: q+g! n,p… Astro: stars, galaxies,..

BEH-like Boson Observation

EWSB: The Scalar Potential From Nature What was the thermal history of EWSB ?

EWSB: The Scalar Potential From Nature What was the thermal history of EWSB ?

Scalar Potential: Thermal History Single-Step EWSB Constrained by experiment, but not the only possibility

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

EW Phase Transition: New Scalars & CPV 1st order 2nd order Increasing mh

EW Phase Transition: New Scalars “Strong” 1st order EWPT Bubble nucleation 1st order 2nd order EWSB Increasing mh SM: 1st order EWPT endpoint

EW Phase Transition: St’d Model 1st order 2nd order Increasing mh SM EW: Cross over transition Temperature Higgs Mass EW Phase Diagram 125 GeV How does this picture change in presence of new TeV scale physics ? What is the phase diagram ?

EW Phase Transition: New Scalars “Strong” 1st order EWPT Bubble nucleation 1st order 2nd order EWSB Increasing mh New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches Novel EWSB patterns New states Higgs prop’s

Electroweak Baryogenesis Ingredients Baryon number violation Strong first order electroweak phase transition Effective CPV

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

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

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

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

III. Electroweak Phase Transition Did the conditions for EWBG exist ?

The Higgs Portal

Portals & Early Universe Standard Model Hidden Sector “Singlets”

EW Phase Transition: Higgs Portal 1st order 2nd order <  > Increasing mh “Higgs Portal” New scalars New scalars that interact with SM via the Higgs +… +…

EW Phase Transition: New Scalars 1st order 2nd order Increasing mh Scan: EWPT-viable model parameters Light: all models Black: LEP allowed New scalars Real Singlet: f ! S Simplest Extension: two states h1 & h2 Profumo, R-M, Shaugnessy JHEP 0708 (2007) 010

EW Phase Transition: St’d Model 1st order 2nd order Increasing mh SM EW: Cross over transition EW Phase Diagram Singlets Temperature 125 GeV Higgs Mass How does this picture change in presence of new TeV scale physics ? What is the phase diagram ?

Experimental Probes: Energy Frontier CMS ATLAS LHC International Linear Collider Future Circular e+e- & pp Thanks: S. Gascon-Shotkin

EW Phase Transition: New Scalars 1st order 2nd order Increasing mh m2 > 2 m1 Mixed States: Precision $ ILC, CPEC, FCC-ee New scalars Real Singlet: f ! S Simplest Extension: two states h1 & h2 m1 > 2 m2 Profumo, R-M, Shaugnessy JHEP 0708 (2007) 010

EW Phase Transition: New Scalars 1st order 2nd order Increasing mh m2 > 2 m1 Mixed States: Precision $ ILC, CPEC, FCC-ee New scalars Novel signatures: Simplest Extension: two states h1 & h2 t+ t- m1 > 2 m2 No & RM, arXiv:1310.6035 : LHC Discovery w/ 100 fb-1

EW Phase Transition: New Scalars 1st order 2nd order Increasing mh Next gen pp m2 > 2 m1 Mixed States: Precision $ ILC, CPEC, FCC-ee New scalars Novel signatures: Simplest Extension: two states h1 & h2 t+ t- LHC m2 ! m1 > 2 m2 Next gen pp: Kotwal, No, R-M, Winslow 1604.XXXX

EW Phase Transition: New Scalars 1st order 2nd order Modified Higgs Self-Coupling m2 > 2 m1 Mixed States: Precision $ ILC, CPEC, FCC-ee h1 m1 > 2 m2

EW Phase Transition: New Scalars 1st order 2nd order Modified Higgs Self-Coupling m2 > 2 m1 Increasing mh New scalars Mixed States: Precision $ ILC, CPEC, FCC-ee m1 > 2 m2 Profumo, R-M, Wainwright, Winslow: 1407.5342

EW Phase Transition: New Scalars 1st order 2nd order Modified Higgs Self-Coupling m2 > 2 m1 Increasing mh New scalars FCC-hh/SPPC FCC-ee/ CEPC HL-LHC ILC Mixed States: Precision $ ILC, CPEC, FCC-ee m1 > 2 m2 Profumo, R-M, Wainwright, Winslow: 1407.5342

IV. CPV & EDMs Did sufficiently effective CPV interactions occur ?

CPV in EW Baryogenesis Unbroken phase Topological transitions MSSM: Chung, Garbrecht, R-M, Tulin ‘09 Bubble interior Bubble exterior LH leptons LH quarks LH fermions BSM CPV Unbroken phase Broken phase CP Violation & Transport Transport: A Competition CPV Chem Eq R-M et al Diffusion MSSM: ~ 30 Coupled Eqns Thanks: B. Garbrecht

EDMs & EWBG: MSSM & Beyond f V g ~ Heavy sfermions: LHC consistent & suppress 1-loop EDMs Sub-TeV EW-inos: LHC & EWB -viable but non-universal phases Compatible with observed BAU de = 10-28 e cm ACME: ThO dn = 10-27 e cm sin(M1b*) sin(M1b*) de = 10-29 e cm dn = 10-28 e cm Next gen de Next gen dn Li, Profumo, RM ‘09-’10 Compressed spectrum

Origin of the resonant behavior VC, C.Lee, MJRM, S.Tulin, 0912.3523, 1106.0747 Particles involved in EWB mix through v(x) When m1 ~ m2 one has maximal mixing and maximal Losc Behavior controlled by Lw vs Losc = 2π vrel/(ω1 - ω2) vs Lcoll Resonant enhancement due to non-adiabatic evolution (Losc/Lw >> 1) Analogy with spin 1/2 in external t-dependent magnetic field. x y B x(T-1) BROKEN PHASE UNBROKEN right-moving modes

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

CPV for EWBG EDM Back up slides & discussion Theoretical creativity

Back Up Slides

Did EWSB Happen Only Once ? Not necessarily BSM “non-singlets” ! Multi-step EWSB

EW Phase Transition: New Scalars <> 1st order 2nd order Increasing mh New scalars Real Triplet  Two-step EWPT & dark matter Patel, R-M, PRD 88 (2013) 035013 ; Fileviez-Perez, Patel, RM, Wang, PRD 79 (2009) 055024

EW Phase Transition: New Scalars <> 1st order 2nd order Increasing mh Small entropy dilution Quench sphalerons New scalars Real Triplet  Baryogenesis Two-step EWPT & dark matter  dark matter Patel, R-M, PRD 88 (2013) 035013

LHC Tests: Modified Higgs Properties    <> 1st order 2nd order S Mass (GeV) SS H Coupling Two-step EWB favorable Patel, R-M, PRD 88 (2013) 035013

LHC Tests: Modified Higgs Properties    <> 1st order 2nd order S Mass (GeV) SS H Coupling EWB favorable HL-LHC, FCC-ee /CPEC ILC 250 Patel, R-M, PRD 88 (2013) 035013

Two-Step EW Baryogenesis Quench sphalerons Small entropy dilution  dark matter Illustrative Model: New sector: “Real Triplet” S Gauge singlet S <f> H ! Set of “SM” fields: 2 HDM Two CPV Phases: dS : Triplet phase dS : Singlet phase Inoue, Ovanesyan, R-M: 1508.05404

Two-Step EW Baryogenesis & EDMs EDMs are Two Loop Two CPV Phases: dS : Triplet phase dS : Singlet phase Insensitive to dS : electrically neutral ! “partially secluded” Inoue, Ovanesyan, R-M: 1508.05404

Illustrative Model: Results Two cases: (A) dS = 0 (B) dS =0 YB Triplet CPV Singlet CPV Present de Future dn Future dp ? Present de No EDM constraints Inoue, Ovanesyan, R-M: 1508.05404

Flavored EW Baryogenesis tL EWBG by mR

Flavored EW Baryogenesis tL EWBG by mR Flavor basis (high T) Mass basis (T=0) Guo, Li, Liu, R-M, Shu 1609.09849

Flavored EW Baryogenesis tL EWBG by mR Flavor basis (high T) Mass basis (T=0) CPV h ! tt Guo, Li, Liu, R-M, Shu 1609.09849

Flavored EW Baryogenesis tL EWBG by mR Flavor basis (high T) Mass basis (T=0) CPV h ! tt EWBG viable Guo, Li, Liu, R-M, Shu 1609.09849

EW Phase Transition: New Scalars & CPV 1st order 2nd order Increasing mh New scalars

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

Symmetries & Cosmic History EW Symmetry Breaking: Higgs BSM Physics? Standard Model Universe How did we go from nothing to something ? 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe How did we go from nothing to something ? 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..

Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? EW Baryogenesis: testable w/ EDMs + colliders Leptogenesis: look for ingred’s w/ s: DBD,  osc 10-35 s 10-11 s 10-5 s ~ 1 m 380k yr QCD: q+g! n,p… QCD: n+p! nuclei Astro: stars, galaxies,..