Lecture V: Electric Dipole Moments and the Baryon Asymmetry

Lecture V: Electric Dipole Moments and the Baryon Asymmetry
M.J. Ramsey-Musolf U Mass Amherst 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,..

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,..

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,..

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

Big Bang Nucleosynthesis: Light element abundances depend on YB

Cosmic Microwave Bcknd: Shape of anisotropies depends on YB

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,..

One number ! BSM Physics

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

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

One number ! IIII IIII IIII … Explanations BARYOGENESIS THEORIES Theory

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

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

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

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…

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

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

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?

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 Sphalerons
Sphaleron Configuration

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

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 ?

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

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 ?

“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

“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

“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

“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

“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 +… +…

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

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

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: : LHC Discovery w/ 100 fb-1

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 XXXX

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

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:

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:

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 = e cm ACME: ThO dn = e cm sin(M1b*) sin(M1b*) de = e cm dn = 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, , 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

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

<> 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)

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)

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)

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:

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:

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:

Flavored EW Baryogenesis
tL EWBG by mR

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

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

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

1st order 2nd order Increasing mh New scalars

“Strong” 1st order EWPT Bubble nucleation 1st order 2nd order EWSB Increasing mh New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches

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,..

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,..

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,..

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,..

Lecture V: Electric Dipole Moments and the Baryon Asymmetry

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Lecture V: Electric Dipole Moments and the Baryon Asymmetry

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