Chiral Symmetries and Low Energy Searches for New Physics

1. Chiral Symmetries and Low Energy Searches for New Physics M.J. Ramsey-Musolf Caltech Wisconsin-Madison

2. Fundamental Symmetries & Cosmic History • What were the fundamental symmetries that governed the microphysics of the early universe? • Were there additional (broken) chiral symmetries? • What insights can low energy (E << MZ) precision electroweak studies provide? • How does the approximate chiral symmetry of QCD the affect low energy search for new symmetries?

3. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History

4. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Puzzles the Standard Model can’t solve Origin of matter Unification & gravity Weak scale stability Neutrinos What are the symmetries (forces) of the early universe beyond those of the SM?

5. Large Hadron Collider Ultra cold neutrons LANSCE, NIST, SNS, ILL CERN What are the new fundamental symmetries? Two frontiers in the search Collider experiments (pp, e+e-, etc) at higher energies (E >> MZ) Indirect searches at lower energies (E < MZ) but high precision Particle, nuclear & atomic physics High energy physics

6. What are the new fundamental symmetries? • Why is there more matter than antimatter in the present universe? • What are the unseen forces that disappeared from view as the universe cooled? • What are the masses of neutrinos and how have they shaped the evolution of the universe? Electric dipole moment & dark matter searches Precision electroweak: weak decays & e- scattering Neutrino interactions & 0nbb-decay Tribble report

7. Cosmic Energy Budget Electroweak symmetry breaking: Higgs ? Weak scale baryogenesis can be tested experimentally Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Baryogenesis: When? SUSY? Neutrinos? CPV? WIMPy D.M.: Related to baryogenesis? “New gravity”? Grav baryogenesis? ?

8. Cosmic Energy Budget Dark Matter BBN WMAP Searches for permanent electric dipole moments (EDMs) of the neutron, electron, and neutral atoms probe new CP-violation Dark Energy T-odd , CP-odd by CPT theorem Baryons What are the quantitative implications of new EDM experiments for explaining the origin of the baryonic component of the Universe ? Chiral odd SU(2)L x U(1)Y invariant for L >> Mweak SM CPV Yukawa suppressed Beyond SM CPV may not be (e.g., SUSY) What is the origin of baryonic matter ?

9. CKM fdSM dexp dfuture Also 225Ra, 129Xe, d If new EWK CP violation is responsible for abundance of matter, will these experiments see an EDM? EDM Probes of New CP Violation

10. Scale Hierarchy: Expand in energy & time scale ratios Weak Scale Baryogenesis Cirigliano, Lee, R-M • B violation • C & CP violation • Nonequilibrium dynamics Topological transitions Theoretical Issues: Transport at phase boundary (non-eq QFT) Bubble dynamics (numerical) Strength of phase transition (Higgs sector) EDMs: many-body physics & QCD Broken phase 1st order phase transition Sakharov, 1967 • Is it viable? • Can experiment constrain it? • How reliably can we compute it? Baryogenesis: New Electroweak Physics 90’s: Cohen, Kaplan, NelsonJoyce, Prokopec, Turok Unbroken phase CP Violation

11. Supersymmetry Fermions Bosons sfermions gauginos Higgsinos Charginos, neutralinos Baryogenesis & Dark Matter: SUSY

12. M1 0 -mZ cosb sinqW mZ cosb cosqW T ~TEW : scattering of H,W from background field MN = ~ ~ T ~ TEW mZ sinb sinqW M2 -mZ sinb sinqW 0 CPV 0 -m -mZ cosb sinqW mZ cosb cosqW -m T << TEW : mixing of H,W to c+, c0 mZ sinb sinqW -mZ sinb sinqW 0 ~ ~ ~ ~ M2 • = N11B 0 + N12W 0 + N13Hd0 + N14Hu0 MC = m T << TEW BINO WINO HIGGSINO Baryogenesis & Dark Matter: SUSY Chargino Mass Matrix Neutralino Mass Matrix

13. Neutralino-driven baryogenesis Baryogenesis | sin fm | > 0.02 | de , dn | > 10-28 e-cm Mc < 1 TeV LEP II Exclusion Two loop de Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 EDM constraints & SUSY CPV

14. Assuming Wc ~ WCDM Cirigliano, Profumo, R-M Dark Matter: Future Experiments

15. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Precision Ewk Probes of New Symmetries Unseen Forces: Supersymmetry ? Unification & gravity Weak scale stability Origin of matter Neutrinos

16. CKM unitarity ? Flavor-blind SUSY-breaking 12k R ParityViolation Kurylov, R-M, Su CKM Unitarity MW CKM, (g-2)m, MW, Mt ,… APV l2 b-decay 12k 1j1 1j1 No long-lived LSP or SUSY DM New physics Kurylov, R-M RPV SUSY Weak decays & new physics See Moulson, Cirigliano

17. Correlations Non (V-A) x (V-A) interactions: me/E b-decay at SNS,“RIAcino”? SUSY Weak decays & SUSY

18. Profumo, R-M, Tulin Future exp’t ? Large L-R mixing: New models for SUSY-breaking Yukawa suppressed L-R mixing: “alignment” models Weak decays & SUSY : Correlations SUSY loop-induced operators with mixing between L,R chiral supermultiplets

19. SM radiative corrections important for precise FpHolstein, Marciano & Sirlin RPV SUSY Pion leptonic decay & SUSY A non-zero DNEW would shift Fp

20. Leading QCD uncertainty: Marciano & Sirlin Probing Slepton Universality vs Min (GeV) Tulin, Su, R-M Prelim New TRIUMF, PSI Can we do better on ? Pion leptonic decay & SUSY

21. “Weak Charge” ~ 1 - 4 sin2 qW ~ 0.1 Lepton Scattering & New Symmetries Parity-Violating electron scattering

22. n is Majorana 12k SUSY loops  SUSY dark matter 12k RPV 95% CL fit to weak decays, MW, etc. Probing SUSY with PV eN Interactions Kurylov, Su, MR-M

23. “DIS Parity” SUSY loops E158 &Q-Weak Linear collider JLab Moller RPV 95% CL Probing SUSY with PV eN Interactions Kurylov, R-M, Su  SUSY dark matter  SUSY dark matter

24. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Neutrinos ? LFV & LNV ? Are they their own antiparticles? Why are their masses so small? Can they have magnetic moments? Implications of mnfor neutrino interactions ?

25. mn< 10-14mB Dirac mnem< 10-9-10-12mB Majorana Neutrino Mass & Magnetic Moments Bell, Cirigliano, Gorshteyn,R-M, Vogel, Wang, Wise Davidson, Gorbahn, Santamaria How large is mn ? Experiment: mn< (10-10 - 10-12) mB e scattering, astro limits Radiatively-induced mn Both operators chiral odd

26. 3/4 0 3/4 1 TWIST (TRIUMF) Muon Decay & Neutrino Mass

27. mn MPs Constraints on non-SM Higgs production at ILC: mn , m- and b-decay corr constrained by mn Also b-decay, Higgs production Erwin, Kile, Peng, R-M 06 Prezeau, Kurylov 05 First row CKM Correlations in Muon Decay & mn Model Independent Analysis 2005 Global fit: Gagliardi et al. Model Dependent Analysis

28. Light nM : 0nbb-decay rate may yield scale of mn How do we compute & separate heavy particle exchange effects? Neutrino Mass & 0n bb - decay

29. How do we compute & separate heavy particle exchange effects? 4 quark operator: low energy EFT Neutrino Mass & 0n bb - decay

30. RPV SUSY No WR - WL mixing WR - WL mix L(q,e) = Chiral properties of Oj++ determine p-dependence of Kpp , KpNN , KNNNN Kpp ~ O (p0) Kpp ~ O (p2) Neutrino Mass & 0n bb - decay Prezeau, R-M, & Vogel

31. Conclusions • Low energy probes of physics beyond the SM give us a unique window on the fundamental symmetries of the early universe that complements direct searches for new physics at colliders • These symmetries - including broken chiral symmetries - are needed to explain the origin of matter, provide for stability of the electroweak scale, incorporate new forces implied by unification, and account for the properties of neutrinos • The broken chiral symmetry of QCD also provides an important tool for sharpening Standard Model predictions for low energy observables and making any deviations interpretable in terms of new symmetries