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Low Energy Precision Tests of Supersymmetry

M.J. Ramsey-Musolf Caltech Wisconsin-Madison. Low Energy Precision Tests of Supersymmetry. M.R-M & S. Su, hep-ph/0612057 J. Erler & M.R-M, PPNP 54, 351 (2005). Outline. Motivation: Why New Symmetries ? Why Low Energy Probes ? Prime Suspect: Supersymmetry Low Energy Precision Tests .

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Low Energy Precision Tests of Supersymmetry

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  1. M.J. Ramsey-Musolf Caltech Wisconsin-Madison Low Energy Precision Tests of Supersymmetry M.R-M & S. Su, hep-ph/0612057 J. Erler & M.R-M, PPNP 54, 351 (2005)

  2. Outline Motivation: Why New Symmetries ?Why Low Energy Probes ? Prime Suspect: Supersymmetry Low Energy Precision Tests • Weak Decays • PVES

  3. Motivation Why New Symmetries ?Why Low Energy Probes ?

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

  5. “Known Unknowns” 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? CPV? SUSY? Neutrinos? WIMPy D.M.: Related to baryogenesis? “New gravity”? Lorentz violation? Grav baryogen ? ?

  6. Present universe Early universe Standard Model Gravity A “near miss” for grand unification Is there unification? What new forces are responsible ? High energy desert Weak scale Planck scale Fundamental Symmetries & Cosmic History

  7. Present universe Early universe Unification Neutrino mass Origin of matter Standard Model Weak Int Rates: Solar burning Element abundances Weak scale unstable: Why is GF so large? High energy desert Weak scale Planck scale Fundamental Symmetries & Cosmic History

  8. Supersymmetry, GUT’s, extra dimensions… There must have been additional symmetries in the earlier Universe to • Unify all matter, space, & time • Stabilize the weak scale • Produce all the matter that exists • Account for neutrino properties • Give self-consistent quantum gravity

  9. 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

  10. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Precision Probes of New Symmetries New Symmetries Origin of Matter Unification & gravity Weak scale stability Neutrinos

  11. Probing Fundamental Symmetries beyond the SM: Use precision low-energy measurements to probe virtual effects of new symmetries & compare with collider results • Precision measurements predicted a range for mt before top quark discovery • mt >> mb ! • mt is consistent with that range • It didn’t have to be that way Radiative corrections Direct Measurements Stunning SM Success Precision Probes of New Symmetries J. Ellison, UCI

  12. Precision ~ Mass Scale M=m~ 2 x 10-9 exp ~ 1 x 10-9 M=MW ~ 10-3 Interpretability • Precise, reliable SM predictions • Comparison of a variety of observables • Special cases: SM-forbidden or suppressed processes Precision, low energy measurements can probe for new symmetries in the desert

  13. II. Prime suspect: Supersymmetry

  14. SUSY: a candidate symmetry of the early Universe • Unify all forces • Protect GF from shrinking • Produce all the matter that exists 3 of 4 Yes Maybe so Maybe Probably necessary • Account for neutrino properties • Give self-consistent quantum gravity

  15. Present universe Early universe Standard Model High energy desert Weak scale Planck scale Couplings unify with SUSY Supersymmetry

  16. =0 if SUSY is exact SUSY protects GF from shrinking

  17. c0 Lightest SUSY particle CP Violation Unbroken phase Broken phase SUSY may help explain observed abundance of matter Cold Dark Matter Candidate Baryonic matter: electroweak phase transition

  18. Supersymmetry Fermions Bosons sfermions gauginos Higgsinos Charginos, neutralinos SUSY: a candidate symmetry of the early Universe

  19. SUSY Breaking Superpartners have not been seen Theoretical models of SUSY breaking Visible World Hidden World Flavor-blind mediation 105 new parameters: masses, mixing angles, CPV phases (40) How is SUSY broken? Models: relate weak scale parameters to each other at high scales (“hidden sector”) SUSY must be a broken symmetry

  20. If nature conserves vertices have even number of superpartners • Lightest SUSY particle is stable viable dark matter candidate • Proton is stable • Superpartners appear only in loops SUSY and R Parity Consequences

  21. L=1 WRPV = ijk LiLjEk + ijk LiQjDk +/i LiHu + ijkUiDjDk B=1 proton decay: Set ijk =0 Li, Qi SU(2)L doublets Ei, Ui, Di SU(2)L singlets R-Parity Violation (RPV)

  22. 12k 1j1 12k 1j1 L=1 L=1 RPV : Four-fermion Operators

  23. III. SUSY & Weak Decays

  24. b-decay New physics SUSY Weak Decays & SUSY

  25. Vertex & External leg Drm SUSY Radiative Corrections Propagator Box

  26. 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 & SUSY

  27. Situation Unsettled kaon decay Value of Vusimportant New physics: too small Weak decays

  28. CKM Summary: PDG04 UCNA

  29. Vus & Vud theory ? New 0+ info CKM Summary: New Vus & tn ? New tn !! UCNA

  30. Correlations Non (V-A) x (V-A) interactions: me/E SUSY b-decay at SNS, RIACINO? Weak decays & new physics

  31. Profumo, R-M, Tulin Future exp’t ? Collider signature: SUSY but only SM-like Higgs Is cSB / mf as in SM ? Large c symmetry breaking: New SUSY models Mass suppressed c symmetry breaking: “alignment” models Weak decays & SUSY : Correlations Chiral symmetry breaking in SUSY

  32. SM radiative corrections also have QCD effects SM strong interaction effects: parameterized by Fp Hard to compute To probe effects of new physics in DNEW we need to contend with QCD Pion leptonic decay & SUSY

  33. 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

  34. Present universe Early universe ? ? Bm!e R = Bm!eg Weak scale Planck scale Lepton Flavor & Number Violation MEG: Bm!eg ~ 5 x 10-14 MECO: Bm!e ~ 5 x 10-17 Also PRIME

  35. 0nbb decay Light nM exchange ? m!eg m!e LFV Probes of RPV: LFV Probes of RPV: Heavy particle exchange ? lk11/ ~ 0.09 for mSUSY ~ 1 TeV lk11/ ~ 0.008 for mSUSY ~ 1 TeV Low scale LFV: R ~ O(1) GUT scale LFV: R ~ O(a) Lepton Flavor & Number Violation Raidal, Santamaria; Cirigliano, Kurylov, R-M, Vogel MEG: Bm!eg ~ 5 x 10-14 Logarithmic enhancements of R MECO: Bm!e ~ 5 x 10-17

  36. Short distance contributions Long range nuclear effects (p’s) Lepton Flavor & Number Violation Faessler et al Prezeau, R-M, Vogel

  37. 0nbb signal equivalent to degenerate hierarchy l111/ ~ 0.06 for mSUSY ~ 1 TeV Loop contribution to mn of inverted hierarchy scale Lepton Flavor & Number Violation

  38. IV. SUSY & PVES

  39. Flavor-dependent sin2 Normalization Scale-dependent effective weak mixing Constrained by Z-pole precision observables Flavor-independent QW and SUSY Radiative Corrections Tree Level Radiative Corrections

  40. Vertex & External leg SUSY Radiative Corrections Propagator Box

  41. n is Majorana 12k SUSY loops 12k RPV 95% CL fit to weak decays, MW, etc. Probing SUSY with PV eN Interactions  SUSY dark matter ->e+e Kurylov, Su, MR-M

  42. Large NC for fK+ d QWP, SUSY / QWP, SM d QWe, SUSY / QWe, SM Lattice for fK+ Probing SUSY with PV eN Interactions

  43. 0nbb sensitivity l111/ ~ 0.06 for mSUSY ~ 1 TeV Kurylov, Ramsey-Musolf, Su l12k ~ 0.3 for mSUSY ~ 1 TeV & dQWe/ QWe ~ 5% 95% C.L. JLab 11 GeV Møller Probing SUSY with PV eN Interactions

  44. 0nbb sensitivity l111/ ~ 0.06 for mSUSY ~ 1 TeV m!eg m!e LFV Probes of RPV: LFV Probes of RPV: l12k ~ 0.3 for mSUSY ~ 1 TeV & dQWe/ QWe ~ 5% lk31 ~ 0.03 for mSUSY ~ 1 TeV lk31 ~ 0.15 for mSUSY ~ 1 TeV Probing SUSY with PV eN Interactions

  45. “DIS Parity” SUSY loops E158 &Q-Weak Linear collider JLab Moller RPV 95% CL Comparing Qwe and QWp Kurylov, R-M, Su  SUSY dark matter

  46. e RPV Loops p Comparing AdDIS and Qwp,e

  47. Low Energy Probes of SUSY We’re making progress… …won’t leave until the job is done… …and open to new ideas.

  48. Back Matter

  49. -Nucleus DIS: SUSY Loop Corrections wrong sign

  50. -Nucleus DIS: RPV Effects

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