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Fundamental Symmetries of the Early Universe: The Standard Model & Beyond M.J. Ramsey-Musolf Caltech Wisconsin-Madison QuickTime™ and a TIFF (U ncompressed) decompressor are needed to see this picture. Fundamental Symmetries & Cosmic History • What were the fundamental symmetries that governed the microphysics of the early universe? The (broken) symmetries of the Standard Model of particle physics work remarkably well at late times, but they leave many unsolved puzzles pertaining to the early universe • What insights can low energy (E << MZ) precision electroweak studies provide? New forces and their symmetries generally imply the existence of new particles. Looking for their footprints in low energy processes can yield important clues about their character Outline I. Motivation: Why New Symmetries ? Why Low Energy Probes ? II. Brief Interlude: Supersymmetry III. Three Probes, Three Questions: Electric dipole moments & the origin of Matter Weak decays, lepton scattering & new forces Neutrino mass and interactions I. Motivation Why New Symmetries ? Why Low Energy Probes ? Fundamental Symmetries & Cosmic History Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History It utilizes a simple and elegant symmetry principle SU(3)c x SU(2)L x U(1)Y to explain the microphysics of the present universe • Big Bang Nucleosynthesis (BBN) & light element abundances • Weak interactions in stars & solar burning •Standard Supernovae & neutron Model puzzles stars Standard Model successes Fundamental Symmetries & Cosmic History Electroweak symmetry breaking: Higgs ? • Non-zero vacuum expectation value of neutral Higgs breaks electroweak sym and gives mass: • Where is the Higgs particle? Puzzles the St’d Model may or may not solve: SU(3)c x SU(2)L x U(1)Y U(1)EM How is electroweak symmetry broken? How do elementary particles getsuccesses mass ? • Is Standard there more Model than puzzles Standard Model one? Fundamental Symmetries & Cosmic History Electroweak symmetry Puzzles the Standard Model can’t solve breaking: Higgs ? 1. 2. 3. 4. Origin of matter Unification & gravity Weak scale stability Neutrinos Beyond the SM What are the symmetries (forces) of the early universe beyond those of the SM? SM symmetry (broken) Fundamental Symmetries & Cosmic History Electroweak symmetry breaking: Higgs ? Baryogenesis: When? CPV? SUSY? Neutrinos? WIMPy D.M.: Related to baryogenesis? “New gravity”? Lorentz violation? Effects on CMB? • C: Charge Conjugation ? • P: Parity Beyond the SM SM symmetry (broken) Cosmic Energy Budget Fundamental Symmetries & Cosmic History Early universe Present universe Unification? Use gauge coupling energydependence look back in time Standard Model 4 2 gi Weak scale e e() g g() High energy desert log 10 ( / 0 )Energy Scale ~ T Planck scale Fundamental Symmetries & Cosmic History Early universe Present universe Standard Model 4 for A “near miss” 2 grand unification g Gravity i Is there unification? What new forces are responsible ? Weak scale High energy desert log 10 ( / 0 ) Planck scale Fundamental Symmetries & Cosmic History Early universe 2 GF ~ 1 Muniverse Present W EAK Weak Int Rates: Solar burning Element abundances Standard Model 4 Weak scale 2 gi unstable: Why is GF so large? Weak scale Unification Neutrino mass Origin of matter High energy desert log 10 ( / 0 ) Planck scale 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 Supersymmetry, GUT’s, extra dimensions… What are the new fundamental symmetries? Two frontiers in the search Collider experiments Indirect searches at (pp, e+e-, etc) at higher lower energies (E < MZ) energies (E >> MZ) but high precision Large Hadron Collider Ultra cold neutrons CERN High energy physics LANSCE, NIST, SNS, ILL Particle, nuclear & atomic physics Precision, low energy measurements can probe for new symmetries in the desert Precision ~ Mass Scale NEW O M SM O M˜ NEW 2 M=m ~ 2 x 10-9 M=MW exp ~ 1 x 10-9 ~ 10-3 Interpretability • Precise, reliable SM predictions • Comparison of a variety of observables • Special cases: SM-forbidden or suppressed processes II. Brief Interlude: Supersymmetry SUSY: a candidate symmetry of the early Universe • Unify all forces 3 of 4 • Protect GF from shrinking Yes • Produce all the matter that exists Maybe so • Account for neutrino properties Maybe • Give self-consistent quantum gravity Probably necessary SUSY: a candidate symmetry of the early Universe Supersymmetry Fermions Bosons e L,R , q L,R e˜ L,R , q˜ L,R ˜ , Z˜ , ˜, g ˜ W ˜ ,H ˜ Higgsinos H u d W, Z , , g gauginos sfermions Hu,Hd 0 ˜ , Z˜ , ˜ ˜, H ˜ ˜ W , u, d Charginos, neutralinos SUSY and R Parity If nature conserves PR PR 1 3(B L) 1 2S vertices have even number of superpartners Consequences 0 ˜ Lightest SUSY particle is stable viable dark matter candidate Proton is stable Superpartners appear only in loops SUSY must be a broken symmetry Superpartners have not been seen M e˜ me M q˜ mq M ˜ MW ,Z , Can we test models of SUSY breaking mediation ? Theoretical models of SUSY breaking SUSY Breaking Visible World Hidden World Flavor-blind mediation III. Three Probes, Three Questions: • Why is there more matter than antimatter in the present universe? Electric dipole moment searches • What are the unseen forces that disappeared from view as the universe cooled? Precision electroweak: weak decays & lepton scatt • What are the masses of neutrinos and how have they shaped the evolution of the universe? Neutrino oscillations, 0nbb-decay, q13 , … Tribble report What is the origin of baryonic matter ? Cosmic Energy Budget E d dS Dark Matter Baryons B (7.3 2.5) 1011 YB s (9.2 1.1) 1011 ddS(S E) E nnEDM EDM hh BBN WMAP Dark Energy T-odd , CP-odd by CPT theorem What are the Searches for permanent quantitativeelectric implications dipoleof new moments EDM experiments (EDMs) of forthe explaining neutron,the electron, origin of andbaryonic the neutral atoms component probe of new theCP-violation Universe ? EDMs & Baryogenesis Present universe Early universe Sakharov Criteria • B violation • C & CP violation Y1 • Nonequilibrium dynamics Sakharov, 1967 1 L Weak scale baryogenesis can be tested experimentally 1 S ? ? log 10 ( / 0 ) Weak scale Planck scale EW Baryogenesis: Standard Model Weak Scale Baryogenesis Anomalous Processes • B violation • C & CP violation J B • Nonequilibrium dynamics A qL Sakharov, 1967 W W Different vacua: (B+L)= NCS Kuzmin, Rubakov, Shaposhnikov McLerran,… Sphaleron Transitions EW Baryogenesis: Standard Model Shaposhnikov Quark mixing & CPV 2 J s12 s13 s23 c12 c13 c 23 sin 13 (2.88 0.33) 105 Weak Scale Baryogenesis mt4 mb4 mc2 ms2 13 3 10 MW4 MW4 MW2 MW2 • B violation • C & CP violation • Nonequilibrium dynamics F F 1st order 2nd order Sakharov, 1967 • CP-violation too weak • EW PT too weak Increasing mh Baryogenesis: New Electroweak Physics 90’s: Weak Scale Baryogenesis • B violation Cohen, Kaplan, Nelson Joyce, Prokopec, Turok Unbroken phase Topological transitions new • C & CP violation • Nonequilibrium dynamics (x) Broken phase 1st order phase transition CP Violation Sakharov, 1967 new • Is it viable? • Can experiment constrain it? • How reliably can we compute it? new new e EDM Probes of New CP Violation CKM f dSM dexp dfuture e n 199 Hg 1040 1030 1033 1.6 1027 3.0 1026 2.11028 1031 1029 1032 1028 1.11018 1024 Also 225Ra, 129Xe, d If new EWK CP violation is responsible for abundance of matter, will these experiments see an EDM? Present n-EDM limit Proposed n-EDM limit ? Matter-Antimatter Asymmetry in the Universe Better theory M. Pendlebury B. Filippone Riotto; Carena et al.; Lee, Cirigliano, R-M, Tulin “n-EDM has killed more theories than any other single experiment” Baryogenesis: New Electroweak Physics 90’s: Weak Scale Baryogenesis • B violation Cohen, Kaplan, Nelson Joyce, Prokopec, Turok Unbroken phase Topological transitions • C & CP violation • Nonequilibrium dynamics Broken phase 1st order phase transition (x) new Violation More CP SUSY Higgs? Ando,Barger, Langacker ,Profumo, R-M, Shaugnessy, Tulin Sakharov, 1967 Theoretical Issues: new Strength of phase transition (Higgs “Gentle” departure sector) •Bubble dynamics (numerical) Is it viable? new equilibrium& from Transport at phase boundary (non-eq • Can experiment constrain it? QFT) scale hierarchy new Cirigliano, Lee, EDMs: many-body physics & QCD • How reliably can we compute it? eR-M,Tulin Electroweak Phase Transition & Higgs F F 1st order 2nd order LEP EWWG Increasing mh 1st order PT in MSSM: mh < 120 GeV mh>114.4 GeV Constraint on mh relaxed in How is electroweak symmetry SUSY models with more broken? Higgs (LHC, ILC) or ~ 90 GeV (SUSY) Quantum Transport & SUSY CPV Non-equilibrium quantum transport RHIC Violent departure from equilibrium Electroweak Baryogenesis new (x) “Gentle” departure from equilibrium & scale hierarchy Systematic treatment of transport with controlled approximations using non-equilibrium QFT Cirigliano, Lee, R-M, Tulin SUSY CPV & Quantum Transport Chargino Mass Matrix CPV MC = T ~TEWT: ~ scattering TEW ~) ~ of(xH,W from new background field m W 2 cos b M2 mW 2 sin b Neutralino Mass Matrix T << TEW : mixing ~ ~ ~0 of H,W to ~, Resonant CPV: M1,2 ~ ˜ u,d q , W˜ , B˜ , H ˜ M 0 ˜ W 0 -m cos b sin q m cos b cos q M ˜ 1 1 ˆ ˜ ˜ ˜ W H M M = d 0C H˜ M 1 2msin b0sin q M-m sinbsin˜ q N 0 um cos bcos q 2 - 2 -m cos bsin q Z 1 Z 2 Z W mZ sin bsin qW Z W W Z W Z W W -mZ sin bsin qW - 0 EDM constraints & SUSY CPV | sin | > 0.02 Baryogenesis | de , dn | > 10-28 e-cm M < 1 TeV LEP II Exclusion Two loop de Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 SUSY CPV & Dark Matter Chargino Mass Matrix T << T T ~TEW : scattering ~ ~ of H,W from EW CPV 0 N11B 0N Hbd0N14Hu0 cos M2 12W mN213 MC = BINO background field W mW 2 sin b WINO HIGGSINO Neutralino What role Mass can the Matrix precursors of the 0 neutralinos M1 M2 play in0 MN = -m mZ cos bcos qW Z cos bsin qW baryogenesis? mZ sin bsin qW T << TEW : mixing ~ ~ ~0 of H,W to ~, -mZ sin bsin qW -mZ cos bsin qW mZ cos bcos qW mZ sin bsin qW -mZ sin bsin qW 0 - - 0 SUSY Baryogenesis & Dark Matter Neutralino-driven baryogenesis Baryogenesis Charginos & neutralinos LEP II Exclusion Two loop de Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 SUSY Dark Matter: Solar Neutrinos ˜0 Z0 ˜0 n n Neutralino-driven baryogenesis SUGRA: M2 ~ 2M1 Gravitational capture in sun followed by annihilation into high energy neutrinos No signal in SuperK detector AMSB: M1 ~ 3M2 Cirigliano, Profumo, R-M SUSY Dark Matter: Future Experiments Neutralino-driven baryogenesis & nonstandard cosmology Assuming W ~WCDM Cirigliano, Profumo, R-M SUSY Baryogenesis & Colliders LHC era complementarity: • EDMs will remain most powerful probe of electroweak baryogenesis • DM searches will probe 0 driven baryogenesis & non-st’d cosmology • LHC will tellNeutralino-driven us about Higgs & baryogenesis phase transition LHC reach ILC reach Cirigliano, Profumo, R-M Precision Ewk Probes of New Symmetries Electroweak symmetry? Unseen Forces: Supersymmetry breaking: Higgs ? 1. 2. 3. 4. Unification & gravity Weak scale stability Origin of matter Neutrinos n ˜ n ne W ˜0 ˜ e QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. QuickTi me™ and a T IFF (Uncom pressed) decom pressor are needed to see this picture. QuickT ime ™an d a TIFF ( Uncomp res sed) deco mpre ssor ar e need ed to see this pictur e. QuickTime™ and a TIFF ( Uncompressed) decompr essor are needed to see this picture. Beyond the SM QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. SM symmetry (broken) Weak Decays: GF encodes information on the spectrum via radiative corrections Muon Decay n g W e n g ne Z0 n e W e ne n e W W 2 5 G 1 F m 3 192 2 GF g 1 r 2 2 8MW rdepends on parameters of particles inside loops ne Comparing radiative corrections in different processes can probe particle spectrum n n Z 0 g e g e n Z0 n n e Z0 e n e n Z e e GFZ g 2 2 1 rZ 2 8MW rdiffers from rZ Z0 0 Comparing radiative corrections in different processes can probe particle spectrum GFZ 1 rZ r GF Z 0 t Z 0 W W t t mt2 rZ ~ ln 2 MW b m t2 r ~ M W2 Comparing radiative corrections in different processes can probe particle spectrum Direct Measurements Radiative corrections Probing Fundamental • Precision measurements Symmetries beyond predicted a range for mt the SM: before top quark discovery low• mUse mb ! t >> precision energy measurements • mt is consistent with that to probe virtual effects range of new symmetries & • Itcompare didn’t have tocollider be that with way results Stunning SM Success J. Ellison, UCI Weak decays: light quarks d u e ne Vud t Vcd Vtd u s u e ne c b u e ne 2 2 Vud Vus Vub 0.9487 0.0010 2 = Vus Vub d Vcs Vcb s Vts Vtb b 1 SM 0.9968 0.0014 Expt 0.0482 0.0008 0.00001 0.000007 Weak decays: light quarks d u e ne u s u e ne b u e ne b-decay n p e ne A(Z,N) A(Z 1,N 1) e n e e ne 0 c Vud t Vcd Vtd Vus Vub d Vcs Vcb s Vts Vtb b GFb Vud 1 rb r GF SUSY loops Weak decays & SUSY d u e ne u s u e ne b u e ne n b-decay W ˜ n ˜ 0 n n p e ne ˜ GFb Vud 1 rb r GF SUSY SUSY loops ne 0 n ˜e e n e ˜ O ~ 0.001 SM O e Vus Vub d Vcs Vcb s Vts Vtb b SUSY A(Z,N) A(Z 1,N 1) e n e ˜0 ˜ n ne c Vud t Vcd Vtd e r SUSY Radiative Corrections n W Propagator n Vertex & External leg ˜ n W ˜0 W n e ˜ n ne ne e W n˜ e W ˜ 0 ˜ ˜ e e e˜ W n˜ 0 ˜ n ˜ n ˜ ne ˜0 Box ˜ ne e ne e Weak decays & SUSY R Parity Violation R-M, V Flavor-blind dSu VKurylov,VSUSY- d u e ne ud us breaking u c t Vcd V MW td s u e ne b u e ne n ne ne ub Vcs Vcb s CKM Unitarity Vts Vtb b CKM, (g-2), MW, Mt ,… APV O l2 b ~ 0.001 SM GF 12k 12k ˜ n p e ne e n O Vud 1 rb r G F nd e n 1) e n e A(Z,N) A(Z 1,N q˜ n ˜ n 0 ˜ 1j1 M˜ L Mq˜ L 1j1 e n e Kurylov, ed No long-lived LSPSUSY or SUSY loops DMR-M SUSY RPV e ˜ e b-decay e˜ ˜ n 0 SUSY k W R ˜0 e j L e ˜ CKM Summary: PDG04 Neutron lifetime e J pe basymmetry UCNA J CKM Summary: New Vus & n ? Neutron lifetime Vus & Vud theory ? UCNA New 0+ info basymmetry New n !! Correlations Weak decays & SUSY d u e ne u s u e ne b u e ne n c Vud t Vcd Vtd Vus Vub d Vcs Vcb s Vts Vtb b J n ˜ n W ˜0 n e u˜ d pe pn pnpe dW 1 a Bme E eAJn E e En EnE e ˜0 u ˜ O J p~ 0.001 SM O n e SUSY ne n ˜e ˜ e SUSY Non (V-A) x (V-A) interactions: me/E Chiral symmetry in SUSY? Weak decays & SUSY : Chiral Symmetry Chiral () Rotation Gauge interactions: symmetric Higgs interactions: break symmetry, but gently for 1st & 2nd generations Is sym breaking gentle for 1st & 2nd generation sfermions ? Weak decays & SUSY : Correlations Chiral symmetry breaking in SUSY ˜0 u ne ˜e n u˜ n J d ˜ e Future exp’t ? J pn Profumo, R-M, Tulin Mass suppressed symmetry breaking: “alignment” models Large symmetry breaking: New SUSY models Pion leptonic decay & SUSY SM strong interaction effects: parameterized by F Hard to compute SM radiative corrections also have QCD effects n ˜0 u To probe effects of new physics in NEW we need to contend with QCD n ˜ n u˜ d ˜ n Pion leptonic decay & SUSY New TRIUMF, PSI Leading QCD uncertainty: Marciano & Sirlin ˜0 u ne ˜e n u˜ d ˜ e ? Can we do better on Tulin, Su, R-M ˜ n d ˜ Prelim n u˜ vs ˜0 u n Probing Slepton Universality Min (GeV) Lepton Scattering & New Symmetries Parity-Violating electron scattering e e Z 0 e , p e , p e e e , p e , p N N GF Q2 2 APV Q F(Q ,q ) W N N 4 2 “Weak Charge” ~ 0.1 in SM Enhanced transparency to new physics Small QCD uncertainties (Marciano & Sirlin; Erler & R-M) QCD effects (s-quarks): measured (McKeown, Souder, Beck,…) Probing SUSY with PV eN Interactions e Z SUSY dark matter e 0 ˜ Z0 f SUSY loops ˜ e˜ e f e e˜ f f QWp,SUSYQuickTime™ QWp,SM and a TIFF (Uncompressed) decompressor are needed to see this picture. n is Majorana ne e ˜ Rk e Q e, SUSY W Kurylov, Su, MR-M RPV 95% CL fit to 12k decays, M ,etc. 12k weak W n e, SM W Q Probing SUSY with PV eN Interactions Kurylov, R-M, Su “DIS Parity” SUSY loops SUSY N SUSY dark darkmatter matter QWp,SUSYQuickTime™ QWp,SM and a TIFF (Uncompressed) decompressor are needed to see this picture. Linear collider E158 &QWeak JLab Moller RPV 95% CL QWe, SUSY QWe, SM Conclusions • The fundamental symmetries of the Standard Model provide a successful basis for explaining the microphysics of the present universe, but additional symmetries are needed to address important questions about earlier times Origin of matter, unification, size of the Fermi constant, neutrino mass, gravity,… • High precision, low-energy studies provide a powerful probe of new symmetries that complement the view provided by colliders EDMs, weak decays, lepton scattering, neutrino properties & interactions, lepton flavor… • This field provides a rich interplay of particle, nuclear, & atomic physics with cosmology in both theory & exp’t
