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Symmetries of the Early Universe and the Origin of Matter: 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 • Can new symmetries at the weak scale account for the origin of matter and how can we find out? A combination of precise low-energy measurements, high energy collider experiments, dark matter searches, and theoretical advances will help us determine if new symmetries at the electroweak scale can account for the abundance of matter Outline I. Motivation: Why New Symmetries ? Why Low Energy Probes ? II. Brief Interlude: Supersymmetry III. Symmetries and the Origin of Matter • General Considerations • Theoretical challenges and developments • Phenomenology in the LHC era and beyond 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? Grav baryogen ? • 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 Probes of New Symmetries Electroweak symmetry New Symmetries breaking: Higgs ? 1. 2. 3. 4. Origin of Matter Unification & gravity Weak scale stability Neutrinos ˜ e 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) Comparing loop effects 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 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 , How is SUSY broken? Theoretical models of SUSY breaking SUSY Breaking Visible World Hidden World Flavor-blind mediation III. Symmetries & the Origin of Matter • Baryogenesis: General Considerations • Theoretical challenges and developments • Phenomenology in the LHC era and beyond What is the origin of baryonic matter ? Cosmic Energy Budget E B Dark Matter Baryons B (7.3 2.5) 1011 YB s (9.2 1.1) 1011 d dS dddS(S S (E E)E E ) EDM EDM EDM EDM hhh 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 ? Ingredients for Baryogenesis Sakharov Criteria Anomalous B-violating processes • B violation • C & CP violation • Nonequilibrium dynamics Sakharov, 1967 Prevent washout by inverse processes Ingredients for 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 More Higgs? CP Violation Ando,Barger, Langacker, O.Connell,Profumo, R-M, Shaugnessy, Tulin, Wise new Sakharov, 1967 Theoretical Issues: Strength of phase transition (Higgs new sector) •Bubble dynamics (expansion rate) Is it viable? Transport at phase boundary (non-eq • Can experiment constrain it? QFT) EDMs: many-body physics & QCD • How reliably can we compute it? e new Electroweak Phase Transition & Higgs F F 1st order 2nd order Need Increasing mh Stop loops in VEff LEP EWWG t˜ EMSSM ~ 10 ESM ! mH< 120 GeV So that Gsphaleron is not too fast mh>114.4 GeV ComputedorESM ! mGeV ~ 90 H < 40 GeV (SUSY) S Electroweak Phase Transition & Higgs e e Z0 F sin2q Z0 F 1st order 2nd order LEP EWWG Need Increasing mH Singlet Higgs (SUSY or non-SUSY) S S S Decay So that Gsphaleron is not too fast mh>114.4 GeV Mixing ComputedorESM ! mGeV ~ 90 H < 40 GeV (SUSY) Reduced SM Higgs branching ratios Electroweak Phase Transition & Higgs B.R. reduction F F 1st order 2nd order LEP EWWG mH Unusual final states S b S Increasing m H Need b O’Connell, R-M, Wise Singlet Higgs (SUSY or non-SUSY) S S S Decay So that Gsphaleron is not too fast mh>114.4 GeV Mixing How is electroweak symmetry broken? (LHC, ILC) ComputedorESM ! mGeV ~ 90 H < 40 GeV (SUSY) 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 (x) new Broken phase 1st order phase transition CP Violation Sakharov, 1967 Theoretical Issues: new Strength of phase transition (Higgs “Gentle” departure from equilibrium& sector) •Bubble dynamics (expansion rate) Is it viable? new scale hierarchy Transport at phase boundary (non-eq QFT) • Can experiment constrain it? Lee, Cirigliano, new R-M,Tulin EDMs: many-body physics & QCD • How reliably can we compute it? e Quantum Transport & Baryogenesis 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 Bubble Wall Dynamics VFree (2V (1 pressure energy Dine et al,Reflection St’d Model pressure p > pminParticles : transmitted vwParticles with M(2 increasing mH with M(1 p < pmin : reflected SUSY or other models ? mt Higgs pressure Boost pressure Fewer particles with p > pmin in wall rest frame; more reflection Quantum Transport & Baryogenesis Electroweak Baryogenesis new (x) 1. Evolution is non-adiabatic: vwall > 0 !decoherence 2. Spectrum is degenerate: T > 0 ! Quasiparticles mix Density is non-zero 3. ParticlePropagation: Beyond familiar (Peskin) QFT 0 LI IN Assumptions: 1. 2. 3. Evolution is adiabatic Spectrum is non-degenerate Density is zero 0 OUT Quantum Transport & Baryogenesis Electroweak Baryogenesis new (x) 1. Competing Evolution Dynamics is non-adiabatic: vwall > 0 !decoherence CPV 2. Spectrum is degenerate: T > 0 ! Quasiparticles mix Det bal 3. Density is non-zero Cirigliano, Lee,Tulin, R-M Scale Hierarchy: Fast, but not too fast Systematically derive transport eq’s from Lnew ed = vw (k / w<< 1 Hot, but not too hot ep = Gp / w<< 1 Dense, but not too dense e = / T << 1 Work to lowest, nontrivial order in e’s Error is O (e) ~ 0.1 Cirigliano, Lee, R-M 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 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 Sakharov, 1967 (x) new Broken phase 1st order phase transition CP Violation Elementary particle EDMs: N!1 Theoretical Issues: new Strength of phase transition (Higgs Many-body EDMs: Engel,Flambaum, sector) •Bubble dynamics (expansion rate) Is it viable? new Haxton, Henley, Transport at phase boundary (non-eq • Can experiment constrain it? QFT) new R-M Khriplovich,Liu, EDMs: many-body physics & QCD • How reliably can we compute it? e EDMs in SUSY One-loop f˜ ˜0 q˜ f˜ f q, l, n… EDM: ˜0 g q˜ q Chromo-EDM: q, n… Dominant in & atoms nuclei EDMs & Baryogenesis f˜ q˜ ˜ 0 g q˜ ˜ 0 new f˜ q (x) f ˜,B ˜,H ˜ u,d q,W Future de dn dA Cirigliano, Lee, Tulin, R-M Resonant Non-resonant T ~ TEW EDMs in SUSY Decouple in large One-loop f˜ ˜0 q˜ ˜0 f˜ f q, l, n… EDM: limit q˜ q Chromo-EDM: q, n… Dominant in & atoms nuclei Two-loop g EDM only: no chromo-EDM g g g Weinberg: small matrix el’s EDMs & Baryogenesis | sin | > 0.02 Baryogenesis | de , dn | > 10-28 e-cm M < 1 TeV LEP II Exclusion Future de, dn Two loop de Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 SUSY Baryogenesis & Colliders LHC reach ILC reach Present de Prospective de 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 Dark Matter: Relic Abundance ˜ 10 t˜ suppressed ˜ 10 Neutralino-driven baryogenesis t t ~10 LEP II Exclusion W,Z ~i0 , ~ j ~ 0 1 too fast Non-thermal 0 W,Z SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 SUSY Dark Matter: Solar Neutrinos ˜0 Z0 ˜0 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 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 tell us about Higgs & phase transition Cirigliano, Profumo, R-M 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 unification, size of the Fermi Origin of matter, constant, neutrino mass, gravity,… • New symmetries at the weak scale may be able to account for the origin of matter A combination of precise low-energy experiments (EDM searches), collider studies, dark matter searches and theoretical advances will help us find out • This field provides a rich interplay of particle, nuclear, & atomic physics with cosmology in both theory & exp’t Conclusions We’re making progress… …and open to new ideas.
