Probing Supersymmetric Baryogenesis: from Electric Dipole Moments to Neutrino Telescopes

Stefano Profumo California Institute of Technology TAPIR Theoretical AstroPhysics Including Relativity Kellogg Rad Lab Probing Supersymmetric Baryogenesis: from Electric Dipole Moments to Neutrino Telescopes Based on: V.Cirigliano, SP and M.Ramsey-Musolf Musolf, JHEP07(006)00 SP and M.Ramsey-Musolf (Caltech/Madison) [work in progress] S.Ando (Caltech), V.Barger (Madison), SP, M.Ramsey-Musolf, G.Shaughnessy (Madison) [work in progress] INT, University of Washington Seattle, WA, Thursday, March, 007

Phenomenology of SUSY EW Baryogenesis Systematic Treatment of Baryon Asymmetry Computation in Electroweak Baryogenesis (*) Consider a specfic, viable Supersymmetric setup Study the Phenomenology Outline the MSSM Parameter Space compatible with EW Baryogenesis Explore the resulting EDM s ( and loop) Connection with Dark Matter (relic abundance and detection) Prospects for Collider searches (Tevatron-II, LHC and ILC) (*) Cirigliano, Lee, Ramsey-Musolf, Tulin; see C.Lee s and M.J.Ramsey-Musolf s talks

The Nightmare of Popper s s Quote In so far as a scientific statement speaks about reality, it must be falsifiable: And in so far as it is not falsifiable it does not speak about reality Karl Popper, The Logic of Scientific Discovery Supersymmetric Electro-Weak Baryogenesis: a falsifiable theory

Supersymmetric EW Baryogenesis Additional bosonic degrees of freedom couple to the Higgs (e.g. a light scalar top, x6) In the Minimal Supersymmetric Extension of the Standard Model (MSSM) A strongly first order EW Phase Transition occurs for larger, LEP-viable values of m h The theory features potential additional CP-violating sources - Gaugino/Higgsino sector - Scalar quark sector BONUS: the MSSM provides ideal candidates for non-baryonic Dark Matter as well! (*) see C.Lee s and M.J.Ramsey-Musolf s talks

EWB in the MSSM: Requirements In the MSSM, successful EW baryogenesis requires: at odds with:. Light enough stop m < ~ t m t m~ t > (LEP-II) 95GeV. Light enough Higgs m h <0GeV m h >4GeV (LEP-II) 3. Strong enough CP-violating sources (3rd generation squarks, higgsinos) e, n and atomic EDM s

Interludium: Neutralinos and Charginos M N = M 0 Gaugino Mass Relations 0 -m Z cos(mβ sin = αθ W M ) m Z cos β cos θ W M m Z sin β sin θ W -m Z sin β sin θ W -m Z cos β sin θ W m Z cos β cos θ W 0 -μ m Z sin β sin θ W -m Z sin β sin θ W -μ 0 χ= Ν B 0 + Ν W 0 + Ν 3 H d 0 + Ν 4 H u 0 μ μ e i φ μ T ~T EW : scattering ~ ~ of H,W from background field T << T EW : mixing ~ ~ of H,W to ~ χ +, ~ χ 0 BINO WINO HIGGSINO M C = M m W μ cos β g v d (x) m sin β W g v u (x)

EWB in the MSSM: Setup Free parameters in the game: M,, M μ, φμ

EWB in the MSSM: Setup Free parameters in the game: M,, M μ, φμ The second stop must be heavy, and mostly left-handed Increase the Higgs mass m~ m, m~ = 0 TeV t t t Reduce the SUSY contribution to Δρ

EWB in the MSSM: Setup Free parameters in the game: M,, M μ, φμ The second stop must be heavy, and mostly left-handed Increase the Higgs mass m~ m, m~ = 0 TeV t t t Reduce the SUSY contribution to Δρ Other sfermions must be heavy to suppress CP-violating processes (e.g. -loop EDM s) ~ 0 TeV m f

EWB in the MSSM: Setup Free parameters in the game: M,, M μ, φμ The second stop must be heavy, and mostly left-handed Increase the Higgs mass m~ m, m~ = 0 TeV t t t Reduce the SUSY contribution to Δρ Other sfermions must be heavy to suppress CP-violating processes (e.g. -loop EDM s) ~ 0 TeV m f The generated BAU also depends on the heavy MSSM Higgs sector through Δβ m A =50 GeV, 000 GeV

Resonant EW Baryogenesis even if all these conditions hold, CP-violating sources are large enough if close-to-resonant conditions are met in the gaugino-higgsino sector M, μ v (x) v(y) x ~ μ ~ W, B ~ x ~ H ( ) M, M ) H ( Resonant Chargino Source: Well known fact (*) Resonant Neutralino Source: Novelty! (**) Connection with Dark Matter!! (*) M.Carena et al., (003); Lee et al., (005) (**) V.Cirigliano, S.Profumo, M.Ramsey-Musolf (006)

EW Baryogenesis and DM In the (R-parity conserving) MSSM the LSP is stable The LSP must be a phenomenologically viable relic (electrically and color neutral, low enough relic abundance and direct detection rates) μ M M Mass μ M M (a): EWB and DM are unrelated (b): EWB-DM connection

Baryon Asymmetry in the MSSM What we learn:. sub-tev mass parameters Central WMAP BAU. sinφ μ >0.0 Neutralino Neutralino driven driven baryogenesis baryogenesis 3. Two-funnel structure Central WMAP BAU Neutralino Neutralino driven driven baryogenesis baryogenesis Supergravity -like gaugino mass pattern 5 sin ϑw M = M 3 sin ϑ W / Anomaly mediation -like gaugino mass pattern M g M 3 g g = β β M g

Electric Dipole Moments CP-violating interactions in the SUSY sector induce EDMs In the present setup, the best probe is the electron EDM -loop (electron) EDM Asymptotically vanish in the limit of large sfermion masses -loop EDM Only contribution In, e.g., SplitSUSY

EDMs and EW Baryogenesis sinφ μ Only two-loop EDMs (heavy sfermions limit) Anomaly mediated case even worse! Maximal phases are not compatible with EW Baryogen. exp, cur d e.6 0 7 e cm

EDMs and EW Baryogenesis sin φ μ < What we learn:. EDM and EWB are compatible. maximal phases are excluded by current data 3. there is a lower bound on the el. EDM 8 d e 0 e cm >> d e exp, fut 0 9 30 e cm EDM experiments will conclusively test the EW Baryogenesis scenario!

EWB and DM: a closer look M, The higgsino mixing is required to have a low enough relic abundance in the N χ M h μ case and fulfill EWB + right thermal χ production Large higgsino mixing implies large couplings to the Higgses, and hence large direct detection rates even with heavy s-quarks μ B ~ B ~ H ~ Since ~ the DM particle is light this means that m ~χ < m t < m t the local DM number density is large the number of pair annihilations is large ( ρ = m n ) DM DM ( n ) DM DM

The Neutralino Relic Abundance & EWB m A = TeV, sin(φ μ )=0.5 Resonant s(h) ann. Stop coann. Excessive relic abundance regions are ruled out (caveat: low-t reheating) Bino-Higgsino mixing m ~χ < m~ t < m t Low relic abundance regions are viable assuming either non-thermal production or cosmological enhancement η Ω ( WMAP th ) th Ω Ω Ω CDM χ / χ In the anomaly mediated SUSY bckg. case 30 η Ω 300 Neutralinos can be responsible for both Baryogenesis and Dark Matter

Direct & Indirect Dark Matter Searches DIRECT DETECTION Observation of scattering events of WIMPs off nuclei in low background environments HIGH ENERGY NEUTRINOS FROM THE SUN / EARTH Search for energetic neutrinos produced in χχ pair annihilations in the core of nearby gravitational dips, as the center of the Sun or of the Earth XENON -t Super-K IceCube

Dark Matter searches and EWB All the CP parameter conserving space case will (no be EWB) within reach of next CP generation violating case direct (EWB) detectors and of km size neutrino telescopes (e..g IceCube) A sizable portion of the parameter space which we expect to be compatible with EWB is already ruled out by SuperK data on the neutrino flux from the Sun CP phases suppress direct detection and enhance the neutrino flux f/sun

Dark Matter searches and EWB: Zooming Out Supergravity mediated SUSY breaking Anomaly mediated SUSY breaking Both ton-sized direct detectors AND neutrino telescopes will conclusively probe EW Baryogenesis!

Collider Searches m~ t < Tevatron (*) m~ χ + ~ t cχ~ 0 LHC same sign top (**) LHC trilepton (***) e e + + e e ILC (****) ILC ~ ~ χ + χ * ~ t ~ t (*) Demina et al, PRD (000); (**) Kraml&Raklev, 005; (***) Profumo et al, 006; (****) Carena et al, 005

EW Baryogenesis in the MSSM: Summary Two-funnel structure (chargino & neutralino driven) Will be probed by next generation electron EDM exp MSSM EW Baryogenesis Could be seen at LHC Will be probed at ILC What lies BEYOND? Compatible (and/or( and/or connected) with Neutralino CDM Already constrained by SuperK Will be probed at - IceCube -Ton-Sized Dir.Det.

Beyond the Minimal SUSY SM Adding a Gauge Singlet Superfield S to the Superpotential strongly affects SUSY EWB, adding tree-level cubic terms ( *) 3 W = μh d Hu + hs H d HuS + ks + αs + u u d d u + 3 ( c c c g Qu H + g Qd H g g Le H ) (as general as possible, including the μ-term, linear and cubic terms in S) (**) The corresponding tree level scalar field potential reads: e d (*) M.Pietroni, Nucl.Phys. B40 (993) 7; (**) Davies et al., Phys.Lett. B37 (996) 88

Beyond the Minimal SUSY SM. The EWPT is more naturally strongly first order (e.g. if the singlet Higgs is light). The bound on the Higgs mass is alleviated (both for EWB and theoretically) 3. No need for light stops 4. Extra possible non-trivial CP-structure Scopes of the projects: Study the dynamics of the EWPT (bubble walls, diffusion, wash-out ) Assess the new contribution to EW precision observables Study the CP-structure Evaluate the new contributions to Electric Dipole Moments DM physics (light singlino ) (*) (*) F.Ferrer, L.Krauss and S.Profumo, PRD 74 (006) 5007

A Toy Model Toy Model Warm-up: Minimal Singlet Extension Singlet Extension of the SM Higgs Sector (*) (*) D O Connell, M.Ramsey-Musolf, M.Wise, hep-ph/0604; S.Profumo and M.Ramsey-Musolf ( ) ( ) ( ) 4 / 3 / / / / 4 ), ( 4 4 3 3 S b S b S b H H S a H H S a H H H H m S H V + + + + + + = + + + + λ The EW Phase Transition in Singlet Models The EW Phase Transition in Singlet Models

The EW Phase Transition in Singlet Models A Toy Model Warm-up: Minimal Singlet Extension of the SM Higgs Sector (*) V ( H, S) m = a S b S + λ + H H + ( H H ) + 4 + + ( H H )/ + a S ( H H ) / + b S 3 3 / 3+ b 4 S 4 / 4 / + Singlet v.e.v. before the EW Phase Transition b b R = b 4 3 ( T c ) Singlet 0 < Singlet R T > T T c = 0 R > T c / 9 / 9 Obtain Strongly First Order EWPT without tree-level cubic terms (a =b 3 =0) Connect the order parameter φ c / T c to low-energy, collider observables (*) D O Connell, M.Ramsey-Musolf, M.Wise, hep-ph/0604; S.Profumo and M.Ramsey-Musolf

Cosmological probes: Gravitational Waves When two or more bubbles collide, spherical symmetry is broken; A fraction of their kinetic energy is released in Gravitational Waves Turbolent motions provide another source of GW s The dynamics of the EWPT enter through α = ΔV 4 T * Latent Heat (False vacuum energy) over Transition T f coll = h 0. 0 Ω GW ( f coll ) H* β β = Γ & / Γ β >> H * T =T Bubble Nucleation Time Scale β T* mhz H* 00 GeV 00 3 g* 5 α + α g* 00 * /3 (*) Kamionkowski, Kosowski, Turner (994); Nicolis (003) Gravity Wave spectrum [h 0 ΩGW ] f [mhz]

Cosmological probes: Heavy Relic Abundances Super-Cooling dilutes the abundance of Heavy Relics If T f.o. m 0 χ T c the EWPT affects the χ relic density

Cosmological probes: Heavy Relic Abundances Super-Cooling dilutes the abundance of Heavy Relics If T f.o. m 0 χ T c the EWPT affects the χ relic density T c With a strongly first order EWPT, the Universe is trapped in false vacuum φ c =0 until quantum tunneling becomes efficient (T * ) The vacuum energy is then released, re-heating the Universe to T c T * s s f i T T c * 3 ( n χ ( n χ ) ) f i T T * c 3 Superheavy Relic Density Dilution