Dark Matter Expect Unexpected outside LHC Jingsheng Li

Introduction SM is confirmed precisely? NO! Dark Matter is OUT THERE!! SC=SM+more ∟(New Phy=ptc+int) +unexpected ∟astrophy effect? ∟ modify gravity?

Outline Standard Cosmology Evidence for Dark Matter Relic Density Candidates Dark Matter Detection

Standard Cosmology Smooth Universe Friedman Eqn Content ( w=  /P, ) baryon w=0 radiation w=1/3 c.d.m. w=0 c.c. w=-1

A Brief History of Universe

Properties of DM Dark (rotation curve, gra. lensing) Cold (Structure formation) Weakly Interacting (rotation curve, Bullet Cluster)  b /  m =1/6 ( BBN, CMB, Bullet Cluster 1E )

Evolution of CDM Boltzmann Eqn (1+2  3+4) Note: Eq (T>m), freeze out (T<m)

Relic Density

Lee-Weinberg Bound Anti-baryon 45GeV L Scalar DM Higgs exchange, even weaker, expect for Boehm, Fayet (N=2) Lee-Weinberg is good for >GeV range

Candidate VS Test Gra Lensing Lee-Weinberg +Z width Direct Search PAMELA /ATIC MACHOs X Anti-Baryon X SM L X MSSM X Neutralino  X? Gravitino --? Axion --? UED w/ KK-parity, LH w/ T-parity, Techni Baryon, monopole, R ….

SUSY WIMP SUSY w/ R-parity provides LSP Spctrum depends on Mediation Scheme Hidden Sector GMSB: gravitino as LSP, cosmo constraint: NLSP decay, BBN and CMB constraints Gravity Mediated, decay, BBN constraint Neutralino as LSP: In Lee-Weinberg bound

Neutralino Decay channels  univ ~10Gyr, set upper bound for  M h 2 <0.3, lower bound for , upper bound for m int. Cosmology set upper bound on superpartner, good for LHC?

Axion (non-thermal CDM) PQ SSB  Axion PQ EB  Coupling to Nucleon Red Giant emission bound SN1987A bound Oscillation energy Critical density bound Search:

Detection MET Direct Detection Indirect Detection

Direct Detection TypeScintillator Cryogenic Crystal Noble Liquid matterial NaI, CsIGe, SiAr, Xe ProNormal T Distinguish e / NNew tech, potential Con Background  Low T, $ Exp DAMACDMSXENON ResultSolar modulation

Indirect Detection Annihilation at Center of Sun Galaxy CenterHalo in to  e+ detected by AMANDA, IceCube GLAST, HESS, INTEGRAL AMS, HEAT, PAMELA, ATIC Result511KeV from bulge excess

Result from indirect detection e + excess beyond prediction 10 GeV ~ 100GeV (PAMELA), e + e - excess upto TeV (ATIC) ATIC: sharp 600GeV no astrophy explaination SUSY needs 10TeV for PAMELA No p - excess Usual Neutralino can’t explain Very large, conflicts with required relic density.

Solution? New interaction to annihilate  Sommerfeld enhancement (Arkani-Hamed) Breit-Wigner enhancement (Murayama) Nonthermal production (Kumar) DM decay