Galactic Center Signals : Compressed Dark Matter Halos and SUSY models Yann Mambrini, DESY Hamburg – LPT Orsay, in collaboration with C. Muñoz and E. Nezri The Dark Side of The Universe Worshop, Seoul, May 25 th 2005 Based on : Based on : hep-ph/ (Astrp. J. Phys.) hep-ph/ (JCAP) hep-ph/0506???

Outline III)The center galactic detection Principle The experiments IV)The Galaxy profiles Classical examples A more realistic scenario : adiabatic compressed profiles I)Introduction II)Supersymmetry Supergravity landscape mSUGRA A more realistic scenario : general SUGRA VI) Conclusion and Outlooks

Introduction MODELS MSUGRA General SUGRA Heterotic Strings Brane World NMSSM... DATA EGRET CANGAROO VERITAS HESS HEAT...

Effective Models Landscape SUGRA SUGRA M1 M2 M3 mH1 mH2 mQ mU mD mL mE Au Ad A  μ B MSUGRA M0 M1/2 A Tanb Signμ Effective String String M3/2 tan b d GS cos q =0Heteroticstring M3/2 Tan b b+ d GS =0 Branes

Supergravity Landscape M1 M2 M3 mH1 mH2 mQ mU mD mL mE Au Ad A  μ B SUGRA SUGRA M0 M1/2 A Tanb Signμ mSUGRA. mSUGRA M3 = (1+ d'3) M1/2.d'3. d'3 > 0. d'3 < 0 MH1 = (1+ d1) M0.d1.d1>0.d1<0

Effective Models Landscape bis Tan M1M2M3..mH1mH2..AbAtGeneralSUGRA. Tan M1/2M0A Sgn( ) mSUGRA Tan M1/2(1 + d'1) M1/2(1 + d'2) M1/2(1 + d'3).. M0(1 + d1) M0(1 + d2).. Parametrize d SUGRA Tan M3/2 (b1 + dGS) M3/2 (b2 + dGS) M3/2 (b3 + dGS).. M3/2 (1 + n1) M3/2 (1 + n2).. String Motivated

Indirect detection from GC Indirect detection from GC c c g g GLAST (2007) HESS (Namibie, 2004) 1 dN d 1 dN d d E 2 dE 4 M ∫ dl ∫ dl22 = (r) =. (r) = 0 (r/R0) [1 + (r/a) ] (-)/ (cm, s ) ~ 1010 (cm, s ) ~ (100 GeV) (100 GeV) 10 cm s M J ∆ h ~ ~ 0.1 → ~ 10 J h ~ ~ 0.1 → ~ 10 J 3.10 cm s

The adiabatic compression M i ( r i ) r i = [ M CDM ( r f ) + M b (r f )] r f N-Body simulation (NFW, Moore..) Today baryon distribution ??? Baryon fall in the Galactic Center Redistribution of mass in the gravitational potential Baryons Neutralino s (r) ~ 1/r (NFW) (NFW) (r) ~ 1/r (NFW compressed ) (NFW compressed ) 1.5 Baryon falls in the central region to form galaxy ReReRedistribution of masses in the gravitational potential ( r ) ( r ) arb. units Log 10 ( r ) NFW NFWcompressed

The relic density constraints Neutralino ≡ Higgsino Light High fluxes Neutralino ≡ Bino M1= M / 2 High fluxes Neutralino ≡ Bino M1 = M / 2 Low fluxes M0 M1/2

TOOLS SUSPECT2 SDECAY Br Micromegas1.3 W b -> s g b -> s g g-2 Bs -> µ+ µ- DarkSusy4 Directe Indirecte E+e- s Suspect2* (Strings, RGE, CCB) Low Energy Spectrum Couplings (A. Djouadi, Y.M, M. Mulheitner, 03)

Exp. Part I EGRET (Y.M, C. Munoz, 05) MSUGRAWMAP Acc. Const. MH1MAP M3 = M/2 WMAP Acc. Const.

Exp. Part II A.C.T. : CANGAROO II, HESS (Y.M, C. Munoz, 05)

Exp. Part III Satellite GLAST (Y.M, C. Munoz, E. Nezri 05) MSUGRAMAP Acc. Const. MH1MAP M3 = M/2 MAP Acc. Const. A B C D

Exp. Part IV Combining EGRET, CANGAROO and GLAST? (Y.M, C. Munoz, E. Nezri 05)

Summary M1 M2 M3 mH1 mH2 mQ mU mD mL mE Au Ad A  μ B SUGRA SUGRA M0 M1/2 A Tanb Signμ mSUGRA. mSUGRA M3 = (1+ d'3) M1/2.d'3 MH1 = (1+ d1) M0.d1 EGRET CANGAROO EGRET EGRET + CANGAROO CANGAROO

Accelerator vs Astroparticle (Y.M, C. Munoz, 05)

Conclusion Futur experiment (GLAST) will be able to reach all the parameter space of SUGRA Compressed profiles can fit experimental data excesses Direct application to string motivated models Restriction of the parameter space using collider/astro complementarity using collider/astro complementarity