Galactic Center Signals : Galactic Center Signals : Compressed Dark Matter Halos and Compressed Dark Matter Halos and

SUSY modelsSUSY models

Yann Mambrini, DESY Hamburg – LPT Orsay,in collaboration with

C. Muñoz and E. Nezri

The Dark Side of The Universe Worshop, Seoul, May 25th 2005

Based on :Based on :hep-ph/0407158 (Astrp. J. Phys.)hep-ph/0407158 (Astrp. J. Phys.)

hep-ph/0407352 (JCAP)hep-ph/0407352 (JCAP)hep-ph/0506???hep-ph/0506???

OutlineOutline

III)III) The center galactic detectionThe center galactic detectionPrinciplePrinciple

The experimentsThe experiments

IV)IV) The Galaxy profilesThe Galaxy profilesClassical examplesClassical examples

A more realistic scenario : adiabatic compressed profilesA more realistic scenario : adiabatic compressed profiles

I)I) IIntroductionntroduction

II)II) SupersymmetrySupersymmetrySupergravity landscapeSupergravity landscape

mSUGRAmSUGRAA more realistic scenario : general SUGRAA more realistic scenario : general SUGRA

VI) VI) Conclusion and OutlooksConclusion and Outlooks

IntroductionIntroduction

MODELSMODELS

MSUGRAMSUGRA

General SUGRAGeneral SUGRA

Heterotic StringsHeterotic Strings

Brane WorldBrane World

NMSSMNMSSM

......

DATADATA

EGRETEGRET

CANGAROOCANGAROO

VERITASVERITAS

HESSHESS

HEATHEAT

......

Effective Models LandscapeEffective Models Landscape

SUGRASUGRA

M1M2M3mH1mH2mQmUmDmLmEAuAdAtμB

MSUGRAMSUGRA

M0M1/2ATanSignμ

EffectiveEffective StringString

M3/2<Ft><Fs>

tan GS

cos<V>=0

Heterotic Heterotic stringstring

M3/2

Tanb+<t>

GS<V>=0 BranesBranes

Supergravity LandscapeSupergravity LandscapeM1M2M3mH1mH2mQmUmDmLmEAuAdAtμB

SUGRASUGRA

M0M1/2ATanSignμ

. mSUGRAmSUGRA

M3 = (1+ d'3) M1/2M3 = (1+ d'3) M1/2..

d'3d'3

..

d'3 > 0d'3 > 0..

d'3 < 0d'3 < 0

MH

1 =

(1+

d1)

M0

MH

1 =

(1+

d1)

M0

..

d1d1 ..

d1>0d1>0

..

d1<0d1<0

Effective Models Landscape bisEffective Models Landscape bisTan Tan M1M1M2M2M3M3....mH1mH1mH2mH2....AbAbAtAt

GeneralGeneralSUGRASUGRA..

Tan Tan

M1/2M1/2

M0M0

AA

Sgn( Sgn( ))

mSUGRAmSUGRA

Tan Tan M1/2(1 + d'1)M1/2(1 + d'1)M1/2(1 + d'2)M1/2(1 + d'2)M1/2(1 + d'3)M1/2(1 + d'3)....M0(1 + d1)M0(1 + d1)M0(1 + d2)M0(1 + d2)....

ParametrizedParametrizedSUGRASUGRA

Tan Tan M3/2 (b1 + dGS)M3/2 (b1 + dGS)M3/2 (b2 + dGS)M3/2 (b2 + dGS)M3/2 (b3 + dGS)M3/2 (b3 + dGS)....M3/2 (1 + n1)M3/2 (1 + n1)M3/2 (1 + n2)M3/2 (1 + n2)....

String MotivatedString Motivated

Indirect detection from GCIndirect detection from GC

GLAST (2007)GLAST (2007)

HESS (Namibie, 2004)HESS (Namibie, 2004)

d 1 dN1 dN < < v > v > d d d E d E 2 dE2 dE44 M M

∫∫ dldl22

22==

. (r) =(r) = 00

(r/R0) [1 + (r/a) ](r/R0) [1 + (r/a) ] (-)/(-)/(cm , s ) (cm , s ) ~ 10~ 10 1010

-13-2 -1 < < v v > (100 GeV) > (100 GeV)

10 cm s M10 cm s M22

22

-29-29 33 -1-1 J J ∆∆

h h ~ ~ 0.1 ~ ~ 0.1 →~→~1010 J J 3.10 cm s 3.10 cm s

< < v > v >

-1-1 33 -11-11 22 -27-27

The adiabatic compressionThe adiabatic compression

MMii ( r ( ri i ) r) rii = [ M = [ MCDMCDM ( r ( rff ) + M ) + Mbb (r (rf f )] r)] rff

N-Body simulationN-Body simulation(NFW, Moore..)(NFW, Moore..)

Today baryon Today baryon distributiondistribution??????

Baryon fall in the Galactic CenterBaryon fall in the Galactic Center

Redistribution of mass Redistribution of mass in the gravitational potentialin the gravitational potential

BaryonsBaryons

NeutralinosNeutralinos

(r) ~ 1/r (r) ~ 1/r (NFW)(NFW)

(r) ~ 1/r (r) ~ 1/r (NFW (NFW compressed)compressed)

1.51.5

Baryon falls in the central region Baryon falls in the central region to form galaxyto form galaxy

ReReReReRedistribution of masses Redistribution of masses

in the gravitational potentialin the gravitational potential

( r )( r )arb. unitsarb. units

200200

100100

LogLog1010 ( r( r )) 00 11-1-1-2-2-3-3

NFWNFW

NFW NFW compressedcompressed

The relic density constraintsThe relic density constraints

Neutralino Neutralino ≡≡ HiggsinoHiggsino

LightLight

High fluxesHigh fluxes

Neutralino Neutralino ≡≡ BinoBino

M1= M / 2M1= M / 2

High fluxesHigh fluxes

Neutralino Neutralino ≡≡ BinoBino

M1 = M / 2M1 = M / 2

Low fluxesLow fluxes

M0M0

M1/2M1/2

TOOLSTOOLS

SUSPECT2

SDECAY

BrBr

Micromegas1.3

b -> sb -> s

g-2g-2

Bs -> Bs -> µ+ µ-µ+ µ-

DarkSusy4

DirecteDirecteIndirecteIndirecte

E+e-

Suspect2* (Strings, RGE, CCB)

Low Energy SpectrumLow Energy SpectrumCouplingsCouplings

(A. Djouadi, Y.M, M. Mulheitner, 03)(A. Djouadi, Y.M, M. Mulheitner, 03)

Exp. Part IExp. Part IEGRETEGRET

(Y.M, C. Munoz, 05)(Y.M, C. Munoz, 05)

MSUGRAMSUGRAWMAPWMAP

Acc. Const.Acc. Const.

MH1MH1MAPMAP

Acc. Const.Acc. Const.

M3 = M/2M3 = M/2WMAPWMAP

Acc. Const.Acc. Const.

Exp. Part IIExp. Part IIA.C.T. : CANGAROO II, HESSA.C.T. : CANGAROO II, HESS

(Y.M, C. Munoz, 05)(Y.M, C. Munoz, 05)

Exp. Part IIIExp. Part IIISatellite GLASTSatellite GLAST

(Y.M, C. Munoz, E. Nezri 05)(Y.M, C. Munoz, E. Nezri 05)

MSUGRAMSUGRAMAPMAP

Acc. Const.Acc. Const.

MH1 MH1 MAPMAP

Acc. Const.Acc. Const.

M3 = M/2M3 = M/2MAPMAP

Acc. Const.Acc. Const.

AA BB CC DD

Exp. Part IVExp. Part IVCombining EGRET, CANGAROO Combining EGRET, CANGAROO

and GLAST?and GLAST?

(Y.M, C. Munoz, E. Nezri 05)(Y.M, C. Munoz, E. Nezri 05)

SummarySummaryM1M2M3mH1mH2mQmUmDmLmEAuAdAtμB

SUGRASUGRA

M0M1/2ATanSignμ

. mSUGRAmSUGRA

M3 = (1+ d'3) M1/2M3 = (1+ d'3) M1/2..

d'3d'3

MH

1 =

(1+

d1)

M0

MH

1 =

(1+

d1)

M0

..

d1d1

EGRETEGRET

CANGAROOCANGAROO

EGRET EGRET ++ CANGAROOCANGAROO

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

ConclusionConclusion

Futur experiment (GLAST) will be able to reach allFutur experiment (GLAST) will be able to reach allthe parameter space of SUGRAthe parameter space of SUGRA

Compressed profiles can fit experimental data excessesCompressed profiles can fit experimental data excesses

Direct application to string motivated modelsDirect application to string motivated models

Restriction of the parameter spaceRestriction of the parameter space using collider/astro complementarityusing collider/astro complementarity