galactic center signals : compressed dark matter halos and susy models yann mambrini, desy hamburg...
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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
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