1500H>0H.Baer,mSUGRA orCMSSM:simplest(and mostJ.o'Farconstrained) modelfor supersvmmetric1000dark mattermsUR-parity conservation,radiative1600electroweak symmeuryreakmg1400Free parameters (set at GUT scale): mos1200m1/2,tan ,Ao,sign(μ)100100020002500mz(Gev)800电E4 main regions where neutralino fulfillsmh=114Gev700WMAP relic density:600.bulk region (low mo and mi/2)a)mxt=104Gev500. stau coannihilation region mx~mstan400·hyperbolic branch/focus point (mo>>mi2)300funnel region(mAH~2m)200100However,general MSSM model versions giveparameters:,AtAh(and perhaps several m12003004005008001006007009001000m1/2 (GeV)
mSUGRA or CMSSM: simplest (and most constrained) model for supersymmetric dark matter R-parity conservation, radiative electroweak symmetry breaking Free parameters (set at GUT scale): m0 , m1/2, tan A0 , sign() 4 main regions where neutralino fulfills WMAP relic density: • bulk region (low m0 and m1/2) • stau coannihilation region m mstau • hyperbolic branch/focus point (m0 >> m1/2) • funnel region (mA,H 2m ) However, general MSSM model versions give more freedom. At least 3 additional parameters: , At , Ab (and perhaps several more.) H. Baer, A. Belyaev, T. Krupovnickas, J. O’Farrill, JCAP 0408:005,2004
DetectionofWIMpColliderIndirect detectionDM increases inGalaxies-annihilationrestarts(αp2:IDlooksfortheannihilation productsof WiMPs,such astheneutrinos,gamma rays,positrons at theground/space-basedexperimentsindirectdetectionDirect detection of WiMPat terrestrialdetectors口via scattering of WIMP of the detector material.Directdetectionxx→li=xl→xl
Detection of WIMP Collider Indirect detection DM increases in Galaxies, annihilation restarts(∝ρ2); ID looks for the annihilation products of WIMPs, such as the neutrinos, gamma rays, positrons at the ground/space-based experiments Direct detection of WIMP at terrestrial detectors via scattering of WIMP of the detector material. Direct detection p e + _ indirect detection 𝜒𝜒LJ → 𝑙 LJ 𝑙 ⇔ 𝜒𝑙 → 𝜒𝑙
Fluxof the annihilationproductsdSUSYdpFluxisdeterminedby(E) ×μcosm ()dEdEtheproductsoftwofactorsThefirstfactoristhestrengthof the口interaction,determinedcompletelybyparticlephysicsdpSUSYPdN1(ov)dEBdE4元2mx2The secondby the distribution of DM口dcosmop(r)dV=dop (r)dlThe flux depends onboththe口astrophysicsandtheparticle aspects
Flux of the annihilation products Flux is determined by the products of two factors The first factor is the strength of the interaction, determined completely by particle physics The second by the distribution of DM The flux depends on both the astrophysics and the particle aspects. 𝑑𝛷 dE = 𝑑𝛷SUSY dE (𝐸) × 𝛷 cosmo(𝜓) 𝑑𝛷SUSY dE = 1 4𝜋 𝜎𝑣 2𝑚𝜒2 dN𝑓 dE 𝐵𝑓 𝛷 cosmo = 1 𝑑 2 න 𝜌 2 (𝑟) dV = න 𝑑𝛺 න 𝜌 2 (𝑟)dl
GC andSubhalosforindirectΦα(ov)p2detectionThefluxesof the annihilationproductsare proportional to口the annihilation cross section and the DM density square.Fluxesaregreatly enhanced byclumpsof DM.The Galacticcenter and center of subhaloshave high口density.Thereare5%~1o%DMofthetotalhalomass are enclosed in the clumps Thefollowingcharacters makesubhalosmoresuitableforDMdetection·GCisheavily contaminated bybaryonicprocesses.·Structures in CDM from hierarchicallyi.e.the smallerobjectsformearlierandhavehighdensity.·Subhalos may be more cuspy profilethanthe GC..Massismore centrally concentratedwhenan objectisinan environment withhigh density
GC and Subhalos for indirect detection The fluxes of the annihilation products are proportional to the annihilation cross section and the DM density square. Fluxes are greatly enhanced by clumps of DM. The Galactic center and center of subhalos have high density. 𝛷 ∝ 𝜎𝑣 𝜌 2 There are 5%~10% DM of the total halo mass are enclosed in the clumps. The following characters make subhalos more suitable for DM detection: •GC is heavily contaminated by baryonic processes. •Structures in CDM from hierarchically, i.e., the smaller objects form earlier and have high density. • Subhalos may be more cuspy profile than the GC. • Mass is more centrally concentrated when an object is in an environment with high density
11112h0)MProem口6a福or一s01eVSLL
Problems at small scale of CDM Galactic satellite problem and cusp at GC Nature of dark matter or astrophysics process?