Bad Honnef,

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1 Astro-Particle Dark Matter Search Physics with AMS 02 Chan Hoon Chan Chung Hoon Chung RWTH-Aachen, Germany Bad Honnef, on behalf of AMS Collaboration

2 Outline AMS Experiment Overview of Detector Science with AMS Precision Measurements of Charge CRs High Energy γ-rays Search for Cosmic Anti-Matter (He, C) Search for Dark Matter (e +, p -, γ,...) Summary & Launch Schedule

3 High Energy Particle Physics Experiment High Statistics, Long Duration Measurements Charged Particles & Nuclei Spectra High Energy Gamma Rays ISS : m, 420 t, 400km, Inclination = o, revolutions/day,

4 Evidence for Dark Matter WMAP, ApJ 148, 2003 Ω i ρ i / ρ c ρ c = 3H 2 / 8πG N, H = 100 h [km/s/mpc] h = 0.72 ± 0.08 from HST(2001) Ω 0 = Ω Λ + Ω Μ + Ω γ Ω 0 = 1.02 ± 0.02 Ω Λ = 0.73 ± 0.04 Ω Μ = 0.27 ± 0.04 Ω b = ± Ω γ = NGC 1560, 1992 Ω CDM h VIRGOHI21, 2005 CMB + Large-Scale Structure SN Ia + BBN + Weak lensing,... CMB + 2dF Cold Dark Matter Nature of the Cold Dark Matter? Cosmological Concordance Model

5 Nature of Dark Matter is the most challeging topic in Physics WIMP-like Candidates : SUSY Neutralino (LSP), Kaluza Klein(KK), Axion, Axino, Gravitino, WIMPzilla, Q-balls,... Numerous Possibility Experimental Techniques Direct Detection : Nuclear recoils in low background detectors : CDMS, CRESST, DAMA, EDELWEISS, GENIUS, UKDMC,.. Indirect Detection Annihilation products in the Halo & GC : - (Extra) Galactic Diffuse Gamma Rays : AMS-02, GLAST, MAGIC, CANGAROO, HESS, VERITAS - Charged Cosmic Anti-Particles (e +, p, d) : BESS-Polar, PAMELA, AMS-02 Indirect Detection Annihilation products from Sun & Earth : - Neutrino(ν) : Antares, AMANDA, Ice-Cube Relic abundance of neutralino dn dt = 3H 2 Ω h χ n < συ > cm 3 < συ > Neutralino Annihilation 2 ρ ( r, z) p. ( R, z, T ) χ Φ =< συ > C ( T ) m χ ( ) n 2 n 2 / s 0

6 CR Source Cas A SN R in X-Rays Crab Nebula AGN Galactic : SNRs, Pulsars, Extragalactic : AGN,.. Exotic : GRBs,.. DarkMatter : WIMPs χχ e +, p -, γ, ν μ,.. p, He, γ, e -, C, N, O, isotropes,... CR Propagation Magnetic Field Synchrotron ISRF Inverse Compton ISM gas Bremsstrahlung, Compton Scattering ISM gas... nuclear interaction, radioactive decay, spallation, CR Detection AMS-02 p, p -, He, γ, e -, e +, μ -, μ +, Li, Be, B, C, N, O, isotopes,...

7 Cosmic Rays Flux Cosmic Rays Composition : P = 88%, He = 9%, e ± = 2%, γ < 1% Primary Comic Rays : (P, He, C, O, Fe) Important for Secondary Production Secondary/Primary Nuclei : (B/C, 10 Be/ 9 Be) Constraints on CR Propagation & Diffusion Models Gamma Rays : Gamma-Rays Astrophysics Secondary Anti-Particles : CR nuclei + ISM π ± μ ± e ± χχ bb, W + W, Z 0 Z 0, ha, hz e +, p, D+X Indirect Dark Matter Detection

8 Matter AMS-02 Detector Anti-Matter Dimension = 3.0m 3.0m 3.0m, 7 t Acceptance = 0.5 m 2 sr, Min. 3 yrs Operation Nuclear Charge Separation up to Z=26 Detector Response to 0.3 TeV Cosmic Rays

9 Superconducting Magnet racetrack coils dipole coils B B Superfluid He Vessel Diameter = 1.2 m, Height = 0.8 m, Weight = 2.3 t B dipol = [T], E stored = 1.15 MJ, I = 459.5[A] Cold Heat Exchanger : Superfluid Helium ( o, 2500 l) Long Duration Operation without refill

10 Silicon Tracker One of eight tracker layers Structure : 5 Planes (8 Layers), Active Area : 6.6 m 2 Total Units : 192 Ladders, Channels : 200,000 Laser Alignment System ( x = 4 μm)

11 Silicon Tracker (cont.d) Position Resolution R max (= pc/ Z e) = 3000 (GV) σ = 10 μm 20% 120 GeV/c muon beam Rigidity (GV) σ x = 10 [μm], ±Q, de/dx Rig. Resol. ~ 1TV(He)

12 ToF & ACC Upper ToF Anti-Coincidence Counter Lower ToF Fast Trigger prim σ t 130 [ps] Layers = 4 (2 + 2) Area = 8 m 2 ToF : 34 Paddles ACC : 16 Cylindrical Shell Paddles

13 TRD One of 328 Straw Modules TRD Octagon Size = m 3, Mass = 350 kg Layers = 20 (328 Modules, 5248 Straws) Gas = 8100 l Xe, 2000 l CO 1bar

14 Longterm Stability Homogeneous Gas Gain SF = 6.3 = 20 yrs operation Precise Integration of 328 Modules Proton Rejection (>100) 2 M z = 100 μm

15 RICH Radiator (Aerogel and NaF) Cerenkov Cone Mirror θ c cosθ c = 1/(βn) PMTs Array Radiators = NaF(n=1.336) and Aerogel(n=1.035) 680 PMT's Array, Spatial Pixel Size = mm 2 Velocity Measurement : Δβ/β 0.07 % (Z=1) Charge Measurement ( Q ) : Z 26 (w/ Tracker + ToF) ( Q ) : N γ Z 2 L [1 - (βn) -2 ] m (β,z,r) = R Z e (1- β 2 ) 1/2 / βc

16 p e ± ECAL Lead foil (t:1mm) Fibers (φ:1mm) 3/9 Superlayers Hamamatsu fine mesh PMT 648 mm 3D sampling E em Structure = 9 Superlayers (Pb + Fiber Sandwich) Thickness = 16.4 X o and ~ 0.5 λ nucl. Standalone Gamma Trigger (single photon, e ± ) Size = cm 2, mass = 640 kg Nr. of PMT = 324 PMTs (granularity = 2 2 cm 2 )

17 Direct Search for Anti-Helium He/He GV / 1000 Sensitivity of Antimatter (He/He) ~ 10-9

18 Nuclear Charge Resolution Accelerator 2.25, 10GeV/n Cosmic Spectra from He to Co with 1% accuracy Understanding of Composition of Galactic Comsic Rays

19 Galactic Cosmic Rays Abundance of Galactic Cosmic Nuclei Permanent Cosmic Radiation Monitor NASA - JSC, Francis A. Cucinotta He Fe As function of time and energy for each nuclei Oxygen flux Time Abundance of Comic Nuclei Energy (GeV/n) p B Ne P Ca Mn Co Production of Secondary Particles Time & Energy Dependence of the Flux Solar Modulation Effects

20 Secondary/Primary CRs Diffusion of Cosmic-Rays Lifetime of Cosmic-Rays CRs Propagation Model τ( 10 Be) = 1.6 Myr Galactic Halo Size CR Confinement Time

21 Photon Detection δe/e~ GeV γ e + + e - Single Photon Mode γ EM Shower 6% 3% γ EM Shower σ θ ~ 0.02 GeV 1.0 o γ EM Shower 0.02 o γ e + + e - Conversion Mode γ e + + e - δe/e = (10.89 ± 0.28)%/ Ε + (2.48 ± 0.05)% σ (θ) = ο ο /Ε

22 Gamma Rays and Sky Survey Gamma Rays Sensitivity Gamma-rays Source : AGN, Pulsars, SNRs, GRB, Nuclear Spectral lines, Sun, CR proton, electron interactions w/ gas, ISRF π 0 decay, Inverse Compton, Bremsstrahlung + Exotic Gamma-rays Sources

23 Proton and Helium Force Field Approx. 2 2 ( E m ) Φ ( E) = ΦIS( EIS) 2 2 ( E m ) E = E IS IS Z φ P He

24 Electron and Positron e - e + π ± μ ± ν μ (99.987%) π 0 2 γ (98.798%) μ ± e ± ν e ν μ (~100%)

25 Positron Fraction and Anti-proton P Critical Issues for exotic sources Need Powerful and Efficient Background Discriminations + Exotic Sources WIMP(neutralino) annihilations

26 SUSY Scenarios (DarkSUSY+Isasugra) msugra Benchmark Points {m 1/2, m 0, tanβ, A 0, sign(μ) } Focus-point region (large m 0 ) No EWSB Funnel region Growing m 0, m 1/2 Cosmologically preferred large tanβ 0.1 < Ω χ h 2 < 0.3 WMAP < Ω χ h 2 < CL Bulk region (low m 0, m 1/2 ) LSP is charged stau hep-ph/ hep-ph/ Co-annihil. Tail region (large m 1/2 )

27 Constraints on SUSY Models LEP : m(χ 1 ) > 46 GeV, m(χ ± )> 104GeV, m h >114.4 GeV BR(b s γ) : CLEO, Belle, BaBar, LEP B X s γ = (3.41± 0.36) 10-4 Muon (a μ = (g μ - 2) / 2) : BNL E821 a μ (SM) = (8) μ = g a μ (Exp) = (6) a μ =[a μ (Exp) -a μ(sm) ] 1010 = 27 ± 10 (2.7 σ) CMB : WMAP < Ω CDM h 2 < (2σ) μ eh 2mc s 2 Uncertainties from Astrophysics : Halo Models (NFW, Moore, Isothermal, Burket,..) Sub-Structure (DM distribution) Cosmic Propagation Models, Solar Modulation Accurate Background Estimations (e +, p -, γ)

28 Galactic DM Halo Models

29 Properties of Neutralino Point L (Bulk region) m 0 =303, m 1/2 =450 GeV tanβ = 47, sign(μ) = +1 A 0 = 0 m χ = GeV

30 Neutralino Annihilations e + P

31 A B C D G H I J K L M

32 Bulk Annihilation Points B C G m χ = 94.91GeV m χ =158.10GeV m χ =148.02GeV tanβ=10 tanβ=10 tanβ=20 I m χ =138.11GeV tanβ=35 L m χ =180.98GeV tanβ=50 χ χ ~ f f f m χ m ~ f 2 Low m 0, m 1/2 Dominant Neutralino Anni. t-channel sfermion exchange

33 Co-annihilation Tail Points A D m χ =242.87GeV m χ =212.45GeV tanβ= 5 tanβ=10 Sign(μ)<0 Low m 0 and Coannihilation extending to large m 1/2 H m χ =388.42GeV tanβ=20 J m χ =309.22GeV tanβ=35 Stau(Stop) co-anni. m χ m τ1 (m t1 ) χ τ~ τ~ τ γ

34 A-annihilation Funnels Points K m χ =554.27GeV Both m 0, m 1/2 grow large tanβ=35 Sign(μ)<0 Resonant very large tanβ ~ & m A ~ 2 m χ Dominant Annihilation s-channel A (or H) exchange M m χ =794.22GeV tanβ=50 χ A (h,z,h) f χ tan β m m W fd m m χ A 2 N 1 f N 3(4)

35 A B C D G H I J K L M

36 Conclusions AMS-02 has capabilities : High Precision, High Statistics Measurements of Charged CRs Gamma-rays : Known Point + Unidentified + Exotic sources With Outstanding Performances at High Energies Essential to Indirect Search for Dark Matter AMS-02 has potential to observe WIMP (Neutralino) annihilation signals in cosmic rays Observation of cosmic positrons, antiprotons and diffuse gamma-rays Investigation cosmologically allowed msugra parameters space with experimental constraints (collider and rare decays bounds) Optimistic but large enhancement mechanism should be existed (local clumpy DM,..) Also Need good understanding on astrophysical (+ instrumental) backgrounds AMS-02 Experiment will provide a discovery potential for New Physics

37 Launch Schedule AMS CERN (2006) 2. AMS Space ESTEC (2007) 3. NASA/KSC (2008) 4. Installation On-board ISS (2008)

38 In 2008 AMS-02 Mission Starts High Statistics, Long Duration Measurements Charged Particles & Nuclei Spectra Direct Search for Antimatter with Sensitivity 10-9 Gamma Rays Astrophysics Existence of Relic Dark Matter Signatures from CRs ISS : m, 420 t, 400km, Inclination = o, revolutions/day,