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Indirect Dark Matter Search with AMS

Cosmic Ray Astrophysics with AMS02 – PS1 D.Haas. Indirect Dark Matter Search with AMS. T. Siedenburg for the AMS Collaboration. 6 emes Rencontres du Vietnam, Hanoi 9-Aug-2006. Cosmic Puzzle. Clues in CR Spectra ?. Precision Cosmology

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Indirect Dark Matter Search with AMS

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  1. Cosmic Ray Astrophysics with AMS02 – PS1 D.Haas Indirect Dark Matter Search with AMS T. Siedenburg for the AMS Collaboration 6emes Rencontres du Vietnam, Hanoi 9-Aug-2006

  2. Cosmic Puzzle Clues in CR Spectra ? Precision Cosmology WMAP CMB Power SpectrumSDSS 3D Matter SpectrumHubble SN-Ia Redshift 1/s/GeV 1/d/GeV T. Siedenburg AMS Dark-Matter

  3. Detecting a SUSY Neutralino as Dark-Matter Candidate e Structure: Cold Dark-Matter WIMP: Weakly Interacting Massive Particle Direct Detection current local density SD/SI Visible Matter Dark Matter Halo Indirect Detection: Neutralino-Annihilation Solar/terrestrial neutrinos GC solar lifetime average g AMS02 Dark-Matter Detection Spectrum/Line from GC Charged Anti-Particles 1GeV-1TeV: 5 kpc Sphere T. Siedenburg AMS Dark-Matter

  4. e+e+ + e– Signal propagation and Background Galactic Models and Solar Modulation Nuclear abundance: B, C, 10Be, 9Be, ... Standard particles: e, pSecondary prod.: e, p Tracking + charge / isotope separation Signal from WIMP annihilation Particle Generators & DM Density Contributions to : e, p, g, D Proton supression by 106 Electron supression by 104 Gamma reconstruction (energy / angle) Dark Matter Detection Requirements T. Siedenburg AMS Dark-Matter

  5. STS-912.-12.JUN 1998 AMS01 Precursor Flight Permanent Magnet 0.15 Tm26 Si-Strip Tracker Planes4 Sc-Panel TOF Trigger LayersAerogel Čerenkov + Veto ACC 108 Events in 10 days AMS01 T. Siedenburg AMS Dark-Matter

  6. Proton Suppression:Bremsstrahlung ~ 1/m2 q1 q2 • 3 track events with converted gmiddle track from primary e • Efficient track reconstruction • Reject high dE/dX |Q|>1 events • Keep backtraced extraterrestrial events • Background e– with wrong charge p  p p+p– p  p p0  p e+e– (g) • Reconstruct invariant masses at radiation and conversion vertex AMS01 Positron Selection above 3.5 GeV Primary Positron TOF 1 Photon TOF 2 @ @ TOF 3 TOF 4 SecondaryPositron SecondaryElectron T. Siedenburg AMS Dark-Matter

  7. Proton MC Selected AMS01 Positrons Background from p and e MCReweight for geomagnetic cutoff spectral indexScale to measured p and e flux Geomagnetic Cutoff 118 Selected 24.9 Protons 6.5 Electrons Spectral Index T. Siedenburg AMS Dark-Matter

  8. Acceptance and Livetime Corrections for Flux Calculation dF / dE = N / (A ∙ T ∙ DE) For each 4sec Flight Period* Get Shuttle Coordinates * Backtrace particle in 9 cosq, 8 j, 8 p bins * Sum DAQ livetime for extraterrestrial tracksSeparately up/down e+/e– 5000 CPU Days “Upward” Shuttle Floor Trapped Particle Geometrical Acceptance A Average Livetime T T. Siedenburg AMS Dark-Matter

  9. e+e+ + e– AMS01 Positron Fraction AMS01 Lepton Fluxes J.Olzem, H.Gast J.Olzem, H.Gast Cancellation of systematics in fraction( Detector acceptance / Livetime ) T. Siedenburg AMS Dark-Matter

  10. Tracking and Particle ID 3m 6700 kg Improve with AMS02 TRD Xe/CO2Straws p+rej. >102 1-300 GeV 0.5m2sr 3.5m TOF Trigger (2up+2low) st: = 120ps: b dE/dX: Z Superconducting Magnet 0.8 Tm2 2.5t superfluid He Silicon Strip Tracker 6m2 p up to 1TV and Z(dE/dX) RICH Aerogel/NaF 3sSep. A~26 1-12 GeV + Z ECAL 3D lead/scint-fibre h rej. >103 1-300 GeV 0.05m2sr 3 years above atmosphere T. Siedenburg AMS Dark-Matter

  11. TRD Positron Proton Separation dE/dX from TrackerRICH (and TOF) Charge / Isotope Separation A/Z = 2 GSI Beamtest 1 Layer 0 20 Layer TRD Beamtest bfrom RICH (1-12 GeV/n) Momentum from Trackerwith Supercond. Magnet Mass for Isotope Sep. T. Siedenburg AMS Dark-Matter

  12. 0.4 X0 ECAL Conversion AMS02 GAMMA DETECTION ECAL 16.4 X018 x/y samplings Effective Area / cm2 Energy and angle 1 GeV – 1 TeV h/e Separation: 103 shower-shape Acceptance: 0.05m2sr E / GeV Angular Resolution / deg Energy Resolution / % Star Tracker: 30“ E / GeV E / GeV T. Siedenburg AMS Dark-Matter

  13. Determine Propagation Model Parameter Errors from Variation with AMS02 MC Error Estimation Secondary/Primary: Traversered MatterUnstable/Stable: Confinement Time AMS02 Nuclei and Isotopes 105 C 104 B > 100 GeV/n in 3 years 10510Be 0.5-10 GeV in 3 years B/C 10Be / 9Be Agl NaF AMS02 MC TOF E / GeV/n E / GeV/n T. Siedenburg AMS Dark-Matter

  14. 4x106 AMS02 Positrons from 5-300 GeV e+e+ + e– Proton Rejection 106 from TRD 1000-100 ECAL 100-1000 E/p 10 Improve precision of SM background predictionto enhance sensitivityfor subtle deviations within the same dataset e.g. WIMP annihilations… T. Siedenburg AMS Dark-Matter

  15. Test of mSUGRA parameter space with precise positron fraction Focus Point Rapid Funnels Constraints: gm-2 mhWCDMbsg BSm+m–mt=175.2GeVmb=4.2GeVas=0.1187 Fixed: A0 = 0 sign(m) = +1 Free: m0 m1/2 tanb E / GeV E / GeV BF 6.1e3 BF 1.7e5 Bulk Point Co-Annihilation BF 1.2e5 BF 3.2e3 E / GeV E / GeV T. Siedenburg AMS Dark-Matter

  16. AMS02 Antiprotons and Gammas Electron Rejection 104 from TRD + ECAL + E/p 1 GeV EGRET Excess and de Boer DM ring interpretation hard to confirmCuspier Halo-Profile: flux x10 106 Antiprotons 0.5-100 GeV Sensitivity: 7x10-9 / cm2 / s Antiprotons sensitive to solar modulation Ro = 8.0 kpc, r0 = 0.3 GeV/cm3, a = 20 kpc LIS + Geomagn.cutoff p A.Jacholskowska et al.Phys.Rev.D 74 023518 (2006) from galactic center m0= 60 GeVm1/2= 250 GeVA0=0 tanb=10 m>0 BF 2.0e1 (3 years) T. Siedenburg AMS Dark-Matter

  17. Conclusion AMS Dark-Matter Detection AMS01: Successful flight, HEAT Positron excess not excluded AMS02: Complete, large acceptance, 3 years above atmosphere Tracking – 3 TV RICH 1 – 12 GeV Calorimetry 1 GeV – 1 TeV TRD 1 – 300 GeV High statistics e, p and AZ to tune cosmic models e, p, and g spectra for combined dark-matter fit AMS02 is on schedule for flight in 2009 Shuttle isback to flight T. Siedenburg AMS Dark-Matter

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