Trento Summary: Antimatter & Dark Matter Search. Status Dark Matter Search
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1 Trento Summary: Antimatter & Dark Matter Search Th. Kirn & Th. Siedenburg Status Dark Matter Search W. Wallraff Hausseminar, November 9 th 200
2 Trento: Matter, Antimatter, Dark Matter How to reach Trento by car Along the A22 Brenner motorway and the S.S.2 Abetone and Brenner. The S.S.45 bis, Gardesana occidentale from Brescia and the Gardesana orientale from Verona; from Milan the S.S.42 to Tonale and Mendola; from Venice the S.S.47 of Valsugana; from Vicenza the S.S.46, all converge on Trento. Villa Tambosi Kirn
3 II International Workshop on Matter, Antimatter and Dark Matter ECT*, Villa Tambosi, Trento, October 29 and 30th 200 PROGRAM: FIRST DAY, October 29th: Registration MORNING SESSION : Chairman: M. Panasyuk Recent Measurements on Cosmic Rays Spectra and Composition 9.00 Welcome by ECT* Scientific Secretary, Prof. Renzo Leonardi R. Battiston (Perugia): Status of AMS on the ISS J. Casaus (CIEMAT): Review of precision measurements on high energy hadrons B. Bertucci (Perugia): Review of precision measurements on high energy leptons Coffee break P. Zuccon (Perugia): FLUKA simulation of the interaction of high energy CR with the atmosphere T. Sanuki (Tokyo): Review on balloons muon measurements in the atmosphere M. Gibilisco (ECT*): An analytical solution of the cosmic rays transport equation in the presence of the geomagnetic field A. Sakharov (ETHZ): Macroscopically large antimatter regions in the Universe 3.5 Lunch (Villa Tambosi) AFTERNOON SESSION : Chairman: G. Battistoni Interaction of Cosmic Rays with the Earth Geomagnetic Field E. Fiandrini (Perugia): Trapped leptons measurement by AMS Kirn 2
4 M. Buenerd (Grenoble): Secondary atmospheric particle populations at balloon and satellite altitudes D. Heynderickx (Belgium): Review on modelling of radiation belts Coffee break M. Casolino (Roma2): Review on NINA- and NINA-2 results V. Mikhailov (Moscow): Low Energy Electrons and Positrons with Maria2 instrument M. Panasyuk (MSU, Moscow): Review on anomalous trapped CR belts M. Durante (Napoli): Review on biological implications of recent measurements of trapped CR on LEO A. Masiero (SISSA): Neutrinos and cosmology today Social Dinner (Ristorante Orso Grigio ) SECOND DAY, October 30th: MORNING SESSION : Chairman: F. Cervelli Recent Developments on atmospheric neutrinos M. Shiozawa (ICRR, Tokyo): Review of experimental results on cosmic rays neutrinos M. Vietri (Roma3): Extreme Energy Cosmic Rays and their sources and neutrino astronomy T. Stanev (Bartol): State of the art in calculations of the atmospheric neutrino flux Coffee break V. Plyaskine (ITEP): A recent new atmospheric neutrinos calculation G. Battistoni (Milano): Calculation of secondary particle production in atmosphere and hadronic interaction F. Vissani (LNGS): Massive neutrinos and theoretical developments F. Cei (Pisa): Supernovae neutrinos (experimental status) 3.00 Lunch (Villa Tambosi) AFTERNOON SESSION : Chairman: B. Bertucci Dark matter and gamma rays P. Ullio (SISSA): Review of CR and Dark Matter Searches P. Giommi (ASI SDC): Review of previous X-rays missions N. Produit (Versoix): INTEGRAL, a gamma ray observatory Coffee break M. Tavani (Milano): Theoretical review on physics with gamma rays M. Pohl (Geneva): Gamma physics with AMS V. Choutko (MIT): AMS background studies for positrons and gamma rays A. Morselli (Roma2) : Dark Matter Search with gamma rays with EGRET and GLAST Kirn 3
5 Antimatter Search Kirn 4
6 Composition and Energy Spectrum of Cosmic Rays Relative abundance of particles, elements and isotpes is related to: Primordial nucleosynthesis for the particles created just after the Big-Bang: γ,p,e,d,he 4,He 3,Li 7 Astrophysical sources accelerating primaries: e,p,he,c,o,fe Interactions with interstellar gas create secondaries: e ±,p,p, Li, Be, B propagation described by Leaky Box model Intensity [m -2 s - sr - ev - ] γ p e + + e - He AMS rate 0 3 / s / min / d / y Energy/Nucleon [GeV] Kirn 5
7 Direct Antimatter Search p: - Measurements do not provide evidence for extragalactic antimatter - p-flux near earth can be explained mainly by secondary interactions of cosmic rays 0 - Cosmic Ray P BESS(95+97) BESS(93) IMAX CAPRICE 0-3 p flux (m -2 sr - sec - GeV - ) Kinetic Energy (GeV) Bottino Bergstrom Biebar Mitsui λ(r,β) Mitsui λ(r) p /p ratio BESS(95+97) BESS(93) CAPRICE Golden et al. Bogomolov et al. Buffington et al. IMAX PBAR LEAP MASS2 0-0 Kinetic Energy (GeV) Kirn 6
8 Direct Antimatter Search antinucleon: Discovery of antinucleus (He) evidence for cosmologically significant amounts of antimatter Discovery of C antistars Presently, no antinucleus with Z 2 has ever been found in cosmic radiation - ASM-0 98: He/He <. 0 6 ; R<00GV - BESS 93-98: He/He < ; R<6GV Kirn 7
9 AMS0 STS-9 Precursor Flight Scintillators Low Energy Particle Shield Honeycomb Low Energy Particle Shields Particle Trajectory TOF Layers S S2 Foam lectronics Magnet Veto Counters Silicon Wafers Honeycomb Computers m Permanent Magnet ACC Tracker T Planes T2 T3 B=0.5T T4 T5 T6 Nd-Fe-B: 46 MGOe S3 S4 Aerogel Photomultipliers z^ Aerogel Cerenkov ^x ^ y STS9 2- June 998 Shuttle Discovery Mean altitude 370 km 90 min orbitinclined at5.7 Trigger-rate Hz Recorded 0 8 events in 00 h Kirn 8
10 AMS0 Results Maximum rigidity (p/z) depends on magnetic latitude Flux(Particles/s/MeV) < θ M <. θ M >. 0.9 < θ M < < θ M < 0.9 Proton Flux 0.7 < θ M < < θ M < < θ M < < θ M < < θ M < 0.4 θ M < Kinetic Energy (GeV/N) Kirn 9
11 AMS0 Results He 0 events AMS STS - 9 He events Events Antimatter/Matter Upper Limit 95% CL Z= GV Sign Rigidity Published Conservative Limits Smoot et al. (975) Golden et al. (997) Buffington et al. (98) BESS AMS Rigidity (GV) Kirn 0
12 AMS0 Results Events C Li B Be N E Tracker (MIPS) AntiMatter/Matter Upper Limit R min =.6 GV Excluded AMS STS < Z < R GV max Golden et al. (74) Smoot et al. (75) Antimatter/Matter Upper Limit 95% CL Z> Smoot et al. (75) AMS Rigidity (GV) Kirn
13 AMS02 A Particle Spectrometer for ISS How to suppress proton background to 0 6 perform high statistic tracking up to TV? Large acceptance 0.5 m 2 sr in orbitfor 3 years TRD Particle ID & 3D tracking 20 layers fleece + Xe/CO channels 6mm straw-tubes and p + /e + < 0 2 (0-300 GeV) TOF,2 Trigger σ t 25ps Anticoincidence (Veto) counter Silicon strip tracker with internal laser alignment 6m 2 in 3 double + 2 single xy layers σ charge separation up to TV Superconducting Magnet (ETH) B = 0.9T V = 0.6m 3 TOF 3,4.3m distance to TOF,2 p + /e + > 3σ below 2 GeV PFRICH AGL(+NaF) Radiator for A 27 and Z 28 separation > 3σ from -2 GeV ECAL 3D sampling lead/scint.-fibre with p-e matching and shower-shape p + /e + < 0 4 (0-300 GeV) Kirn 2
14 AMS02 Expectations AMS0 statistics 0 3 momentum reach 6 Yield in GV/c intervals, for 3 years on ISS AMS on ISS Region of antimatter (He) AMS-0 ~0 9 events Helium Statistics /GV/c 0 9 He GV p + > TeV 0 7 e > 0 GeV Kirn 3
15 AMS02 Expectations Yield in GeV/c intervals, for 3 years on ISS Yield in GeV/c intervals, for 3 years on ISS AMS-0 AMS-0 Protons ~3 x 0 6 events Energy > TeV GeV/c Electrons ~0 7 events Energy > 0 GeV GeV/c Yield in GeV/c intervals, for 3 years on ISS Yield in GeV/c intervals, for 3 years on ISS AMS-0 Antiprotons 0 6 events Energy > 5 GeV GeV/c AMS-0 Positrons 4 x 06 events Energy > 5 GeV GeV/c Kirn 4
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