1. Matter/antimatter asymmetry in the Universe? The CR antimatter component and its direct detection Baikal summer school, July 2005 P.Spillantini, University and INFN, Florence, Italy

2. GeV | TeV | PeV | EeV | ZeV | High Z [ENTICE, ECCO] Light elements and Isotopes [ACE] Antiparticles and Antinuclei [BESS, PAMELA, AMS] Elemental Composition [CREAM, BEAR, ACCESS?,NUCLEON?, INCA?, PROTON-5?] Direct detection Balloons & Satelites Indirect detection (EAS) [arrays & florescence] CR flux – 5 boxes Extreme Energy CR AUGER, TUS, EUSO, KLYPVE?,OWL??

11. Nucleus Star galaxy Cluster of galaxies Super-cluster ?? Anti-Nucleus Anti-Star Anti-galaxy Anti-Cluster of galaxies Anti-Super-cluster Anti - ??

13. Antiparticles and CR difficulties needed for antip : secondary production high energy (  100 GeV/n) high energy (  1 TeV) long diffusion time long path galactic wind for antiN: CP violation  Sakharov conditions All Matter Universe Matter and antimatter in separated domains  Symmetric Cosmologies Asymmetric Cosmologies Both possible in Big Bang theories  It is possible rely only on observations antip spectrum antiN search  From e.m. observations Only local asymmetry (~10 -8 of the Universe volume)  Antiparticles and CR

14. Antip: curve

15. Antip: curve + vecchi dati

16. Antip: curve + nuovi dati

17. Antip: curve + nuovissimi dati

18. (no assumption on antiHe spectrum) AMS STS-91 (1998 ) (antiHe spectrum same shape of He spectrum) Antimatter (no PAMELA) ANTIMATTER LIMITS

19. AntiM. ‘ideal scheme’

20. Antiproton Positron

21. Antip: curve + vecchi dati

22. ASTROMAG on FREEDOM

23. Permanent presence in Space International Space Station “FREEDOM” Hubble Space Telescope

24. CGRO AXAF (CXO) HST SIRTF + Particle-Antiparticle Superconducting Magnet Facility (ASTROMAG) + Very Long Base Interferometer (VLBI) + Advanced Composition Explorer (ACE) Great Observ. (+scritte)

25. Experiments approved for the first phase of the ASTROMAG facility WIZARD:antiparticle spectra, antinuclei, etc..(USA, Italy, Sweden, Germany) LISA:elemental and isotopic spectra, etc. (USA, other??) MAGIC-SCINATT: elemental composition at knee (USA, Japan) Experiments for ASTROMAG

26. EUSO, (OWL) HNC ISTP/ WIND A.C.E. ASTROMAG PAMELA, AMS ENTICE, ECCO NASA Part. Astroph. Program Cut-off momentum

27. Balloon Flights - BESS (93, 95, 97, 98, 2000) - Heat (94, 95, 2000) - IMAX (96) - [BESS Long duration flights (2004)] (Wizard Coll.) - MASS – 1,2 (89,91) - TrampSI (93) - CAPRICE (94, 97, 98) - [  in flight (2004?)]

29. New Generation of Antimatter Researches in Cosmic Rays New Generation of AntiM a)Longer duration ballooning b) Experiments in space

30. payload services He Air Class A Balloons 2.8 Mm 3 @ 5 g/cm 2 lifting power ~ 11t Balloon 5 t services 3 t payload 3 t Open Balloons

31. Km 0 C°C° -100 40 Atmospheric temperature versus Altitude 0 Atmosph. T vs Altitude

32. Ballooning in Antarctica

33. BESS - Polar

34. BESS Polar LDB

36. New Generation of Antimatter Researches in Cosmic Rays New Generation of AntiM b) Experiments in space

37. O. Adriani 1, M. Ambriola 2, G.Barbarino 16, L.M. Barbier 4, G. Bazilevskaja 6, R. Bellotti 2, D. Bergstrom 7, M. Boezio 3, E. Bogomolov 10, V. Bonvicini 3, M. Boscherini 1, F. Cafagna 2, P. Carlson 7, M. Casolino 8, G. Castellini 15, E.R. Christian 4, M. Circella 2, R. D’Alessandro 1, C.N. De Marzo 2, M.P. De Pascale 9, G. Furano 9, A.M. Galper 11, A. Grigorjeva 6, P. Hansen 7, S.V. Koldashov 11, M.G. Korotkov 11, J.F. Krizmanic 4, S. Krutkov 10, A. Iannucci 9,B. Marangelli 2, A. Menicucci 9, W. Menn 12, V.V. Mikhailov 11, M. Minori 9, N. Mirizzi 2, J.W. Mitchell 4, E. Mocchiutti 7, A.A. Moiseev 11, A. Morselli 9, R. Mukhametshin 6, J.F. Ormes 4, G.Osteria 16, P. Papini 1, G. Percossi 9, P. Picozza 9, M. Ricci 5, P. Schiavon 3, M. Simon 12, R. Sparvoli 9, P. Spillantini 1, P. Spinelli 2, S.A. Stephens 13, S.J. Stochaj 14, Y. Stozhkov 6, R.E. Streitmatter 4, F. Taccetti 15, A. Vacchi 3, E. Vannuccini 1, G. Vasiljev 10, S.A. Voronov 11, N. Weber 7, R. Wischenwksi 9,Y. Yurkin 11, N. Zampa 3, GL. Zampa 3 1 University and INFN, Firenze (Italy) 2 University and INFN, Bari (Italy) 3 University and INFN, Trieste (Italy) 4 NASA Goddard Space Flight Center Greenbelt (USA) 5 Laboratori Nazionali INFN, Frascati (Italy) 6 Lebedev Physical Institute (Russia) 7 Royal Institute of Technology, Stockholm (Sweden) 8 Electronic Engineering Department, II University, Roma-Tor Vergata (Italy) 9 II University and INFN, Roma-Tor Vergata (ltaly) 10 Ioffe Physical Technical Institute (Russia) 11 Moscow Engineering and Physics Institute, Moscow (Russia) 12 Siegen University, Physics Department, Siegen (Germany) 13 Tata Institute of Fundamental Research, Bombay (India) 14 Particle Astrophysics Laboratory, NMSU, Las Cruces (USA) 15 Istituto di Ricerca Onde Elettromagnetiche CNR, Firenze (Italy) 16 University and INFN, Napoli (Italy) Wizard Collaboration

38. Balloon exp’s MASS (89) MASS1(91) TS93 (93) CAPRICE (94) CAPRICE (97) CAPRICE (98) [CAPRICE (03)] Low En. C.R. in orbit NINA (98) NINA2 (00) Life Science on MIR and ISS SIL-EYE-1 (95) MIR SIL-EYE-2 (97) MIR SIL-EYE-3 (02) ISS ALTEA (04) ISS PAMELA Background

39. Neutron Detector PAMELA: apparato nudo 1024 tubes, Ø=4mm (distributed on 18 layers) 5 magnets, 4.8 kG @ center  IMAGING (2.4mm granularity)  16 Xo deep  44 Si layers + W  4.4 kchannels Scintillation Counters Hodoscopes 2 layers 1 layer 5 counters 36 He3 counters MASS = 480 kg POWER = 345 W GF = 20.5 cm2sr MDR = 740 GV/c Si  -strip, double side, double metallization  6 planes x 6 sensors  37 kchannels

40. PAMELA Positrons50 MeV - 270 GeV Antiprotons80 MeV – 190 GeV Limit on antinuclei ~7 10 -8 (He /He) Electrons50 MeV – 2TeV Protons80 MeV – 700 GeV Nuclei< 300 GeV/n (Z  8) study of the solar modulation after the 23 rd solar cycle maximum. GF 20.5 cm 2 sr Mass 480 Kg Dimensions cm3 120 x 40x45 Power Budget 345W PAMELA (RIM 02)

41. Antip (3 andamenti) Spillover of p on antip = 0.2 of the antip flux

42. Distortion of the secondary positron fraction induced by a signal from a heavy neutralino. Distortion of the secondary antiproton flux induced by a signal from a heavy Higgsino-like neutralino. P.Picozza and A.Morselli,astro-ph/0103117 standard Expected data from Pamela for two years of operation are shown in red. Distortion e+ & antip by heavy neutralino.

43. BESS (2004+2006 LDB flights) ANTIMATTER LIMITS AMS STS-91 (1998 ) (antiHe spectrum same shape of He spectrum) (2005-8 ) AntiM (con PAMEA&AMS)

44. Razzo Soyuz

48. (no assumption on antiHe spectrum) AMS STS-91 (1998 ) (antiHe spectrum same shape of He spectrum) BESS (2004+2006 LDB flights) AMS 02 (2005-8) (2003-6 ) AntiM (con PAMEA&AMS) ANTIMATTER LIMITS

49. End of the movie!!