results of the PAMELA mission CR from space based observatories: Piero Spillantini University and INFN, Florence, Italy 3 August 2009 BINP, Akademgorodok, Novosibirsk 19-th century: - discovery of electricity - acceleration of the electrons - production of X-rays Energy up to few KeV End of 19-th century - discovery of natural radioactivity Energy up to few MeV Beginning of 20-th century: - access to high atmosphere - discovery of Cosmic Rays Energy up to many GeV Years 60s of 20-th century: - access to space Astrophysics Years 70s of 20-th century: - permanent presence in space The Great Observatories and the Freedom Space Station Particle Physics Second half of 20-th centuries - accelerators reach CR energies Permanent presence in Space International Space Station FREEDOM Hubble Space Telescope Space Station FREEDOM (1983) CGRO AXAF (CXO+ XMM) HST SIRTF Heavy Nuclei Collector (HNC) and Particle-Antiparticle Superconducting Magnet (ASTROMAG) facilities on board of the Freedom SS + Very Long Base Interferometer (VLBI) + Advanced Composition Explorer (ACE) Great Observ. (+scritte) HNC A.C.E. ASTROMAG NASA Part. Astroph. Program - 3 Cut-off momentum GeV | TeV | PeV | EeV | ZeV | Direct detection Balloons & Satellites Indirect detection (EAS) [arrays & florescence] CR flux 5 boxes 31 decades 13 decades High Z Light Elements and Isotopes Antiparticles and Antinuclei Elemental Composition Extreme Energy CR Direct detection Balloons & Satellites Indirect detection (EAS) [arrays & florescence] Cosmic Rays from Space CGRO AXAF (CXO+ XMM) HST SIRTF Heavy Nuclei Collector (HNC) and Particle-Antiparticle Superconducting Magnet (ASTROMAG) facilities on board of the Freedom SS + Very Long Base Interferometer (VLBI) + Advanced Composition Explorer (ACE) Great Observ. (+scritte) CANCELLED HNC A.C.E. ASTROMAG BESS, PAMELA, AMS AGILE, Fermi-GLAST ENTICE, ECCO OASIS NASA Part. Astroph. Program - 3 Cut-off momentum for HNC : precursors on LDEF and MIR, but ENTICE + ECCO not funded, OASIS?? for ASTROMAG : - LISA collaboration (USA) for isotopes studies continued by ballooning, but it was stopped by the ISOMAX accident. - MAGIC-SCINATT collaboration (USA+Japan) continued by ballooning, but with limited results, ACCESS on ISS never funded. -WIZARD collab. (It,USA,S,D) continued by ballooning, constructed with Russia the Russian-Italian Mission (RIM) program, flew PAMELA [and other missions: SilEye-1-2-3, NINA, NINA-2, ALTEINO, ALTEA] - Japanese-USA built up the BESS ballooning program - a new Elementary Particle physicist collaboration (AMS) joined in studing the same thematic - ASTROGAM collab. disbanded, AGILE and Fermi-GLAST launched in 2008 Antimatter High Z Isotopes Elemental composition CR from space based observatories: What happened in the last 20 years? [HE s] - Loss of Challenger Shuttle (1986) - Freedom Space Station cancelled (beginning of 1991) Consequently: HNC and ASTROMAG facilities cancelled Antimatter on a Cosmological scale? Fundamental question (on 30s to 60s): how can the Universe contain equal amounts of M and antiM ?? Problem of separating M and antiM on large scale Big Bang models based on statist. fluct. M objects < M Sun #Baryon / #Photon #Baryon / #Photon t s #Baryon / #Photon now 1964: CP violation in nature 1967: Sakharovs conditions to achieve baryon asymmetry in the Early Universe: (1) Baryon decay allowed (2) CP violation allowed (3) A period out of equilibrium The three Sakharovs conditions: allow the possibility of an all Matter Universe CP built in the Lagrangian but also: offer a solution to the Matter-antiMatter separation problem in a Baryon Symmetric Universe CP is spontaneous there are DOMAINS with either Matter or antiMatter inflaction can increase these DOMAINS to astronomical scale (indirect observation) high energy ( 100 GeV/n) (direct observation) --- Experimental summary ( signal Limited Statistics by Long Duration Balloon Flights in Antarctica antiproton at low energy (dark matter etc...) and antinuclei at low energy BESS: for Antimatter Researches in Cosmic Rays it is necessary to go in space New Generation of AntiM [PAMELA + AMS-2] PAMELA Satellite borne permanent magnet spectrometer AMS-2 ISS borne superconducting magnet spectrometer Antiproton and positrons up to highest energies Antinuclei up to highest energies Dark matter searches Antiproton and positrons up to highest energies Antinuclei up to highest energies Dark matter searches Solar Physics from WIZARD to PAMELA Experiments approved for the first phase of the ASTROMAG facility Experiments for ASTROMAG WiZard: Russian Italian Missions (RIM) 1989 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 2006 PAMELA NINA-1NINA-2SILEYE-1 SILEYE-2 Alteino-SILEYE-3 ALTEA-SILEYE-4 M 89 M 91 TS 93 C 94 C 97 C 98 SILEYE-2SILEYE-1 ALTEINO: SILEYE-3 ALTEA: SILEYE-4 LAZIO SIRAD MASS-89, 91, TS-93, CAPRICE NINA-2 NINA-1PAMELA LAZIO-SIRAD Antimatter search Life Science Solar physics 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. DAlessandro 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) Neutron Detector PAMELA: apparato nudo 5 magnets, 4.8 center IMAGING (2.4mm granularity) 16 Xo deep 44 Si layers + W 4.4 kchannels Scintillation Counters Hodoscopes 2 layers 1 layer 9 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 Readout pitch 50 Resolution 10 9 triggers recorded and under analysis Mirko Boezio, INFN Trieste - ICHEP08, 2008/08/01 32.3 GV positron 36 GeV/c interacting proton Data Analysis The Analysis has been done using only flight data Beam tests and MC simulations only for cross-checks Antiprotons Antiproton-to-proton ratio astro-ph PRL 102 (2009) *preliminary* (Petter Hofverberg s PhD Thesis) Antiproton-to-proton ratio Secondary Production Models No evidence for any antiproton excess Solar modulation CR + ISM p-bar + ~20% Antiproton-to-proton ratio Secondary Production Models (Donato et al. 2001) Diffusion model with convection and reacceleration Solar modulation: spherical model (f=500MV ) Uncertainty band related to propagation parameters Additional uncertainty of ~25% due to production cs should be considered !! (Ptuskin et al. 2006) GALPROP code Plain diffusion model Solar modulation: spherical model ( f=550MV ) (Moskalenko et al. 2006) GALPROP code Plain diffusion model Solar modulation: drift model ( A300 GeV) LKP -- M= 300 GeV (Hooper & Profumo 2007) Primary positron sources Astrophysical processes Local pulsars are well- known sites of e + e - pair production: they can individually and/or coherently contribute to the e + e - galactic flux and explain the PAMELA e + excess (both spectral feature and intensity) if one or few nearby pulsars dominate, anisotropy could be detected in the angular distribution possibility to discriminate between pulsar and DM origin of e + excess All pulsars (rate = 3.3 / 100 years) (Hooper, Blasi, Serpico 2008) Example: pulsars H. Yksak et al., arXiv: v2 Contributions of e- & e+ from Geminga assuming different distance, age and energetic of the pulsar diffuse mature &nearby young pulsars Hooper, Blasi, and Serpico arXiv: Pulsars: Most significant contribution to high-energy CRE: Nearby (d < 1 kpc) and Mature ( Tyear) Pulsars S. Profumo Example of fit to both Fermi and Pamela data with known (ATNF catalogue) nearby, mature pulsars and with a single, nominal choice for the e+/e- injection parameters Preliminary Cosmic-ray antimatter search BESS combined (new) expected Galactic cosmic-ray origin & propagation Cosmic Rays Propagation in the Galaxy PAMELA: Galactic H and He spectra Preliminary !!! Very high statistics on a very wide energy range - Precise measurement of spectral shape - Possibility to study time variations and transient phenomena Local spectrum: injection spectrum galactic propagation Local primary spectral shape: study of particle acceleration mechanism Power-law fit: ~ E - ~ 2.76 still large discrepancies among different primary flux measurements (statistical errors only) Proton flux Interstellar spectrum July 2006 August 2007 February 2008 Decreasing solar activity Increasing GCR flux Solar modulation (statistical errors only) B/C Preliminary PAMELA preliminary results Li/C Be/C RED: JULY 2006 BLUE: AUGUST 2007 P/(cm^2 sr GeV s) Secondary particles (reentrant albedo) Penumbra Primary and secondary spectra: Magnetic equator RED: JULY 2006 BLUE: AUGUST 2007 P/(cm^2 sr GeV s) Primary and secondary spectra: Intermediate latitudes Secondary particles (reentrant albedo) Penumbra p e e p A look to Earth: the geomagnetic field SAA South Atlantic Anomaly Proton spectrum in SAA, polar and equatorial regions Trapped Galactic Spectrum of proton radiation belt inside the SAA B < 0.19 G 0.19 G B < 0.20 G 0.20 G B < 0.21 G B > 0.30 G 0.22 G B < 0.23 G 0.21 G B < 0.22 G Always: 10 GV < cutoff < 11 (statistical errors only) Solar Physics Solar CR propagation Solar Energetic Particle events (SEPs) 80 MeV 50 MeV Proton detection threshold Electron detection threshold -Solar modulation effects -High energy component of Solar Proton Events (from 80 Mev to 10 GeV) -High energy component of e- and e+ in Solar Events (from 50 MeV) + Nuclear composition of Gradual and Impulsive Events + He isotopic composition Preliminary! December 13th 2006 event SEPs accelerated during CMEs SEP spectral shape and time evolution study of particle acceleration mechanisms in CME PAMELA is measuring the Antiprotons and Positrons to the high energies (> 150 GeV) with an unprecedented statistical precision setting a new lower limit for finding Antihelium looking for Dark Matter candidates providing measurements on elemental spectra and low mass isotopes with an unprecedented statistical precision and is helping to improve the understanding of particle propagation in the interstellar medium measuring the high energy tail of solar particles. For the future (other >3 years data): Fluxes of e+ (300GeV), e- (500 GeV), p (700GeV) Fluxes of light nuclei (up to O) and light isotopes Monitoring of solar activity by SEP measurement Anomalous CR (??), Jovian e- (?) AMS-2 Cosmic-ray antimatter search BESS combined (new) expected AMS-2 on ISS AMS Altitude: Km Inclination: 51.7 AMS-02 on ISS In Orbit 2010 TRD RICH Vacuum Case Tracker MAGNET He Vessel The Completed AMS Detector on ISS Transition Radiation Detector (TRD) Silicon Tracker Electromagnetic Calorimeter (ECAL) Magnet Ring Image Cerenkov Counter (RICH) Time of Flight Detector (TOF) Size: 3m x 3m x 3m Weight: 7 tons Pamela and AMS-02 Space Observatories at 1AU Jovian electrons Anomalous Nuclei Nearby e - Sources Magnetospheric physics Solar Modulation Solar Energetic particles Matter : Antimatter PBH Dark Matter Galactic cosmic rays R. B., SAA, Albedo, secondary particle Atmosphere 23 Xo 40 km Extended Air Shower Particle Astrophysics Experiments (further acceleration?) Propagation (through Galaxy) SIRFT CGRO AXAF(CXO) HST VLBI Modulation (through Heliosphere) Cosmic Ray creation acceleration injection Direct detection Underground, Under-ice, Underwater Cosmic rays: about 10 Myears in the Galaxy (6-7 g/cm 2 ) Definition of Astrop.expts (con animazione) Thank you for yor attention C Gazie per lattenzione