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Diapositiva 1 PAMELAPAMELA SpaceSpace MissionMission FirstFirst ResultsResults inin CosmicCosmic RaysRays Piergiorgio Picozza INFN & University of Rome “ Tor Vergata” , Italy Virtual Institute of Astroparticle Physics June 20, 2008 Robert L. Golden ANTIMATTERANTIMATTER Antimatter Lumps Trapped in our Galaxy antiparticles Antimatter and Dark Matter Research Wizard Collaboration -- BESS (93, 95, 97, 98, 2000) - MASS – 1,2 (89,91) - - Heat (94, 95, 2000) --TrampSI (93) - IMAX (96) -CAPRICE (94, 97, 98) - BESS LDF (2004, 2007) - ATIC (2001, 2003, 2005) - AMS-01 (98) AntimatterAntimatter “We must regard it rather an accident that the Earth and presumably the whole Solar System contains a preponderance of negative electrons and positive protons. It is quite possible that for some of the stars it is the other way about” P. Dirac, Nobel lecture (1933) 4% 23% 73% Signal (supersymmetry)… … and background )(GLAST AMS-02 pCR p+ → ISM p + p+ + p p + + + +pCR pISM →π → μ e → →π0 → γγ e+ → e − Another possible scenario: KK Dark Matter Lightest Kaluza-Klein Particle (LKP): B(1) Bosonic Dark Matter: fermionic final states no longer helicity suppressed. e+e- final states directly produced. As in the neutralino case there are 1-loop processes that produces monoenergetic γγin the final state. P Secondary production (upper and lower limits) Simon et al. ApJ 499 (1998) 250. from χχ Secondary annihilation production (Primary Bergström et production al. ApJ 526 m(c) = 964 (1999) 215 GeV) Ullio : astro- ph/9904086 AntiprotonAntiproton--ProtonProton RatioRatio Potgieter at al. arXiv:0804.0220v1 [astro-ph] WhatWhat dodo wewe needneed?? MeasurementsMeasurements atat higherhigher energiesenergies BetterBetter knowledgeknowledge ofof backgroundbackground HighHigh statisticsstatistics ContinuousContinuous monitoringmonitoring ofof solarsolar modulationmodulation LongLong DurationDuration FlightsFlights AntimatterAntimatter DarkDark MatterMatter SpaceSpace MissionsMissions PAMELA BESS 15-06-2006 2007 AMS-02 2009 PEBS-DbarSUSY 2011-2013 GAPS 2013 GammaGamma SpaceSpace ExperimentsExperiments AGILE 11-06-2008 23-04-2007 PAMELAPAMELA Payload for Antimatter Matter Exploration and Light Nuclei Astrophysics PAMELAPAMELA CollaborationCollaboration Italy: Bari Florence Frascati Naples Rome Trieste CNR, Florence Russia: Moscow St. Petersburg Germany: Sweden: Siegen KTH, Stockholm Pamela as a Space Observatory at 1AU Search for dark matter annihilation Search for antihelium (primordial antimatter) Search for new Matter in the Universe (Strangelets?) Study of cosmic-ray propagation Study of solar physics and solar modulation Study of terrestrial magnetosphere Study of high energy electron spectrum (local sources?) - + e- p e p (He,...) Trigger, ToF, dE/dx - + Sign of charge, rigidity, dE/dx Electron energy, dE/dx, lepton-hadron separation GF ~21.5 cm2sr Mass: 470 kg Size: 130x70x70 cm3 DesignDesign performanceperformance Energy range Antiproton flux 80 MeV - 190 GeV Positron flux 50 MeV – 270 GeV Electron/positron flux up to 2 TeV (from calorimeter) Electron flux up to 400 GeV Proton flux up to 700 GeV Light nuclei (up to Z=6) up to 200 GeV/n He/Be/C: -8 Antinuclei search Sensitivity of O(10 ) in He-bar/He • Unprecedented statistics and new energy range for cosmic ray physics • Simultaneous measurements of many species ResursResurs--DK1DK1 satellitesatellite Main task: multi-spectral remote sensing of earth’s surface Built by TsSKB Progress in Samara, Russia Lifetime >3 years (assisted) Data transmitted to ground via high-speed radio downlink PAMELA mounted inside a pressurized container Mass: 6.7 tonnes Height: 7.4 m Solar array area: 36 m2 PAMELAPAMELA LaunchLaunch 15/06/15/06/0606 16 Gigabytes trasmitted daily to Ground NTsOMZ Moscow OrbitOrbit CharacteristicsCharacteristics 350 km SAA 70ο 610 km • Low-earth elliptical orbit • 350 – 610 km • Quasi-polar (70o inclination) • Lifetime >3 years (assisted) PAMELA Orbit Outer radiation belt Download @orbit 3754 – 15/02/2007 07:35:00 MWT NP SP S1 S2 S3 95 min Inner EQ EQ radiation belt (SSA) orbit 3751 orbit 3752 orbit 3753 Flight data: 0.171 GV positron Flight data: 0.169 GV electron Flight data: 0.632 GeV/c antiproton annihilation Flight data: 84 GeV/c interacting antiproton Flight data: 92 GeV/c positron Flight data: 14.7 GV Interacting nucleus (Z = 8) PAMELAPAMELA StatusStatus TillTill 2nd2nd ofof MarchMarch 20082008 PAMELAPAMELA hashas collectedcollected ~~ 8.8TB8.8TB ofof data,data, correspondingcorresponding toto ~~ 10109 triggerstriggers AntiprotonAntiproton--ProtonProton RatioRatio preliminary AntiprotonAntiproton--ProtonProton RatioRatio preliminary Cirelli, Franceschini, Strumia arXiv:0802.3378v2 [hep-ph] PamelaPamela PositronsPositrons th TillTill AugustAugust 3030th aboutabout 2000020000 positronspositrons fromfrom 200200 MeVMeV upup toto 200200 GeVGeV havehave beenbeen analyzedanalyzed MoreMore thanthan 1500015000 positronspositrons overover 11 GeVGeV OtherOther eighteight monthsmonths datadata toto bebe analyzedanalyzed PositronPositron -- ElectronElectron ratioratio Pre lim in ary PAMELA PositronPositron -- ElectronElectron ratioratio PositronPositron -- ElectronElectron ratioratio Pre lim in ary PositronsPositrons withwith HEATHEAT Preliminary PositronsPositrons withwith HEATHEAT && PAMELAPAMELA ProblemsProblems 9 BackgroundBackground calculationcalculation 9 SolarSolar ModulationModulation atat lowlow energiesenergies 9 ChargeCharge--signsign dependencedependence ofof solarsolar modulationmodulation DiffusionDiffusion HaloHalo ModelModel SecondariesSecondaries // primariesprimaries i.e. Boron/ Carbon to constrain propagation parameters D. Maurin, F. Donato R. Taillet and P.Salati F. Donato et.al, ApJ, 563, 172, ApJ, 555, 585, 2001 [astro-ph/0101231] 2001 [astro-ph/0103150] B/C Ratio Antiproton flux Astrophysic B/C constraints Nuclear cross sections!! Preliminary B/CB/C ResultsResults PreliminaryPreliminary HeliumHelium andand HydrogenHydrogen IsotopesIsotopes SecondarySecondary toto PrimaryPrimary ratiosratios Flux (p/cm^2 sr s) Kinetic Energy (GeV) Proton flux July 2006 Preliminary !!! GalacticGalactic HH andand HeHe spectraspectra SolarSolar PhysicsPhysics withwith PAMELAPAMELA SolarSolar ModulationModulation ofof galacticgalactic cosmiccosmic raysrays Continuous monitoring Pamela AMS-01 of solar activity Caprice / Mass /TS93 BESS Study of charge sign dependent effects Asaoka Y. et al. 2002, Phys. Rev. Lett. 88, 051101), Bieber, J.W., et al. Physi- cal Review Letters, 84, 674, 1999. J. Clem et al. 30th ICRC 2007 AntiprotonAntiproton fluxesfluxes A range of minimal (R-parity conserving) SUSY predictions of Galactic antiprotons spectrum, with neutralino masses 45-700 GeV Annual Variation of P spectrum Annual Variation P flux (m-2sr-1s-1GeV-1) Proton fluxesatTOA Kinetic Energy (GeV) p/p ratio Time variation of p/p ratio at solar maximum Observed data by BESS Charge dependent model prediction(Bieber et al.) Bieber, J.W., et al. Phys. Rev. Letters, 84, 674, 1999. AntiprotonAntiproton--ProtonProton RatioRatio preliminary Preliminary !!! SpectraSpectra ProtonProton /c^ rGVs) GeV sr P/(cm^2 RED: JULY 2006 BLUE: AUGUST 2007 2 2 2 2 Primary spectrum FF =Eis ( − M) [( /φ) E+− M ] July 2006 497±2 January 2007 481±2 Φ = August 2007 441±2 PositronPositron FractionFraction Pre lim in ary Mirko Boezio, INFN Trieste - Fermilab, 2008/05/02 Pamela Clem at al. 30th ICRC 2007 ChargeCharge signsign dependencedependence ofof cosmiccosmic rayray modulationmodulation.. Two systematic deviations from reflection symmetry of the interplanetary magnetic field: 1) The Parker field has opposite magnetic polarity above and below the equator, but the spiral field lines themselves are mirror images of each other. This antisymmetry produces drift velocity fields that for positive particles converge on the heliospheric equator in the A+ state or diverge from it in A- state. Negatively charged particles behave in the opposite manner and the drift patterns interchange when the solar polarity diverge. 2) Systematic ordering of turbulent helicity can cause diffusion coefficients to depend directly on charge sign and polarity state. Bieber, J.W., et al. Phys. Rev. Letters, 84, 674, 1999. DecemberDecember 20062006 SolarSolar particleparticle eventsevents Dec 13th largest CME since 2003, anomalous at sol min December 13th 2006 event Preliminary! December 13th 2006 He differential spectrum Preliminary! December 14th 2006 event X-rayX-ray P,e-P,e- Low energy tail of Dec 13th event Arrival of event of Dec 14th MagneticMagneticFieldField NeutronNeutronMonitorMonitor Solar Quiet spectrum BelowEndgalactic of eventspectrum: of Dec 14th Start of Forbush decrease Decrease of primary spectrum Arrival of magnetic cloud from CME of Dec 13th Shock 1774km/s (gopalswamy, 2007) Decrease of Neutron Monitor Flux Preliminary! RadiationRadiation BeltsBelts SouthSouth AtlanticAtlantic AnomalyAnomaly SecondarySecondary productionproduction fromfrom CRCR interactioninteraction withwith atmosphereatmosphere PamelaPamela WorldWorld MapsMaps:: 350350 –– 650650 kmkm altalt 36 MeV p, 3.5 MeV e- PamelaPamela mapsmaps atat variousvarious altitudesaltitudes PRELIMINARY !!!! Altitude scanning PrimaryPrimary andand AlbedoAlbedo (sub(sub--cutoffcutoff measurements)measurements) OtherOther ObjectivesObjectives e rs e v i n U e h t f o UniverseUniverse n i g ri o e h t r o f SearchSearch forfor thethe existenceexistence ofof AntimatterAntimatter inin thetheh rc AMS a e S Accelerators PAMELAPAMELA AMSAMS inin SpaceSpace Search for the existence of anti Universe antimatter
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