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AMS-02 and the Great Questions

AMS-02 and the Great Questions The experiment and the main tasks: looking for Antimatter, Strangelets and Dark Matter. Nicolò Masi Bologna University and INFN. May 9 2012. Matter. An Improved Version of AMS-01. Anti-Matter. Antimatter. Astrophysics , Dark Matter.

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AMS-02 and the Great Questions

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  1. AMS-02 and the Great Questions The experiment and the main tasks: looking for Antimatter, Strangeletsand Dark Matter NicolòMasiBologna University and INFN May 9 2012

  2. Matter An Improved Version of AMS-01 Anti-Matter Antimatter Astrophysics, Dark Matter The TOF system provides: - the fast trigger to the whole AMS; - the measurement of the time of flight (Δt– better than 180 ps), for the determination of the particle velocity (β), with a resolution of few %; - the distinction from upward and downward going particles at a level of 10-9 necessary to distinguish between matter and antimatter; - the measurement of the absolute particle charge up to Z =15.

  3. Lower TOF pre-integration(CERN, Geneva, Switzerland)

  4. AMS at Cape Kennedy 2011 Launches Date: May 8-9 Mission: STS-134 LaunchVehicle: Space Shuttle Endeavour Launch Site: Kennedy Space Center - Launch Pad 39° STS-134 Description: Space shuttle Endeavourwilldeliver an EXPRESS Logistics Carrier-3 (ELC-3) and the Alpha MagneticSpectrometer (AMS-02) to the ISS ESA Astronaut: Roberto Vittori

  5. Go baby go!

  6. And physics begins

  7. AMS-02 and the Antiworld:Islands of Antimatter? The CPT theorem assures that any particle species there exists the antiparticle with exactly the same mass and decay width and eventually opposite charges. This striking symmetry would naturally lead us to conclude that the Universe contains particles and antiparticles in equal number densities. The observed Universe is drastically different. • 100 MeV g flux excludes wide antimatter regions up 100 Mpc • Sakharov’s 3 Principles of Baryogenesis ….. • … but alternative models predict distant antimatter local domains • A single anti-He CR nucleus represents a strong evidence for Antimatter Domains in our Universe

  8. Expected Goal for Antinuclei Search Antihelium/HeliumFlux 10 years

  9. Cosmic Rays

  10. New Physics: Strangelets

  11. From quark stars 10 years

  12. Dark Matter Program(TOF Group)

  13. Dark matter: • is inferred to exist since 1934 from gravitational effects on visible matter and background radiation, undetectable by emitted or scattered em radiation. According to observations of structures larger than galaxies, as well as Big Bang cosmology interpreted under the Friedmann equations and the FRW metric, DM accounts for 23% of the mass-energy density of the observable universe. Ordinary matter accounts for only 4.6%. • Local Evidences: • Galactic Rotation Curves • Dynamics of Galaxy Clusters • X-Ray Cluster Emission • Strong Gravitational Lensing • Anomalous CosmicRayFluxes • Cosmological Evidences: • CMB AcousticPeacks (from WMAP and PLANCK) • StructureFormation and Evolution

  14. Non barionic DM candidates • WIMP (Weakly Interacting Massive Particles): Qem=0, QS =0, stable (𝛕 > 1/H0), 𝝆relic compatible (𝜴 ≲ 0.3), which can only interact via weak or gravitational force, preferablyminimal (scalar or Majorana-like), foundamental, cold (non relativistic) • Lightest supersymmetric particles (LSP). Neutralino𝝌 WIMP Mass Region: 100 GeV÷10 TeV Indirect detection with AMS -products of the annihilation of DM particles: the signal can consists of photons, neutrinos and antimatter (positrons, antiprotons and antideuterons)

  15. PAMELA results on the Cosmic-Ray Antiproton Flux No Dark Matter Signal! Clear Signal!

  16. Primary CR Positron from Dark Matter

  17. And alsoHigh Energy Hadrons Total Flux High Energy SUSY Wino, Little Higgs, Kaluza-Klein Theory, Right-handed Neutrino, PBH, Singlet Scalar, Minimal DM, Technicolor… Antiproton High Energy Signal from KK particle

  18. Facenda… Wehave 1 year data @ CNAF = 15 billionsparticles = a lot of fun! Kinetic Energy (GeV)

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