CHARGED PARTICLE OBSERVATION from ‘SPACE’ European Astroparticle Physics Meeting Munich, November 23-25, 2005 M. Bourquin, University of Geneva

M. Bourquin November Advantage of space and balloon experiments Detectors are above the atmosphere : –Direct measurements of CR composition –Very precise measurements, using state-of the-art particle physics technology satellites and ISS ( cover the full sky when in Earth orbit) balloons (about 5 gr/cm 2 remaining)

M. Bourquin November Overview of experiments Experiments Presenting Analyzed Flight Data, Active Detectors TRACER, ATIC, BESS, TIGER, BETS, CPDS, MARIE Experiments Presenting Analyzed Flight Data, Passive Detectors RUNJOB, CAKE Experiments With Recent Data, Analysis Underway BESS-Polar, CREAM Experiments With Advanced Hardware PAMELA, AMS-02 New Experiments CALET, CREST, NUCLEON, INCA R. Streitmatter, 29th ICRC, 2005

M. Bourquin November Difficulties for Satellites and ISS: Schedule uncertainties linked to launch uncertainties Complex issues of space qualification and safety procedures: Limited weight, limited power, accelerations and vibrations, pressure change, limited data transfer, temperature changes, operation without human intervention for Long Duration Balloon Flights: weather conditions (e.g. at South Pole !)

M. Bourquin November Balloon-borne Experiment Superconducting Spectrometer - POLAR 8-day, 17 hour Antarctic flight, Dec BEFORE AFTER

M. Bourquin November Topics addressed by CR space experiments Indirect dark matter search (antiprotons, positrons, antideuterons) Understanding propagation processes (nuclei e.g. B, C, Fe) Search for primary antimatter (antinuclei) Search for new forms of matter (e.g. strangelets)

M. Bourquin November Cosmic Ray Fluxes

M. Bourquin November AMS-01 on STS-91 Shuttle Flight

M. Bourquin November AMS-01 Proton Spectra Above cutoff: cosmic rays Sub-cutoff: trapped particles Downward Upward

M. Bourquin November Helium in near Earth Orbit with AMS-01

M. Bourquin November Properties of next generation magnetic spectrometers R. Battiston, Rapporteur Talk on Direct Measurements and Origin of CR, ICRC,2003

M. Bourquin November ANTI Anticoncidence system Multiple particles rejection TRK Si Tracker + magnet Permanent magnet B=0.4T 6 planes double sided Si strips 300  m thick Spatial risolution ~3  m MDR = 1000 GV/c TOF Time-of-flight Level 1 trigger particle identification (up to 1GeV/c) dE/dx Plastic scintillator + PMT Time Resolution ~ 70 ps ANTI Anticoincidence system Defines tracker acceptance Plastic scintillator + PMT S4ND S4 and Neutron detectors Identify hadron interactions Plastic Scintillator 36 3 He counters in a polyetilen moderator PAMELA DETECTOR CALO Si-W Calorimeter Imaging Calorimeter : reconstructs shower profile discriminating e + /p and p/e - at level of ~ Energy Resolution for e ±  E/E = 15% / E 1/2. Si-X / W / Si-Y structure 22 W planes 16.3 X 0 / 0.6 l 0

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Pamela in Samara, Russia 4/09/05

M. Bourquin November The Satellite: Resurs DK1 -Soyuz-TM Launcher from Baikonur -Launch in Lifetime >3 years -PAMELA mounted inside a Pressurized Container, attached to Satellite -Earth-Observation- Satellite

M. Bourquin November R. Battiston, Rapporteur Talk on Direct Measurements and Origin of CR, ICRC,2003

M. Bourquin November BESS-Polar: Lower Energy, High Statistics Measurements to lower energy. Reduced geomagnetic influence Less material in particle path Long Duration Flight Technical flight Fall 2003 Antarctic flight Winter Antarctic Flight Winter More than double present p-bar statistics in first flight ~22 times present solar-minimum p-bar statistics in flight

M. Bourquin November Courtesy M. Buénerd

M. Bourquin November Calorimeter Preliminary Energy Deposit Distribution ~100 TeV incident energy Energy deposit gives a quick check of the energy spectrum It shows a reasonable power law with data extending well above 100 TeV

M. Bourquin November AMS-02 on the International Space Station

M. Bourquin November AMS-02 Detector TRD:e/p separation TOF: ß and |Z|, sign(Z) Star tracker: pointing Magnet: 0.8 T, sign(Z) Si tracker: p, |Z|, sign(Z) ACC: anticoincidence system RICH: ß and |Z|, sign(Z) ECAL: e/p separation

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M. Bourquin November Antiproton Production in the Galaxy Primary antiprotons could originate from the annihilation of the dark matter particles (Susy neutralinos) concealed inside the galactic halo. Secondary antiprotons are produced through the spallation of CR protons on the interstellar materiel. Spectrum peaks at about 2 GeV Presently antiprotons have very large propagation uncertainties, which has to be understood to search for effects due to primary antimatter.

M. Bourquin November Antiproton fluxes A M Lionetto, A Morselli and V Zdravkovic (2005)

M. Bourquin November Antiproton spectra: Pamela expectation for Diffuse and Convection model in 3 yr Antiproton spectra: PAMELA expectation for DC model A.Lionetto, A.Morselli, V.Zdravkovic, JCAP09(2005)010

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M. Bourquin November Dark matter search with antiprotons Secondary antiproton flux Distorsion by WIMP (examples with 964 GeV and 777 GeV neutralino, P. Ullio, astro-ph )

M. Bourquin November Positron spectra: PAMELA expectation for DC model DRB DC A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [ astro-ph/ ]

M. Bourquin November Dark matter search with positrons: AMS-02 Neutralinos induce a distortion of the spectrum Sensitivity after one year of data P. Maestro, based on models by Baltz and Edsjö

M. Bourquin November Description of CR propagation Diffusion models have several free parameters to be fixed by observations

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M. Bourquin November Be/ 9 Be – radioactive clock 10 Be (t 1/2 = 1.51 Myr) is the lightest radioactive secondary isotope having a half-life comparable with the CR confinement time in the Galaxy. In diffusion models, the ratio 10 Be/ 9 Be is sensitive to the size of the halo and to the properties of the local interstellar medium 1 year AMS will separate 10 Be from 9 Be for 0.15 GeV/n < E < 10 GeV/n after 3 years will collect  Be

M. Bourquin November Antimatter search - antihelium Pamela ( ) Bess Polar (20 days)

M. Bourquin November Search for New Particles AMS-01 reported an anomalous event (Z/A = 0.114), background probability < Compatible with a strangelet from a ‘color locked’ model. Ф ~ (m 2 sr sec) -1 Properties: AMS-02: statistics x 10 3

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M. Bourquin November Conclusions 1.The new space experiments are quite impressive detectors: Pamela, AMS-02, BESS, CREAM They will collect very precise data on charged CR. They are unavoidable for a full understanding of propagation processes to unravel new physics.

M. Bourquin November Propagation uncertainties still require multi- messenger observations Ex: Dark matter searches : importance of simultaneous measurements of Be prepared to compare results between CR experiments and gamma rays experiments and with LHC experiments!

M. Bourquin November Several Astroparticle experiments are ‘Recognized’ at CERN: RE1RE1(AMS) Alpha Magnetic Spectrometer (AMS) for Extraterrestrial Study of Antimatter, Matter and Missing Matter on the International Space Station RE3RE3(AUGER PROJECT) The Pierre Auger Observatory Project RE4RE4(L3+C) L3 + Cosmics Experiment RE5RE5(EXPLORER) The Gravitational Wave Detector EXPLORER RE6RE6(ANTARES) ANTARES: An Undersea Neutrino telescope RE7RE7(GLAST) GLAST RE8RE8(LISA) LISA RE9RE9(NESTOR) NESTOR-Neutrino Extended Submarine Telescope with Oceanographic Research RE2ARE2A(CAPRICE) Cosmic AntiParticle Ring Imaging Cerenkov Experiment RE2BRE2B(PAMELA) Search for Antimatter in Space 3. How make European teams more competitive and to reduce expenditures by pooling resources?

M. Bourquin November Create an European Astroparticle Centre at CERN ? It is planned to establish at CERN an AMS Payload Operations and Control Centre (POCC) and a Science Operations Centre (SOC)