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CHARGED PARTICLE OBSERVATION from ‘SPACE’

CHARGED PARTICLE OBSERVATION from ‘SPACE’. European Astroparticle Physics Meeting Munich, November 23-25, 2005 M. Bourquin, University of Geneva. Advantage of space and balloon experiments. Detectors are above the atmosphere : Direct measurements of CR composition

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CHARGED PARTICLE OBSERVATION from ‘SPACE’

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

  2. 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/cm2 remaining) M. Bourquin November 2005

  3. Overview of experiments R. Streitmatter, 29th ICRC, 2005 • 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 M. Bourquin November 2005

  4. 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 2005

  5. Balloon-borne Experiment Superconducting Spectrometer - POLAR 8-day, 17 hour Antarctic flight, Dec. 2004 BEFORE AFTER M. Bourquin November 2005

  6. 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 2005

  7. Cosmic Ray Fluxes M. Bourquin November 2005

  8. AMS-01 on STS-91 Shuttle Flight M. Bourquin November 2005

  9. AMS-01 Proton Spectra Downward Upward Above cutoff: cosmic rays Sub-cutoff: trapped particles M. Bourquin November 2005

  10. Helium in near Earth Orbit with AMS-01 M. Bourquin November 2005

  11. Properties of next generation magnetic spectrometers R. Battiston, Rapporteur Talk on Direct Measurements and Origin of CR, ICRC,2003 M. Bourquin November 2005

  12. TOF Time-of-flight Level 1 trigger particle identification (up to 1GeV/c) dE/dx Plastic scintillator + PMT Time Resolution ~70 ps Anticoncidence system Multiple particles rejection ANTI TRK Anticoincidence system Defines trackeracceptance Plastic scintillator + PMT ANTI Si Tracker + magnet Permanent magnet B=0.4T 6 planes double sided Si strips 300 m thick Spatialrisolution ~3m MDR = 1000 GV/c Si-W Calorimeter ImagingCalorimeter : reconstructs shower profile discriminating e+/p and p/e- at level of ~ 10-5 Energy Resolution for e±E/E = 15% / E1/2. Si-X / W / Si-Y structure 22 W planes 16.3 X0 / 0.6 l0 CALO S4 and Neutron detectors Identify hadron interactions Plastic Scintillator 36 3He counters in a polyetilen moderator S4 ND PAMELA DETECTOR M. Bourquin November 2005

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  14. Pamela in Samara, Russia4/09/05

  15. The Satellite: Resurs DK1 • Soyuz-TM Launcher from Baikonur • Launch in 2005 • Lifetime >3 years • PAMELA mounted inside aPressurized Container, attached to Satellite • Earth-Observation- Satellite M. Bourquin November 2005

  16. R. Battiston, Rapporteur Talk on Direct Measurements and Origin of CR, ICRC,2003 M. Bourquin November 2005

  17. 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 2004-2005 • Antarctic Flight Winter 2007-2008 • More than double present p-bar statistics in first flight • ~22 times present solar-minimum p-bar statistics in 2007-2008 flight M. Bourquin November 2005

  18. Courtesy M. Buénerd M. Bourquin November 2005

  19. 0 CalorimeterPreliminary 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 2005

  20. AMS-02 on the International Space Station M. Bourquin November 2005

  21. 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 M. Bourquin November 2005

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  26. 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 2005

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

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

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  30. Dark matter search with antiprotons Distorsion by WIMP (examples with 964 GeV and 777 GeV neutralino, P. Ullio, astro-ph 9904086) Secondary antiproton flux M. Bourquin November 2005

  31. Positron spectra: PAMELA expectation for DC model DRB DC A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [astro-ph/0502406] M. Bourquin November 2005

  32. Dark matter search with positrons: AMS-02 Neutralinos induce a distortion of the spectrum Sensitivity after one year of dataP. Maestro, based on models by Baltz and Edsjö M. Bourquin November 2005

  33. Description of CR propagation Diffusion models have several free parameters to be fixed by observations M. Bourquin November 2005

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  35. 1 year 10Be/9Be – radioactive clock 10Be (t1/2 = 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 10Be/9Be is sensitive to the size of the halo and to the properties of the local interstellar medium AMS will separate 10Be from 9Be for 0.15 GeV/n < E < 10 GeV/n after 3 years will collect 10510Be M. Bourquin November 2005

  36. Antimatter search - antihelium Pamela (2004-2007) Bess Polar (20 days) M. Bourquin November 2005

  37. Search for New Particles AMS-01 reported an anomalous event (Z/A = 0.114), background probability < 10-3 Compatible with a strangelet from a ‘color locked’ model. Ф ~ 10-5 (m2 sr sec)-1 AMS-02: statistics x 103 Properties: M. Bourquin November 2005

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  39. Conclusions • 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 2005

  40. 2. 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 2005

  41. 3. How make European teams more competitive and to reduce expenditures by pooling resources? Several Astroparticle experiments are ‘Recognized’ at CERN: RE1(AMS) Alpha Magnetic Spectrometer (AMS) for Extraterrestrial Study of Antimatter, Matter and Missing Matter on the International Space Station RE3(AUGER PROJECT) The Pierre Auger Observatory Project RE4(L3+C) L3 + Cosmics Experiment RE5(EXPLORER) The Gravitational Wave Detector EXPLORER RE6(ANTARES) ANTARES: An Undersea Neutrino telescope RE7(GLAST) GLAST RE8(LISA) LISA RE9(NESTOR) NESTOR-Neutrino Extended Submarine Telescope with Oceanographic Research RE2A(CAPRICE) Cosmic AntiParticle Ring Imaging Cerenkov Experiment RE2B(PAMELA) Search for Antimatter in Space M. Bourquin November 2005

  42. It is planned to establish at CERN an AMS Payload Operations and Control Centre (POCC) and a Science Operations Centre (SOC) Create an European Astroparticle Centre at CERN ? M. Bourquin November 2005

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