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The Pamela experiment ready for flight

The Pamela experiment ready for flight. Oscar Adriani – INFN Firenze, Università di Firenze on behalf of the Pamela collaboration P ayload for A ntimatter M atter E xploration and L ight Nuclei A strophysics. Russia :. Italy :. CNR, Florence. Bari. Florence. Frascati. Naples. Rome.

larissa-keith
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The Pamela experiment ready for flight

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  1. The Pamela experiment ready for flight Oscar Adriani – INFN Firenze, Università di Firenze on behalf of the Pamela collaboration Payload for Antimatter Matter Exploration and Light NucleiAstrophysics The Pamela experiment ready for flight O. Adriani

  2. Russia: Italy: CNR, Florence Bari Florence Frascati Naples Rome Trieste USA: GSFC India: NMSU Mumbai Sweden: Germany: Siegen KTH, Stockholm Moscow St. Petersburg The Pamela experiment ready for flight O. Adriani

  3. Study antiparticles in cosmic rays • Search for antimatter • Search for dark matter • Study cosmic-ray propagation • Study solar physics and solar modulation • Study the electron spectrum (local sources?) Pamela’s scientific objectives The Pamela experiment ready for flight O. Adriani

  4. Antiproton flux 80 MeV - 190 GeV Positron flux 50 MeV – 270 GeV Electron flux up to 800 GeV Proton flux up to 1000 GeV Electron/positron flux up to 2 TeV Light nuclei (up to Z=6) up to 500 GeV/n Light isotopes (D, 3He) up to 1 GeV/n Antinuclei search (sensitivity better than 10-7 in He/He) PAMELA Capabilities • Long-term monitoring of the solar modulation of cosmic rays • Energetic particles from the Sun (e+) • High-energy particles in the Earth magnetosphere The Pamela experiment ready for flight O. Adriani

  5. Antiprotons Propagation / Dark Matter Extragalactic primordials Black holes / Dark Matter Unexplored Region Secondary production (CAPRICE94-based) Bergström et al. Secondary production (upper and lower limits) Simon et al. Primary production  annihilation (m() = 964 GeV, Ullio 2002) PAMELAenergy range The Pamela experiment ready for flight O. Adriani

  6. Positrons Propagation / Dark Matter Charge modulation effects Unexplored Region Secondary production ‘Moskalenko + Strong model’ (1998) without reacceleration Secondary production ‘Leaky box model’ (Protheroe 1982) PAMELAenergy range Primary production annihilation (m() = 336 GeV Baltz & Edsjö 1999) The Pamela experiment ready for flight O. Adriani

  7. Antiprotons Secondary production (CAPRICE94-based) Bergström et al. Primary production  annihilation (m() = 964 GeV) Secondary production (upper and lower limits) Simon et al. > 3.104 antiprotons 80 MeV/c - 190 GeV/c The Pamela experiment ready for flight O. Adriani

  8. Positrons Secondary production ‘Moskalenko + Strong model’ (1998) without reacceleration Secondary production ‘Leaky box model’ (Protheroe 1982) Primary production annihilation m() = 336 GeV > 3.105 positrons 50 MeV/c - 270 GeV/c The Pamela experiment ready for flight O. Adriani

  9. Cosmic-ray Antimatter Search He / He CR production ~O(10-14) The Pamela experiment ready for flight O. Adriani

  10. Expected Fluxes in 3 Years • ‘Semi-Polar’ orbit (700)  Low energy particles • Wide energy range + 3 years mission  Reliable measurements The Pamela experiment ready for flight O. Adriani

  11. Launch date: June 14-16, 2006 Satellite and orbit Resurs DK1 • Earth observation • 350 / 610 km • Inclination = 70.4o • Soyuz 2 launcher • Baikonur Cosmodrome • 3 year mission Pamela operational • Housed in an atmospheric pressure vessel • Temperature = 5oC ÷ 35oC • All subsystems must withstand launch vibrations! • Electronics must withstand up to ~3 krad During launch / orbital manoeuvres 350 - 610 km • Total mass ~ 470kg / 345W power budget The Pamela experiment ready for flight O. Adriani

  12. The PAMELA subdetectors 1.2 m Mass ~450 kg Power ~360 W Geometrical Factor ~20.5 cm2sr The Pamela experiment ready for flight O. Adriani

  13. Magnetic spectrometer (I) • Si Tracker + magnet • Rigidity measurement • 5 Nd-B-Fe magnet segments • 0.48T at the centre • (13.2 x 16.2 cm2) x 44.5 cm high • 6 planes of 300mm thick double sided Si detectors • <3mm resolution in bending view • +/-10 MIP dynamic range (VA1 chips) The Pamela experiment ready for flight O. Adriani

  14. Magnetic spectrometer (II) Multiple scattering Nx & sx MDR ~ 1 TV/c Momentum resolution 2003  Last beam-test of PAMELA flight model @ CERN-SPS 40-150 GeV/c protons The Pamela experiment ready for flight O. Adriani

  15. Calorimeter (I) • Si-W Calorimeter • Measures energies of e±. • DE/E = 15% / E1/2 + 5% • Si-X / W / Si-Y structure. • 22 Si / 21 W  16X0 / 0.9l0 • Imaging: EM - vs- hadronic discrimination, longitudinal and transverse shower profile • Total number of channels 4224 • Wide dynamic range  1 - 1000 MIP • Calorimeter Requirements: • p/e+ selection eff.  90% • p rejection factor  105 • e- rejection factor  104 The Pamela experiment ready for flight O. Adriani

  16. Calorimeter (II)Electron-Proton Separation SPS Test Beam Data: p & e- 200 GeV/c The Pamela experiment ready for flight O. Adriani

  17. Calorimeter (III) Electron identification efficiency Test Beam Simulation Proton contamination in the electron sample Test Beam Simulation SPS Test Beam Data (p&e- up to 200 GeV) + Simulation At 200 GeV: Proton rejection factor  2.3∙105 Electron selection efficiency  90% The Pamela experiment ready for flight O. Adriani

  18. Trigger/Time of Flight (I) • Plastic scintillator + PMT • Trigger • Detection of albedo particles • Particle identification (up to 1 GeV/c) • dE/dx The Pamela experiment ready for flight O. Adriani

  19. C12 200 MeV/n Δβ ~ 0.009 Trigger/Time of Flight (II) Results from heavy ions beam test at GSI (2006) Time Resolution Charge Resolution Δ(Z=6)~0.26 The Pamela experiment ready for flight O. Adriani

  20. Auxiliary detectors (I) • Anticoincidence system • Defines acceptance for tracks • Plastic scintillator + PMT The Pamela experiment ready for flight O. Adriani

  21. Auxiliary detectors (II) Neutron Counter Shower Scintillator (S4) • Plastic scintillator: 482 mm x 482 mm x 10 mm • 6 PMT read-out • Dynamic range: 1 - 1000 MIP • 2 x 18 3He proportional counters (polyethylene / Cd envelope) • 600 × 550 × 150 mm3 • n + 3He  p + 3H + 765 keV • O(10) more n in hadronic cascades than EM The Pamela experiment ready for flight O. Adriani

  22. Trigger and Data Rate • Level 1 Trigger • TOF Scintillator Coincidence • S1 x S2 x S3 • S2 x S3 • 12 Hz (G.F. = 20.5 cm2sr + background) • Calorimeter Self-trigger (Ee>0.3TeV) • 10 mHz (G.F. = 600 cm2sr) One orbit Data Rate / Storage / Downlink 12 Hz x 5 kByte / event ~ 5 GB/day Up to 20 GB daily on-board Down-linked with a few ground connections per day [PAMELA DAQ ~10% dead-time (10 ms)] The Pamela experiment ready for flight O. Adriani

  23. PAMELA Status (≤2005) Detectors tested at PS / SPS Test facilities as Prototypes and in FM configuration Mass/Thermal Models Qualified, March-May 2003 PAMELA Technological Model completed and delivered to Russia December 2003 Full Cycle of Vibration /Shock of the Flight Model passed at IABG/ Munich, January 2005 PAMELA Flight Model delivered to TSSKB_Progress Factory in Samara (Russia) April 2005 The Pamela experiment ready for flight O. Adriani

  24. Preliminary! Preliminary! • Preliminary results: • no efficiency correction • first-order alignment • no ETA p.f.a. On-ground muon results 2005  acquisition of atmospheric particles during PAMELA test before delivering  Check of spectrometer systematics with positive and negative muons The Pamela experiment ready for flight O. Adriani

  25. PAMELA Event Ground Data Muon: 2.8 GV The Pamela experiment ready for flight O. Adriani

  26. PAMELA Event Ground Data Hadron: 6.6 GV The Pamela experiment ready for flight O. Adriani

  27. PAMELA Event Calorimeter Self Trigger GF  400 cm2 sr The Pamela experiment ready for flight O. Adriani

  28. PAMELA Status (≥2005) • Pamela has been fully qualified in Samara • from May, 2005 up to March, 2006 • Cooling loop • Mechanical interfaces • Power supply tests • Interface with the Very High Speed Radiolink (VRL) • Electrical tests • Many repeated tests have been done during 1 year • Pamela was accepted to be sent to the launch base (March 2006) The Pamela experiment ready for flight O. Adriani

  29. PAMELA Status (2006) (I) • Pamela was transported by airplane from Samara to Bajkonour on March 28, 2006 • 60 days work before launch • Standalone tests • Insertion in the pressurized container • Electrical tests with the satellite • Test of the downlink The Pamela experiment ready for flight O. Adriani

  30. The Pamela experiment ready for flight O. Adriani

  31. The Pamela experiment ready for flight O. Adriani

  32. The Pamela experiment ready for flight O. Adriani

  33. The Pamela experiment ready for flight O. Adriani

  34. PAMELA Status (2006) (II) All the tests were successful (May 18, 2006) Pamela is ‘ready for flight’ Launch window: 14-16 June 2006 Next steps: 4 days after the launch 1 switch on (nominal way – hot parts) for 4 hours data downlink check of data in NTSOMZ receiving station 6 days after the launch: start of commissioning phase hot parts (6 days) cold parts (3 days) +test of various operating modes 17 days after the launch beginning of physics data taking The Pamela experiment ready for flight O. Adriani

  35. PAMELA is the first space experiment which will measure Antiprotons and Positrons to high energies (≥ 200GeV) with an unprecedented statistical precision • PAMELA will set a new lower limit for finding Antihelium • PAMELA will look for Dark Matter candidates • PAMELA has collected ground cosmic-rays for various months at the laboratories of Rome 2 University and at the Samara TSSKB-Progress factory • All detectors are performing as designed and PAMELA seems able to achieve its scientific goals. • Pamela has been delivered to Russia at the end of March 2005 • PAMELA has successfully passed all the integrations tests with the Resurs-DK1 Satellite at TSSKB-Progress factory in Samara • Pamela has been delivered to Bajkonour at the end of March 2006 • PAMELA has successfully passed all the integrations tests with the Resurs-DK1 Satellite at the launch base in Bajkonour and is ‘ready for flight’ • PAMELA will be launched in the 14-16 June 2006 time window Conclusions The Pamela experiment ready for flight O. Adriani

  36. The Pamela experiment ready for flight O. Adriani

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