1. PAMELA Payload for Antimatter Matter Exploration and Light Nuclei Astrophysics

2. PAMELA Collaboration Moscow St. Petersburg Russia: Sweden: KTH, Stockholm Germany: Siegen Italy: BariFlorenceFrascatiTriesteNaplesRome CNR, Florence

3. PAMELA detectors GF: 21.5 cm 2 sr Mass: 470 kg Size: 130x70x70 cm 3 Power Budget: 360W Spectrometer microstrip silicon tracking system + permanent magnet It provides: - Magnetic rigidity  R = pc/Ze - Charge sign - Charge value from dE/dx Time-Of-Flight plastic scintillators + PMT: - Trigger - Albedo rejection; - Mass identification up to 1 GeV; - Charge identification from dE/dX. Electromagnetic calorimeter W/Si sampling (16.3 X 0, 0.6 λI) - Discrimination e+ / p, anti-p / e - (shower topology) - Direct E measurement for e - Neutron detector 3 He tubes + polyethylene moderator: - High-energy e/h discrimination Main requirements  high-sensitivity antiparticle identification and precise momentum measure + -

4. Resurs-DK1: multi-spectral imaging of earth’s surface PAMELA mounted inside a pressurized container Lifetime >3 years (assisted, first time last February). Expected till end 2011. Data transmitted to NTsOMZ, Moscow via high-speed radio downlink. ~16 GB per day Quasi-polar and elliptical orbit (70.0°, 350 km - 600 km) Traverses the South Atlantic Anomaly Crosses the outer (electron) Van Allen belt at south pole Resurs-DK1 Mass: 6.7 tonnes Height: 7.4 m Solar array area: 36 m 2 350 km 610 km 70 o PAMELA SAA ~90 mins Resurs-DK1 satellite + orbit

5. Two independent energy measurements: Rigidity from Tracker -bremsstrahlung above tracker -decreasing energy resolution Energy from Calorimeter -sampling calorimeter -increasing energy resolution  possibility to cross-check the energy measurement Electron (e - ) flux, energy measurement Mirko Boezio, HEAD 2010, 2010/03/03

6. Analyzed data July 2006 – December 2008 (~850 days) Collected triggers >10 9 Identified ~ 5.5 10 5 electrons between 1 and 200 GeV Electron/positron identification: rigidity (R)  SPE |Z|=1 (dE/dx=MIP)  SPE&ToF  =1  ToF e-/e+ separation (charge sign)  SPE (e-/p-bar separation  CALO) ~ no background, issues: - spillover protons at high energy - spectrometer resolution - selection efficiencies S1 S2 CALO S4 CARD CAS CAT TOF SPE S3 ND Electron identification Mirko Boezio, HEAD 2010, 2010/03/03

7. PAMELA Electron (e - ) Spectrum Mirko Boezio, HEAD 2010, 2010/03/03

8. PAMELA Electron (e - ) Spectrum Mirko Boezio, HEAD 2010, 2010/03/03

9. Electron flux - break in the spectrum? Mirko Boezio, HEAD 2010, 2010/03/03 PAMELA Electron (e - ) Spectrum

10. Preliminary PAMELA Electron (e - ) Spectrum Mirko Boezio, HEAD 2010, 2010/03/03

11. Preliminary PAMELA Electron (e - ) Spectrum Mirko Boezio, HEAD 2010, 2010/03/03

12. PAMELA Electron (e - + e + ) Spectrum Mirko Boezio, HEAD 2010, 2010/03/03

13. Very Preliminary!!! PAMELA Electron (e - + e + ) Spectrum Mirko Boezio, HEAD 2010, 2010/03/03 Energy and electron identification based on calorimeter information only!

14. Positron to Electron Fraction In Nature article published data acquired till February 2008 New data reduction: data till end of 2008. With same approach of Nature paper ~30% increase in statistics better understanding of systematics. Secondary production Moskalenko & Strong 98 Adriani et al, arXiv:1001.3522 [astro-ph.HE]

15. Mirko Boezio, HEAD 2010, 2010/03/03 Preliminary Proton and Alpha Spectrum

16. Antiprotons Mirko Boezio, HEAD 2010, 2010/03/03 Errors might be underestimated, possible residual spillover-proton contamination Antiprotons in CRs are in agreement with secondary production Preliminary

17. Proton Spectrum Mirko Boezio, HEAD 2010, 2010/03/03

18. Summary  PAMELA has been in orbit and studying cosmic rays for ~42 months. >10 9 triggers registered and >18 TB of data has been down-linked.  e - spectrum up to ~200 GeV shows spectral features that may point to additional components. Analysis is ongoing to increase the statistics and expand the measurement of the e - spectrum up to ~500 GeV and e + spectrum up to ~300 GeV (all electrum (e - + e + ) spectrum up to ~1 TV).  High energy positron fraction (>10 GeV) increases significantly (and unexpectedly!) with energy. Primary source? Data at higher energies might help to resolve origin of rise (spillover limit ~300 GeV).  Antiproton-to-proton flux ratio and antiproton energy spectrum (~100 MeV - ~200 GeV) show no significant deviations from secondary production expectations. http://pamela.roma2.infn.it

19. Mirko Boezio, HEAD 2010, 2010/03/03