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Antiproton and Electron Measurements and Dark Matter Searches

Antiproton and Electron Measurements and Dark Matter Searches. Piergiorgio Picozza INFN and University of Rome Tor Vergata 8th International Workshop on Identification of Dark Matter 26-30 July 2010, Montpellier, France. THE UNIVERSE ENERGY BUDGET. DM annihilations.

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Antiproton and Electron Measurements and Dark Matter Searches

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  1. Antiproton and Electron Measurementsand Dark Matter Searches Piergiorgio Picozza INFN and University of Rome Tor Vergata 8th International Workshop on Identification of Dark Matter 26-30 July 2010, Montpellier, France

  2. THE UNIVERSE ENERGY BUDGET

  3. DM annihilations DM particles are stable. They can annihilate in pairs. Primary annihilation channels Final states Decay σa= <σv>

  4. e-

  5. Robert L. Golden

  6. Antimatter Search Wizard Collaboration • MASS – 1,2 (89,91) • TrampSI (93) • CAPRICE (94, 97, 98) • BESS (93, 95, 97, 98, 2000) • Heat (94, 95, 2000) • IMAX (96) • BESS LDF (2004, 2007) • AMS-01 (1998)

  7. Charge-dependent solar modulation Solar polarity reversal 1999/2000 Asaoka Y. Et al. 2002 Positron excess? ? ? ¯ + CR + ISM  p-bar + … kinematic threshold: 5.6 GeV for the reaction Cosmic Ray Antimatter Pre-PAMELA status Antiprotons Positrons Moskalenko & Strong 1998 CR + ISM  p± + x m± + x e±+x CR + ISM  p0 + x gge±

  8. PAMELA 15-06-2006 AMS-02 2010-2011 BESS 12-2007 Fermi/GLAST 11-6-2008 ATIC 2002 - 2007 Antimatter and Dark Matter Space Missions

  9. PAMELA Payload for Antimatter Matter Exploration and Light NucleiAstrophysics

  10. PAMELA Instrument

  11. PAMELALaunch15/06/0616 Gigabytes trasmitted daily to GroundNTsOMZ Moscow

  12. Antiprotons

  13. Antiproton Flux(0.06 GeV - 180 GeV) Donato et al. (ApJ 563 (2001) 172) Systematics errors included Ptuskin et al. (ApJ 642 (2006) 902) Adriani et al., astro-ph 1007.0821 PRL in press

  14. Antiproton to proton ratio (0.06 GeV - 180 GeV) Simon et al. (ApJ 499 (1998) 250) Ptuskin et al. (ApJ 642 (2006) 902) Donato et al. (PRL 102 (2009) 071301) Systematics errors included Adriani et al., astro-ph 1007.0821 PRL in press

  15. Time Dependence of PAMELA Proton Flux Preliminary

  16. Antiproton to proton ratioDark Matter constraints I. Cholis astro-ph :1007.1160v1.

  17. Antiproton to proton ratio Di Bernardo et al. astro-ph 0909.4548v3

  18. Wino Dark Matter in a non-thermal UniverseG. Kane, R. Lu, and S. WatsonarXiv:0906.4765v3 [astro-ph.HE)

  19. SAA Trappedpbar • PAMELA GCR • PAMELA

  20. BESS-Polar II Launch - December 22, 2007

  21. Rigidity measurement SC Solenoid (L=1m, B=1T) Min. material (4.7g/cm2) Uniform field Large acceptance Central tracker (Drift chamber d ~200mm Z, m measurement R,b --> m = ZeR 1/b2-1 dE/dx --> Z BESS Detector JET/IDC Rigidity TOF b, dE/dx √

  22. BESS Polar II Observations/Expectations • Event rate ~2.5 kHz; Total events ~4.7 x 109 • Total data volume 13.5 TB (3.07 kB/event) • Expected antiprotons ~10,000 10-20 times previous Solar minimum dataset ECRS? Antiproton Antideuteron Antihelium (Search for PBH) (Search for PBH) (Search for Antimatter)

  23. Positrons

  24. Positron to Electron Fraction Secondary production Moskalenko & Strong 98 Adriani et al, Astropart. Phys. 34 (2010) 1 arXiv:1001.3522 [astro-ph.HE]

  25. Time Dependence of PAMELA Electron (e-) Flux Preliminary

  26. Charge dependent solar modulation A > 0 Positive particles A < 0 Preliminary!! Pamela 2006

  27. A Challenging Puzzle for CR Physics • Uncertainties on: • Secondary production (primary fluxes, cross section) • Propagation models • Electron spectrum But antiprotons in CRs are in agreement with secondary production

  28. A Challenging Puzzle for CR Physics P.Blasi, PRL 103 (2009) 051104; arXiv:0903.2794 Y. Fujita arxiv .0904.5298 Positrons (and electrons) produced as secondaries in the sources (e.g. SNR) where CRs are accelerated. But also other secondaries are produced: significant increase expected in the p/p and B/C ratios. D. Hooper, P. Blasi, and P. Serpico, JCAP 0901:025,2009; arXiv:0810.1527 Contribution from diffuse mature &nearby young pulsars. I. Cholis et al., Phys. Rev. D 80 (2009) 123518; arXiv:0811.3641v1 Contribution from DM annihilation.

  29. Electrons

  30. Electron (e-) Spectrum Preliminary Preliminary

  31. Talk William Gillard

  32. All electronse+ + e-

  33. Courtesy of Luca Baldini

  34. All electron spectrum GLAST ATIC HESS

  35. Preliminary Preliminary ATIC 1 ATIC 2 ATIC 4 ATIC 1+2+4 ATIC 1+2 All three ATIC flights are consistent “Source on/source off” significance of bump for ATIC1+2 is about 3.8 sigma • J Chang et al.Nature456, 362 (2008) ATIC-4 with 10 BGO layers has improved e , p separation. (~4x lower background) “Bump” is seen in all three flights. Significance for ATIC1+2+4 is 5.1 sigma

  36. Example: DM I. Cholis et al. arXiv:0811.3641v1 I. Cholis et al. arXiv:0811.3641v1 See Neal Weiner’s talk

  37. Fermi (e++ e-)

  38. Electrons measured with H.E.S.S.

  39. Fermi (e++ e-) and PAMELA ratioBergstrom et al. astro-ph 0905.0333v1

  40. Pulsars: Most significant contribution to high-energy CRE:Nearby (d < 1 kpc) and Mature (104 < T/yr < 106) PulsarsD. Grasso et al. • Example of fit to both Fermi and Pamela data with known (ATNF catalogue) nearby, mature pulsars and with a single, nominal choice for the e+/e- injection parameters

  41. Fermi (e++ e-)D. Grassoastro-ph0912.3887

  42. All electronsPAMELA very preliminary

  43. TRD Tracker MAGNET Vacuum Case He Vessel RICH AMS-02 on ISS In Orbit Nov. 2010 – Feb. 2011

  44. The Completed AMS Detector on ISS Transition Radiation Detector (TRD) Time of Flight Detector (TOF) Magnet Silicon Tracker Ring Image Cerenkov Counter (RICH) Electromagnetic Calorimeter (ECAL) Size: 3m x 3m x 3m Weight: 7 tons

  45. AMS-02 new configuration

  46. Unique Feature of AMS positrons antiprotons Combining searches in different channels could give (much) higher sensitiviy to SUSY DM signals anti deuterons gamma rays

  47. The Next Future

  48. Future

  49. Perspectives

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