1. WiZard PAMELA WiZard PAMELA Piergiorgio Picozza Commissione II INFN Cascina, 7 Aprile 2009

2. PAMELA Status Today 1028 days in flight Today 1028 days in flight data taking ~73% live-time data taking ~73% live-time ~13 TBytes of raw data downlinked ~13 TBytes of raw data downlinked >10 9 triggers recorded and under analysis >10 9 triggers recorded and under analysis

3. Main Results Antiprotons to protons ratio Antiprotons to protons ratio Positrons to all electrons ratio Positrons to all electrons ratio Protons Spectrum Protons Spectrum Nuclei Ratio Nuclei Ratio Solar Modulation Solar Modulation Solar flares Solar flares Radiation Belts Radiation Belts

4. Antiprotons PRL 102, 051101, 2009 PRL 102, 051101, 2009 Selected Viewpoints in “Physics” Selected Viewpoints in “Physics” 86 citazioni TOP 50+ 86 citazioni TOP 50+

5. Antiproton to proton ratio PRL 102, 051101 (2009) Seconday Production Models

6. Antiproton to proton ratio PRL 102, 051101 (2009)

7. Antiproton Flux Preliminary statistical errors only energy in the spectrometer

8. Mirko Boezio, SLAC Seminar, 2009/01/12 Antiproton Flux Preliminary statistical errors only energy in the spectrometer Secondary production: F. Donato et al., 536 (2001) 172 Secondary production: V. S. Ptuskin et al, ApJ 642 (2006) 902 Preliminary

9. Positrons Nature 458, 697, 2009 Nature 458, 697, 2009 156 citazioni 156 citazioni TOP 100+ TOP 100+ Oltre 100 articoli di interpretazione Oltre 100 articoli di interpretazione

10. Positrons to all electrons ratio Secondary production Moskalenko & Strong 98

11. Positron to Electron Ratio astro-ph 0810.4995 End 2007: ~10 000 e + > 1.5 GeV ~2000 > 5 GeV

12. Interpretation

13. 0808.3725 DM 0808.3867 DM 0809.2409 DM 0810.2784 Pulsar 0810.4846 DM / pulsar 0810.5292 DM 0810.5344 DM 0810.5167 DM 0810.5304 DM 0810.5397 DM 0810.5557 DM 0810.4147 DM 0811.0250 DM 0811.0477 DM During first week after PAMELA results posted on arXiv )

14. Secondary production Moskalenko & Strong 98 Pulsar Component Atoyan et al. 95 Pulsar Component Zhang & Cheng 01 Pulsar Component Yüksel et al. 08 KKDM (mass 300 GeV) Hooper & Profumo 07 PAMELA Positron Fraction

15. DM annihilations DM particles are stable. They can annihilate in pairs. Primary annihilation channels Decay Final states σ= σ a =

16. DM annihilations Resulting spectrum for positrons and antiprotons M= 1 TeV The flux shape is completely determined by: 1) WIMP mass 2) Annihilations channels

17. Data fitting Which DM spectra can fit the data? DM with and dominant annihilation channel (possible candidate: Wino)‏ positrons antiprotons Yes! No!

18. Data fitting Which DM spectra can fit the data? DM with and dominant annihilation channel (no “natural” SUSY candidate)‏ positrons antiprotons Yes! But B≈10 4 No!

19. Data fitting DM with and dominant annihilation channel positrons antiprotons Yes!

20. Model independent results Which DM spectra can fit the data? Fit of PAMELA positrons (only)‏ Lepton channels (e,μ,...) favored but also W

21. Model independent results Which DM spectra can fit the data? Fit of PAMELA positrons+antiprotons Annihilations into quarks, gauge and Higgs bosons hardly constrained and

22. Example: e + & p DM P. Grajek et al., arXiv: 0812.4555v1 See Gordon Kane’s talk

24. Astrophysical Explanation Pulsars S. Profumo Astro-ph 0812-4457 Mechanism: the spinning B of the pulsar strips e - that accelerated at the polar cap or at the outer gap emit γ that make production of e ± that are trapped in the cloud, further accelerated and later released at τ ~ 10 5 years. Mechanism: the spinning B of the pulsar strips e - that accelerated at the polar cap or at the outer gap emit γ that make production of e ± that are trapped in the cloud, further accelerated and later released at τ ~ 10 5 years. Young (T ~10 5 years) and nearby (< 1kpc) Young (T ~10 5 years) and nearby (< 1kpc) If not: too much diffusion, low energy, too low flux. If not: too much diffusion, low energy, too low flux. Geminga: 157 parsecs from Earth and 370,000 years old Geminga: 157 parsecs from Earth and 370,000 years old B0656+14: 290 parsecs from Earth and 110,000 years old B0656+14: 290 parsecs from Earth and 110,000 years old Many others after Fermi/GLAST Many others after Fermi/GLAST Diffuse mature pulsars Diffuse mature pulsars

25. Mirko Boezio, LHC & DM Workshop, 2009/01/06 Example: pulsars H. Yüksak et al., arXiv:0810.2784v2 Contributions of e- & e+ from Geminga assuming different distance, age and energetic of the pulsar Hooper, Blasi, and Serpico arXiv:0810.1527

26. Only secondaries? P. Serpico hep-ph 0810.4846 Anomalous primary electron source spectrum Anomalous primary electron source spectrum Spectral feature in the proton flux responsible for secondaries Spectral feature in the proton flux responsible for secondaries Role of Helium nuclei in secondary production Role of Helium nuclei in secondary production Difference between local and ISM spectrum of protons Difference between local and ISM spectrum of protons Anomalous energy-dependent behaviour of the diffusion coefficient Anomalous energy-dependent behaviour of the diffusion coefficient Rising cross section at high energies Rising cross section at high energies High energy beaviour of the e + /e - High energy beaviour of the e + /e -

27. Diffusion Halo Model

28. Standard Positron Fraction Theoretical Uncertainties T. Delahaye et al., arXiv: 0809.5268v3 γ = 3.54γ = 3.34

29. Explanation with supernovae remnants Shaviz and al. astro-ph.HE 0902.0376

30. PAMELA Proton Spectrum

31. Galactic H and He spectra Preliminary !!!

33. Secondary nuclei B nuclei of secondary origin: CNO + ISM  B + … Local secondary/primary ratio sensitive to average amount of traversed matter (l esc ) from the source to the solar system Local secondary abundance:  study of galactic CR propagation (B/C used for tuning of propagation models) LBM Preliminary

34. Antiproton to proton ratio PRL 102, 051101 (2009)

35. Positron Fraction

36. Solar Modulation of galactic cosmic rays BESS Caprice / Mass /TS93 AMS-01 Pamela Study of charge sign dependent effects Asaoka Y. et al. 2002, Phys. Rev. Lett. 88, 051101), Bieber, J.W., et al. Physi-cal Review Letters, 84, 674, 1999. J. Clem et al. 30th ICRC 2007 U.W. Langner, M.S. Potgieter, Advances in Space Research 34 (2004)

37. Solar modulation Interstellar spectrum July 2006 August 2007 February 2008 Decreasing solar activity Increasing GCR flux sun-spot number Ground neutron monitor PAMELA (statistical errors only)

38. A > 0 Positive particles A < 0 p, e + p, e - -

39. A > 0 Positive particles A < 0 ¯ + ¯ + Pamela 2006 (Preliminary!) Charge dependent solar modulation

40. Solar Physics with PAMELA

41. December 2006 Solar particle events Dec 13 th largest CME since 2003, anomalous at sol min

42. December 13th 2006 event Preliminary!

43. December 13th 2006 He differential spectrum December 13th 2006 He differential spectrum

44. December 14th 2006 event Preliminary! Solar Quiet spectrum Low energy tail of Dec 13th event Below galactic spectrum: Start of Forbush decrease Magnetic Field Neutron Monitor X-ray P,e- Decrease of primary spectrum Arrival of magnetic cloud from CME of Dec 13th Shock 1774km/s (gopalswamy, 2007) Decrease of Neutron Monitor Flux Magnetic Field Neutron Monitor X-ray P,e- Arrival of event of Dec 14th End of event of Dec 14th

45. Radiation Belts South Atlantic Anomaly Secondary production from CR interaction with atmosphere

46. SAA SAA morphology Latitude Altitude Longitude Neutron rate (background) South-Atlantic Anomaly (SAA)

47. Grigorov, Sov. Phys. Dokl. 22, 305 1977 NINA ApJ Supp.132 365, 2001 AMS Phys. Lett. B 472 2000.215, Phys. Lett. B 484 2000.10–22 Lipari, Astrop. Ph. 14, 171, 2000 Huang et al, Pys Rev. D 68, 053008 2003 Sanuki et al, Phys Rev D75 043005 2007 Honda et al, Phys Rev D75 043006 2007  Atmospheric neutrino contribution  Astronaut dose on board International Space Station  Indirect measurement of cross section in the atmosphere nell’atmosfera  Agile e Glast background estimation --- M. Honda, 2008 Proton flux at various cutoffs

48. Proton spectrum in SAA, polar and equatorial regions

49. Stato e Futuro di PAMELA

50. Satellite Satellite Funzionante per almeno altri 3 anni data bassa attività solare primi tre anni Satellite Funzionante per almeno altri 3 anni data bassa attività solare primi tre anni Rimessa in orbita senza toccare PAMELA Rimessa in orbita senza toccare PAMELA Piccoli problemi con le batterie. Possibilità di perdita di un 10% massimo tempo vivo Piccoli problemi con le batterie. Possibilità di perdita di un 10% massimo tempo vivo

51. Apparato PAMELA Report completo ai referee Report completo ai referee Problemi ad un fototubo TOF e ad un piano calorimetro Problemi ad un fototubo TOF e ad un piano calorimetro Efficienza attuale tracciatore ~ 65% stabile da alcuni mesi. Efficienza attuale tracciatore ~ 65% stabile da alcuni mesi.

52. Prolungamento Rapporto pbar/p fino a 200 GeV Rapporto pbar/p fino a 200 GeV Rapporto e/(e - +e + ) fino a 300 Gev Rapporto e + /(e - +e + ) fino a 300 Gev Spettro e + fino a 300 GeV Spettro e + fino a 300 GeV Spettro e - fino a 700 GeV (1 TeV) Spettro e - fino a 700 GeV (1 TeV)

53. Positron selection with calorimeter e-e-e-e- Fraction of charge released along the calorimeter track (left, hit, right) p e+e+e+e+ + Energy-momentum match Starting point of shower Longitudinal profile Rigidity: 20-30 GV

54. e + background estimation from data + Energy-momentum match Starting point of shower e-e- ‘presampler’ p Rigidity: 20-28 GV e+e+ p

55. Prolungamento Rapporti secondari-primari +60% Rapporti secondari-primari +60% Modulazione solare: estremamente importante seguirla nel tempo. Modulazione solare: estremamente importante seguirla nel tempo. Flares solari: segni di ripartenza dell’attività solare. Unico strumento in volo per energie al GeV e superiori. Flares solari: segni di ripartenza dell’attività solare. Unico strumento in volo per energie al GeV e superiori.

56. Prolungamento Studio delle sistematiche Studio delle sistematiche Intercalibrazione con AMS Intercalibrazione con AMS

57. Addendum n. 6 accordo INFN-Roscosmos Accordo solo con INFN, ente non spaziale. Accordo solo con INFN, ente non spaziale. Nessuna interferenza con costi ESA, NASA, ASI stabiliti da convenzioni tipo spaziale Nessuna interferenza con costi ESA, NASA, ASI stabiliti da convenzioni tipo spaziale Non rinegoziazione a costi e potenza Russia attuali Non rinegoziazione a costi e potenza Russia attuali

58. Addendum Agreement n. 6 To the Agreement between Roscosmos and INFN On Joint Implementation of the ”PAMELA” Mission (RIM-2 experiment of the “Russian-Italian Mission” program)

59. Addendum n. 6 Federal Space Agency (ROSCOCMOS) Federal Space Agency (ROSCOCMOS) The Federal Space Agency, reformed from Russian Aviation-Space Agency in compliance with decree # 314 from March, 09, 2004 by President of Russia Federation, being its assigner, represented by Prof. Yu. I. Nosenko, Director Deputy, The Federal Space Agency, reformed from Russian Aviation-Space Agency in compliance with decree # 314 from March, 09, 2004 by President of Russia Federation, being its assigner, represented by Prof. Yu. I. Nosenko, Director Deputy, on one side, on one side, and and The National Institute of Nuclear Physics (INFN) National Executive Institute, involved in fundamental research in the field of nuclear physics and elementary particle physics, represented by the President, Prof. R. Petronzio The National Institute of Nuclear Physics (INFN) National Executive Institute, involved in fundamental research in the field of nuclear physics and elementary particle physics, represented by the President, Prof. R. Petronzio on the other side on the other side noting the successful work of the scientific instrument “PAMELA” on board of the spacecraft “RESURS DK1”, the effective joint activity of Russian and Italian scientists in making quick analysis and diagnostics and in planning the experiment, as well as the first results on antiparticle fluxes study (antiprotons and positrons) in galactic cosmic rays, being of great significance in the field of fundamental cosmology, high energy physics, cosmic ray physics, results on study of cosmic rays fluxes in the near-Earth space, significant for applied physics; noting the successful work of the scientific instrument “PAMELA” on board of the spacecraft “RESURS DK1”, the effective joint activity of Russian and Italian scientists in making quick analysis and diagnostics and in planning the experiment, as well as the first results on antiparticle fluxes study (antiprotons and positrons) in galactic cosmic rays, being of great significance in the field of fundamental cosmology, high energy physics, cosmic ray physics, results on study of cosmic rays fluxes in the near-Earth space, significant for applied physics; considering great interest of parties in prolongation of measurements considering great interest of parties in prolongation of measurements

60. Addendum n. n6 the Parties have agreed about the following: to extend the conditions of Addendum Agreements n. 4 and n. 5 till December, 31 2011. ROSCOSMOS will provide control and operation of the scientific instrument “PAMELA”, acquisition and transfer of “PAMELA” data of volume 14Gbytes/day. INFN will pay for mentioned work 410000 € per year.

61. Costi 200 k€ per quota mantenimento satellite 200 k€ per quota mantenimento satellite 210k€ per 14 (16 in pratica) Gigabytes giornalieri 210k€ per 14 (16 in pratica) Gigabytes giornalieri Ricordo che 60k€ sono già a carico della commissione. Ricordo che 60k€ sono già a carico della commissione.

62. PAMELA Physics Workshop May 11-12, 2009 ROMA Auditorium Via Rieti http:// pamela.roma2.infn.it /workshop09 http:// pamela.roma2.infn.it /workshop09