1. Direct measurements of cosmic rays in space ROBERTA SPARVOLI ROME “TOR VERGATA” UNIVERSITY AND INFN, ITALY Vulcano Workshop 2014 Vulcano Island (Italy), 23° May 2014

2. Galactic cosmic rays: open questions

3. Main physics research lines

4. Balloon experiments (CREAM, ATIC, BESS- Polar, TRACER, TIGER, …) Satellite experiments (PAMELA, FERMI, Gamma-400, …) ISS experiments (AMS, Calet, ISS-Cream, …) Existing platforms

5. Balloon experiments

6. Long Duration Balloons (LDB)

7. Science goals

8. Advanced Thin Ionization Calorimeter (ATIC)

9. ATIC instrument

11. TRACER detector

13. CREAM flights

14. CREAM instrument

15. GCR energy spectra

16. Proton and helium spectra

17. Boron to Carbon ratio

19. TIGER instrument

20. GCR source abundances

21. Cosmic ray electrons

22. Antiproton flux: BESS-Polar

23. Antiproton spectrum

24. Search for antihelium

25. Satellite experiments

26. PAMELA Payload for Matter/antimatter Exploration and Light- nuclei Astrophysics Direct detection of CRs in space Main focus on antiparticles (antiprotons and positrons) Launch from Baykonur PAMELA on board of Russian satellite Resurs DK1 Orbital parameters: - inclination ~70 o (  low energy) - altitude ~ 360-600 km (elliptical) - active life >3 years (  high statistics)  Launched on 15th June 2006  PAMELA in continuous data-taking mode since then!

27. PAMELA published results Antiproton flux + antiproton/proton ratio (100 MeV-200 GeV) Positron flux + positron/electron ratio (100 MeV-200 GeV) Electron flux (1 – 500 GeV) Proton and helium flux (1 GeV – 1.2 TeV) B/C ratio (500 MeV – 100 GeV) H and He isotope flux AntiHe/He Proton flux vs. time – solar modulation Trapped antiproton flux SEP data

28. Antiproton flux Antiproton/proton ratio Positron Fraction Positron flux No evidence for antiproton increase Strong evidence for positron increase

29. Electron flux P and He flux B/C ratio Strong evidence for spectral break

30. All particles PAMELA results Results span 4 decades in energy and 13 in fluxes

31. FERMI OBSERVATORY

33. FERMI all Electron Spectrum A. Abdo et al., Phys.Rev.Lett. 102 (2009) 181101 M. Ackermann et al., Phys. Rev. D 82, 092004 (2010) Found an excess in the all-electron spectrum, but no ATIC feature

34. Fermi Positron Fraction Confirmation of PAMELA positron excess

35. PAMELA & Fermi electron (e - ) spectra Adriani et al., Phys. Rev. Lett. 106, 201101 (2011) Ackermann et al., Phys. Rev. Lett. 108, 011103 (2012)

36. ISS experiments

37. AMS ALPHA MAGNETIC SPECTROMETER  Search for primordial anti-matter  Indirect search of dark matter  High precision measurement of the energetic spectra and composition of CR from GeV to TeV AMS-01: 1998 (10 days) - PRECURSOR FLIGHT ON THE SHUTTLE AMS-02: Since May 19 th, 2011, safely on the ISS. Four days after the Endeavour launch, that took place on Monday May 16th, the experiment has been installed on the ISS and then activated. and then activated. COMPLETE CONFIGURATION FOR >10 YEARS LIFETIME ON THE ISS

38. The AMS-02 detector

39. Positron fraction M. Aguilar et al, PRL 110, 2013 Further confirmation of positron excess

40. AMS preliminary data (ICRC 2013) Good agreement with PAMELA data beyond solar modulation

41. Direct measurements: electron spectrum e + + e - e-e-

42. Direct measurements: Positron flux increasing !

43. AMS preliminary data (ICRC 2013)

44. Apparent conflict with PAMELA (and CREAM, ATIC) data. No hint for break in spectral shape.

45. Direct measurements: P and He: Some “tension”

46. Excellent agreement PAMELA-BESS Proton flux Proton flux x E^2.7

47. Direct  indirect measurements

48. Direct and indirect measurements are starting to meet at 10^14 eV. Direct measurements aim at reaching the “knee”. This would be very important to test and calibrate hadronic interaction models.

49. Future experiments

50. CALET CREST DAMPE GAMMA-400 GAPS The future

51. CALET: launch in 2014-2015

52. ISS-CREAM: launch in 2014-2015

53. DAMPE: launch in 2015 DAMPE: Dark Matter Particle Explorer. Project of Chinese Academy of Sciences, in collaboration with ItalY (INFN) and the University of Geneva for the construction of the tracker Si. Precursor of HERD.

54. Gamma-400: launch in 2018 Approved Russian Space Mission With international cooperation

55. CREST: Cosmic Ray Electron Synchrotron Telescope (E> 2 TeV) One flight completed (2011/2012  10 days): analysis in progress

56. The GAPS experiment A balloon-borne detector ready to flight in 2017/2018

57. Conclusions High energy line Some conflict in the current data: H and He spectra harden with energy (>230 GV) ? H and He spectra are different ? Hi-Z spectra do not show similar hardening Energy dependance of propagation still undecided Composition line Source matter must be a composition of old ISM with newly synthetized matherial, in percentage 80%-20% (sites of acceleration rich in massive stars?)

58. Antimatter line Positrons show enhancement in the E>10 GeV region (new e+ e- source. Correlated to previous?) All electron spectrum shows enhancement at high energy (hundreds GeV). Correlated to previous? No antiproton excess observed both at low and high energy (several DM models and exotics ruled out) No heavier anti-nucleus observed (very stringent limits) Conclusions The new instruments poised to come on line such as CALET, ISS-CREAM, DAMPE, Gamma-400 and GAPS, as well as space instruments continuing to operate and new balloon flights of existing instruments, promise a robust future for cosmic ray research.