1. Summary of Experimental Results keV(10 3 )-ZeV(10 21 ) Narayana Bhat University of Alabama in Huntsville The field of Extensive Air Showers and its potential The field of Extensive Air Showers and its potential Complexity of Instrumentation and uncertainties involved Complexity of Instrumentation and uncertainties involved Particle Densities Particle Densities Muons Muons Radio Measurements Radio Measurements Timing Measurements Timing Measurements Challenges in interpretation. Challenges in interpretation. Conversion of Particle density to shower size using an assumed LD Conversion of Particle density to shower size using an assumed LD Conversion of Timing measurements into Shower Direction Conversion of Timing measurements into Shower Direction Using Hadronic/Electromagnetic Interaction Models to infer the primary energies Using Hadronic/Electromagnetic Interaction Models to infer the primary energies Using secondary measurements to infer the primary species – protons, heavy nuclei, Gamma-rays Using secondary measurements to infer the primary species – protons, heavy nuclei, Gamma-rays Future Promises. Future Promises.

2. Physics with EAS Gamma-ray astronomy  large field of view (~2  sr)  duty cycle  100%  energy threshold: few hundreds of GeV  Limitations  Limited to primarily to galactic sources because of the opacity of space  GRB Counter-parts  Monitoring AGNs   -hadron separation is challenging  Need good direction info  Energy dependent angular resolution. Cosmic ray physics Proton-air cross section measurement  Anti-p /p ratio at energy  TeV with the Moon shadow  Spectrum and composition up to  10 3 TeV and higher  Anisotropy  Limitations  HE Interaction parameters need to be extrapolated.  Many systematics involved  Need to measure as many shower parameters as possible Fundamental Physics

3. Major Facilities (currently operating)  Fermi Satellite Mission (Space)  HESS, MAGIC, VERITAS, HAGAR  ARGOS-YBJ  GRAPES-3  KASCADE – Grande  MILAGRO  Pierre Auger  Tibet AS And the their respective future avatars

4. Cosmic Ray Spectrum

5. The proton-air cross section Extending the energy range with the analog readout Phys. Rev. D 80, 092004 (2009) WAPP 2010P. Camarri

7. The all-particle energy spectrum KASCADE Grande DATA

9. Mass Composition

10. N ch /N  distributions E. Cantoni DATA

11. KASCADE-Grande has collected high quality data in the region 10 16 – 10 18 eV region which will be the basis to look for the iron knee and the galactic- extragalactic transition in the cosmic ray spectrum Recent results of Kascade-Grande regarding the all-particle energy spectrum:  Agreement with KASCADE & EAS-TOP results at the threshold  Agreement between different reconstruction approaches  No single power law  Structures at the threshold and around 10 17 eV  Medium or heavy composition is preferred assuming QGSjetII model

15. Cosmic Ray Anisotropy

16. First Results from KASCADE-Grande (ICRC 2007) Large Scale Anisotropy

17. WAPP 2010P. Camarri17 Proton median energy  2 TeV ARGO-YBJ Heliotail Geminga Galactic Plane ~6 ·10 -4 ~4 ·10 -4 Proton median energy  10 TeV MILAGRO Multiple explanations were proposed: Salvati & Sacco, A&A 485 (2008) 527 Drury & Aharonian, Astrop. Phys. 29 (2008) 420. K. Munakata,AIP Conf Proc Vol 932, page 283 Salvati, A&A 513 (2010) A28 Lazarian & Desiati (2010)

22. Ground based  -ray Astronomy

23. Full DAQ TEST data Ground based  -ray Astronomy Mrk421 flaring activity Ground based g-ray Astronomy Ground based g-ray Astronomy SWIFT X-rays (15-50 keV) FLARES July 2006June 2008Feb 2010 ARGO test data ARGO Full DAQ

24. Porter & Protheroe J. Phys. G 23 (1997) 1765 Tateyama & Nishimura ICRC 4 (2003) 2285 Berezinsky, et al. Astropart. Phys. 1 (1993) 281 Inner Galactic Plane (12 < l < 81 deg., |b| < 2 deg.) Integral Flux : Inner Galaxy

25. 25 Integral Flux : Outer Galaxy 10 -4 10 -5 10 -6 10 -7 10 -8 10 -9 10 -10 10 -11 10 -12 10 -13 10 -14 10 -15 10- 16 1 10 10 2 10 3 10 4 10 5 10 6 (90%C.L.) Outer Galactic Plane (165 < l < 234 deg., |b| < 2 deg.)

26. MGRO J1908+06 confirmed by HESS (2009) Extension  0.34 deg HESS spectrum: dN/dE = 4.14 10 -12 E -2.1 sec -1 cm -2 TeV -1 ( Aharonian et al., 2009) Inside the nebula FERMI detected a pulsar with period 106.6 ms MILAGRO HESS Milagro spectrum: dN/dE = 6.2 10 -12 E -1.5 exp(-E/14.1) sec -1 cm -2 TeV -1 (Smith et al., 2009)

27. Crab Nebula still a standard candle ? HST

28. Multiwavelenght Crab Nebula SED Meyer, Horns, Zechlin 2010

29. Crab Nebula 19-26 September Chance probability: p = 6.6 10 -5 N hit > 40 8 days 46 observation hours Significance 4.8  Expected 1.0  from steady flux

30. Assumption: power law spectra with indexes ranging from the value measured by satellites to 2.5 (only this latter case is considered for Cutoff Power Law spectra) GRB Counter-parts Fluence upper limits in the 1  100 GeV range for GRBs with known redshift 99% c.l.

31. Jordan Goodman – University of Maryland Fall 2010 In 2007, Milagro reported our Galactic plane survey based on data collected up to June 2006. Detected 4 sources at >5σ post-trials. Detected 4 candidate sources at >4.5σ pre- trials. ~100,000 trials in Galactic plane, 500,000 in the sky.

32. Jordan Goodman – University of Maryland July 2009 Summary of Spectral Results  All of the brightest Milagro sources are spatially coincident with Fermi Pulsars (PWN). Fits to the Crab/Mrk 421/MGRO J1908+06 are compatible with IACT observations. Fits to the Crab/Mrk 421/MGRO J1908+06 are compatible with IACT observations. Insufficient significance/resolution to distinguish a soft spectra from hard spectra that cut off Insufficient significance/resolution to distinguish a soft spectra from hard spectra that cut off A cutoff is favored in all sources if the TeV scale if the spectrum is assumed to be hard (2.1). A cutoff is favored in all sources if the TeV scale if the spectrum is assumed to be hard (2.1).

33. Solar wind and IMF radial velocity at emission v r + run rotation Archimedean spiral EARTH x y … so a charged particle that passes through the IMF experiences a B y that changes once or twice from positive to negative (two- or four-sector structure). Consenquently the sun shadow will be seen oscillating once or twice along the north-south direction in a solar rotation period, or Carrington period. Carrington period using Sun shadow displacement

34. Future of Cosmic Ray Research

35. JEM-EUSO Observational Principle JEM-EUSO telescope observes fluorescence and Cherenkov photons generated by air showers created by extreme energetic cosmic rays JEM-EUSO is a new type of observatory on board the International Space Station (ISS), which observes transient luminous phenomena occurring in the earth's atmosphere. The telescope has a super wide field-of- view(60) and a large diameter(2.5m). JEM-EUSO mission aims to initiate particle astronomy at ~10 20 eV. Extreme Energetic Cosmic Rays Air shower A giant natural TPC (500km) 3 to observe EECRs

36. End-to-End Simulations (ESAF): Signal for a p shower (60 deg, 10 20 eV) Mernik et al., 2009

37. Exposure Evolution

38. Science Objectives  Main Objective ： Astronomy and astrophysics through particle channel with extreme energies –Possible identification of the particle and energy sources based on the analysis of the arrival direction –Possible identification of the acceleration and radiation mechanisms with the measurement of energy spectrum from individual sources  Exploratory objective ： –Measurement of extreme energy gamma rays –Detection of extreme energy neutrinos –Estimation of the structure of galactic magnetic field and its intensity –Identification of relativity and quantum gravitational effect –Study of atmospheric luminous phenomena

39. Fall 2010 The HAWC ( High Altitude Water Cherenkov) Observatory

40. HAWC Science Objectives  Discover the origin of cosmic rays by measuring gamma-ray spectra to 100 TeV –Hadronic sources have unbroken spectra beyond 30-100 TeV –Galactic diffuse gamma rays probe the distant cosmic ray flux  Understand particle acceleration in astrophysical jets with wide field of view, high duty factor observations. –Trigger Multi-Messenger/Multi-Wavelength Observations of Flaring Active Galactic Nuclei (including TeV orphan flares) –Detect Short and Long Gamma-Ray Bursts  Explore new physics via HAWC’s unbiased survey of ½ the sky. –Increase understanding of TeV sources to search for new physics. –Study the local TeV cosmic rays and their anisotropy.