1. Andrii Neronov JEM-EUSOJEM-EUSO

2. Problem of the origin of cosmic rays Galactic Extragalactic?

3. Problem of the origin of cosmic rays 8 kpc Cosmic rays with energies below 10 18 eV spread through the Galaxy in a diffusive way, scattering at magnetic field inhomogeneities.

4. Problem of the origin of cosmic rays Deflected/randomized in the Solar system Deflected/randomized in the Solar system Deflected/randomized by the Galactic magnetic fields Deflected/randomized by the Galactic magnetic fields Cosmic ray "astronomy" window Cosmic ray "astronomy" window F~3 UHECR/10 3 km 2 /yr

5. Existing statistics of UHECR events ( ~50 events) is not sufficient for identification of sources via clustering analysis. Order-of-magnitude increase of statistics is needed for a sensible source search. Search for the sources of UHECR Pierre Auger Collab. '07

6. A=π(H tg(Θ/2)) 2 ≈(400 km) 2 Extreme Universe Space Observatory at the Japanese Experiment Module (JEM-EUSO) of the International Space Station is a next-generation UHECR experiment, which will detect fluorescence light from UHECR induced air showers from space ( 400 km altitude) over Θ=60 o field of view. Wide FoV shower imaging telescope in space

7. http://www.nlsa.com/ All-sky exposure Observation of UHECR events from the ISS has an advantage of homogeneous all-sky exposure, which is important for the statistical analysis of clustering pattern of UHECR events on the sky.

8. Time of launch: FY2016-2017 Current status: JAXA: System Requirements Review (SRR) starts in May 2011; ESA: included in the ELIPS/ISS program of ESA in 2010; NASA: APRA proposal, decision by Sept. 2012. RosCosmos: russian participation approved by STEC committee end of 2011, now in the process of approval by the head of the RosCosmos. Operation Period: 3 years (+ 2 years) Launching Rocket : H2B Transportation to ISS: un-pressurized Carrier of H2 Transfer Vehicle (HTV) Site to Attach: JEM Exposure Facility #2 Mass: 1983 kg Power: 926 W (operative), 352 W (non-operative) Data Transfer Rate:285 kpbs Mission parameters HTV launch September 11, 2009

9. The telescope Fresnel lens system Focal surface instrumentation: 2×10 5 pixels (MAPMT)+HV+trigger/readout electronics

10. 4 Proton E=10 20 eV,  =60º UHECR data Air fluorescence emission Air-scattered Cherenkov emission Cherenkov "ground-mark"

11. Clear sky Low altitude Optically thick cloud High altitude Sirrus cloud UHECR data Use of the atmosphere as cosmic ray detector requires precise knowledge of the state of the detector, i.e. knowledge of the real-time atmospheric conditions.

12. Clear sky Low altitude Optically thick cloud High altitude Sirrus cloud UHECR data Use of the atmosphere as cosmic ray detector requires precise knowledge of the state of the detector, i.e. knowledge of the real-time atmospheric conditions. JEM-EUSO Atmospheric Monitoring System

13. Clear sky Low altitude Optically thick cloud High altitude Sirrus cloud Use of the atmosphere as cosmic ray detector requires precise knowledge of the state of the detector, i.e. knowledge of the real-time atmospheric conditions. JEM-EUSO Atmospheric Monitoring System Swiss / UniGE involvement in JEM-EUSO Science Data Centre for the mission

14. Toward solution of the problem of the origin of UHECR 2012 2022 +Exploratory objectives: Detection of UHE gamma-rays Detection of UHE neutrinos Study of Galactic and intergalactic magnetic field Verification of Relativity, search for Quantum Gravity effects Global observations of transient atmospheric phenomena: plasma discharges and lightning.

15. UHE neutrinos UHE neutrinos produce deep-penetrating or up-going air showers readily distinguishable from UHECR showers. JEM-EUSO measurements will either detect the "cosmogenic" neutrinos from UHECR interactions or constrain cosmological evolution of UHECR sources (cut-off energy, slope of z evolution). Gorham et al. 2010 Berezinsky et al. 2010

16. CL No. of events UHE gamma-rays JEM-EUSO will measure depth of the shower maximum X max with precision of 120 g/cm 2 on event-by-event basis, sufficient to discriminate photons from nuclei. Auger SD JEM-EUSO, ideal JEM-EUSO, systematic In the absence of systematics, non-detection of photon-like events puts an upper bound on the photon fraction at the level of ~10 -3 at E~10 20 eV. Hooper et al. 2010 Systematic errors on X max reduce the sensitivity to photon fraction down to ~10 -2 at 10 20 eV, much better than the current Auger upper bound. Detection of GZK photons within the lifetime of JEM-EUSO is possible.