Kosice, April 13, 2011

1. JEM-EUSO in Poland Jacek Szabelski Cosmic Ray Laboratory The Andrzej Sołtan Institute for Nuclear Studies Łódź http: //ipj.u.lodz.pl Kosice, April 13, 2011

2. JEM-EUSOJEM – Japan Experiment ModuleEUSO – Extreme Universe Space Observatory Main scientific target: Measurements of ultra high energy cosmic rays (UHE CR) Japan – 62 USA – 27 France – 19 Germany – 25 Italy – 46 Mexico - 11 Korea – 15 Russia – 6 Switzerland – 6 Spain – 11 Poland - 13 Slovakia – 4 Bulgaria - 7 http: //jemeuso.riken.jp plan to launch at 2016

3. Cosmic rays Astrophysics (primary cosmic rays): energetic stable particles energetic – non-thermal energy distribution energy range up to about 1e20 eV (is there a limit ?) stable particles: protons, nuclei, electrons, gammas, neutrinos, anti-protons, positrons Secondary cosmic rays: secondary energetic particles in atmosphere generated by primary cosmic rays coherent events: EAS (extensive air showers) cascades of gammas, electrons/positrons, muons and hadrons muons

4. Cosmic rays: main scientific problems/questions Cosmic ray sources: • Astrophysical sources • Physical/astrophysical mechanism of acceleration High energy interaction properties (physics at energies above accelerator energies) Ultra high energy cosmic rays studies • Measurements of energy spectrum • Measurements of primary particle masses • Measurements of direction of the events • (search for point-like sources, • isotropy/anisotropy) • Measurements of temporal variations

5. Cosmic ray energy spectrum Direct measurements on balloons and satellites up to 1e15eV (limited by: exposure, energy estimation ) Knee Above 1e14 eV EAS measurements (problems with: mass determination energy estimation) Ankle LHC beam

6. How to accelerate particles ? at CERN now: 3.5·1012 eV from 2013 (?): 7.0·1012 eV JEM-EUSO would measure one particle with 7·1019 eV per day The nature provides particles 107 times more energetic than CERN

7. ground level observations of EAS (extensive air showers) Particles in EAS: photons (10 x Ne) electrons + positron (Ne) muons (0.1 x Ne) hadrons (0.01 x Ne) neutrinos EAS particles goes with a speed nearly c – light speed in vacuum (i.e. might be faster than light in the atmosphere) animation: T.Wibig typical EAS last about 30 microseconds (e.g. 10 km/c)

8. EAS Arrays for 1015 – 1018 eV KASCADE FzKarlsruhe KASCADE-Grande

9. PAO – Pierre Auger Observatory (South hemisphere) FD & SA measurements Expected 25 EAS/ year (E > 5.5 1019eV) FD – only during clear dark nights 3000 km2 FD – fluorescence detectors SA – surface array 7000 km2 sr yr (θ<60°)

10. Auger North 20500 km2 Northern hemisphere ECR > 3 1019eV Expected 175 EAS/ year (E > 5.5 1019eV) Starts 2011/2012 J.L.Harton, 31st ICRC

11. Auger North 20500 km2 Northern hemisphere ECR > 3 1019eV Expected 175 EAS/ year (E > 5.5 1019eV) Starts 2011/2012 J.L.Harton, 31st ICRC

12. EAS longitudinal development vs. ground observation levels VR – Volcano Ranch Ya – Yakutsk PAO – P.Auger Observatory Figure shows an average Ne distribution; In real EAS development • fluctuates • depends on primary particle mass • interpretation depends • on the interaction models EAS array observations at constant but zenith angle dependent depth (EAS development stage)

13. The GZK Effect Greisen (1966) and, independently Zatsepin & Kuz’min (1966) Kenneth Greisen George Zatsepin Vadim Kuz'min CMB p + n -resonance multi-pion production +

14. Energy spectrum: problems at the highest energies Existence of GZK effect Test of Lorentz transformation range of CR < 50 Mpc (ECR > EGZK)

15. Anisotropy / “sources” problems POA: 27 events with ECR > 4 1019eV Wibig + Wolfendale: mass of CR from „source” CEN-A ~ A=12 (i.e. no protons, no iron nuclei)

16. Larger exposure (statistics) is needed to enable experimental solution • Measurements of energy spectrum (GZK cut-off) • Measurements of primary particle masses • (sources and GZK cut-off) • Measurements of direction of the events • (search for point-like sources, • isotropy/anisotropy) Observations from space !!

17. ISS – altitude about 400 km JEM-EUSO: fast camera 400 000 frames per second to measure events lasting about 30 μs EAS neutrino shower particles excite N2, N2 emits UV light

18. JEM-EUSO Telescope on ISS Vertical Mode Tilted Mode Larger effective area (×5) with ~35°tilt

19. JEM-EUSO observation areas (nadir and tilt)

20. Comparison of exposures

21. Optical system

22. Fresnel lens

23. Optical system – diameter about 2.4 m

24. Mutli-anode photomultipliers arrangement in FS FC – Focal Surface = 137 PDM PDM – Photo-Detector Module = 36 MAPMT MAMPT – multi-anode photomultiplier = 64 pixels 1 pixel = 500m x 500m at ground level

25. Photomultiplier (PMT) Multianode photomultiplier (MAPMT) photon → photo-electron →106 electrons (anode) M36 36 anodes MAMPT new MAPMT – M64 – 64 anodes (pixels)

26. Background • Reflection from sky • (Moon, stars, planets) • Man made light (cities) • Lightnings • Meteorites etc. background estimation (per PMT): 25 millions p-e per second camera if very fast: GTU – gate time unit = 2.5 microsec background: 1 p-e per pixel per GTU

27. JEM-EUSO – Polish hardware contribution: 900V DC-DC suppliers for photomultipliers Standard load due to light background: about 70 p-e per GTU per PMT GTU – gate time unit = 2.5 microsec HV suppliers: Cockcroft-Walton and with transformer Input power: 30-50 mW/PDM (preliminary) (400 times smaller than for standard solution)

28. TLE – Transient Luminous Events

30. TLE – transient luminous events discharges to outer atmosphere Such events last 0.5 – 100 millisec (1 millisec = 400 GTU) are extremely long and bright for JEM-EUSO detectors Polish group from Space Research Center and Slovak group from Space Physics Center would collaborate on TLEs

34. Neutrino Shower K. Bittermann, KC-Tü Movie real time: 1/30000 of second

35. Simulations assuming that AGNs are CR sources 3000 events E > 5 1019eV 1000 events E > 7 1019eV particle astronomy ?

36. JEM-EUSO status (March/April 2011) Japan: • Accepted for further preparation to lunch in 2016 by JAXA • Rocket is under development • Transportation module is under development • No government decision Europe (8 countries): • Approved by ESA Programme Board for Human Spaceflights, Microgravity and Exploration, • Selected for inclusion in ELIPS research pool (ELIPS – European Programme for Life and Physical sciences and applications utilising the International Space Station), • Positively reviewed by EAS Astronomy Working Group (AWG) • JEM-EUSO is strongly supported by the ESA-appointed Fundamental Physics Roadmap Advisory Team (FPR-AT) in the document “A Roadmap for Fundamental Physics in Space (July, 26, 2010) USA/NASA: Formal talks are in progress ISS status • Formally accepted till 2015 • Recommendation to continue at least until 2020 • No decision sign on government level (USA, Japan, Europe-ESA)

37. JEM-EUSO in Poland The formal status: Letter of Invitation from RIKEN addressed to: T.Batsch, Jkarczmarczyk, B.Szabelska, J.Szabelski (as Polish coordinator), T.Wibig – IPJ T.Tymieniecka – Podlasie University J.Błęcki, P.Orleański, H.Rothkaehl, K. Słomińska – CBK PAN M.Rybczyński, Z.Włodarczyk – Kielce University G.Siemieniec-Oziebło – OA Jagiellonian University and accepted with pleasure New formal body will be created: the consortium to • apply for funds in Poland (Poland is not ESA memeber, so far) • sign Memorandum of Understanding with RIKEN Poland is going to join ESA – European Space Agency we found the electronic manufacture suitable to produce (assemble) electronics for space, but there are no such enterprise with space certificates in Poland.

38. JEM-EUSO in Poland JEM-EUSO Polish group members (by subject): EAS: B.Szabelska, J.Szabelski, T.Wibig, Z.Włodarczyk High energy interactions: M.Rybczyński, T.Tymieniecka, T.Wibig TLE: J.Błęcki, H.Rothkaehl, K. Słomińska Hardware (High voltage power supply + switches): J. Karczmarczyk, T.Batsch, P. Orleański, J.Szabelski Astronomy (IG magnetic fields): G.Siemieniec-Oziębło Polish coordinator: J.Szabelski

39. JEM-EUSO in Poland Main participating institutions and researches (1): CBK PAN (Warsaw) Space Research Center of the Polish Academy of Sciences Dr. Piotr Orleański is the leader of the group of the hardware for space research, The group has made several devices which are currently in space, they have many years experience and expertize in hardware for space research; Prof. Jan Błęcki and Prof. Hanna Rothkaehl are experts in TLEs, they are participating in a few other space experiments for TLEs measurements OAUJ (Kraków) Astronomical Observatory of the Jagielonian University Prof. Grażyna Siemieniec-Oziębło is working on the galactic and extragalactic magnetic fields, the group is also involved in studies of acceleration mechanisms, and in measurements of Schumann resonance (low frequency radio effect) powered by TLEs and lightnings.

40. JEM-EUSO in Poland Main participating institutions and researches (2): IPJ (Łódź) The Andrzej Sołtan Institute for Nuclear Studies EAS and Cosmic Ray astrophysics are the main topics studied in our group. The Cosmic Ray group in Łódź was set up in the 1950's by Prof. A. Zawadzki (in collaboration with Prof. R. Maze), then developed by Prof. J. Wdowczyk (in collaboration with Prof. Sir A.W. Wolfendale, and Prof. J.N. Capdevielle). The first European Cosmic Ray Symposium was held in Łódź, and in 2009 (together with the University of Łódź) we hosted the 31st International Cosmic Ray Conference.

41. ISS - KIBO

43. Transportation modele H-II is of the bus size

44. Japanese Experiment Module/ Exposure Facility (JEM/EF) KIBO – JEM inside

45. Japanese Experiment Module/ Exposure Facility (JEM/EF) KIBO – JEM inside

46. ISS - KIBO

49. High energy interactions LHC data , and EAS simulations LHC data till s1/2 = 7000 GeV Large differences between models used in EAS simulations for energies above LHC

50. High energy interactions p - p π+- p Large differences between models used in EAS simulations for energies above LHC