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JEM-EUSO Extreme Universe Space Observatory Onboard Japanese Experiment Module JEM-EUSO Extreme Universe Space Observatory onboard Japanese Experiment Module Report on the Phase A Study JEM-EUSO Collaboration December 2008 JEM-EUSO: Extreme Universe Space Observatory onboard Japanese Experiment Module - ii - Report on the Phase A Study (Purple Book) JEM-EUSO Collaboration JEM-EUSO is a collaborating effort of 170 members from 12 countries and 62 institutes (list updated on December 2008): Japan: T. Ebisuzaki, H. Omori, K. Maekawa, Y. Hachisu, K. Katahira, M. Mizutani, Y. Kawasaki, Y. Takizawa, S. Wada, K. Kawai, H. Mase, K. Shinozaki, T. Ogawa (RIKEN), F. Kajino, M. Sakata, Y. Yamamoto, F. Sato, N. Ebizuka, T. Yamamoto (Konan Univ.), M. Nagano, Y. Miyazaki (Fukui Univ. of Technology), T. Shibata, N. Sakaki (Aoyama Gakuin Univ.), N. Inoue (Saitama Univ.), Y. Uchibori (National Institute of Radiological Sciences), K. Nomoto (Tokyo Univ.), Y. Takahashi (Tohoku Univ.), M. Takeda (ICRR), H. Shimizu, Y. Arai, Y. Kurihara, J. Fujimoto (KEK), S. Yoshida, K. Mase (Chiba Univ.) , Y. Mizumoto, J. Watanabe, S. Inoue, K. Asano, T. Kajino (NAOJ), H. Ikeda, M. Suzuki, H. Yano (ISAS/JAXA), T. Murakami, D. Yonetoku (Kanazawa Univ.), N. Sugiyama (Nagoya Univ.), Y. Itow (STE, Nagoya Univ.), S. Nagataki (Yukawa Institute for Theoretical Physics, Kyoto Univ.), A. Saito (Graduate School of Science, Faculty of Science, Kyoto Univ.), S. Abe, M. Nagata (Kobe Univ.), M. Chikawa (Kinki Univ.), F. Tajima (Hiroshima Univ.), M. Sato (Hokkaido Univ.) USA: J. H. Adams, S. Mitchell, M.J. Christl, J. Watts Jr., A. English, R. Young (MSFC/NASA) , Y. Takahashi, D. Gregory, M. Bonamente, V. Connaughton, K. Pitalo, J. Hadaway, J. Geary, R. Lundquist, P. Reardon, T. Blackwell (Univ. Alabama), H. Crawford, E. Judd, C. Pennypacker (LBL, Univ. California, Berkeley), V. Andreev, K. Arisaka, D. Cline (UCLA), A. Berlind ,T. Weiler, S. Czorna (Vanderbilt Univ.), R. Chipman, S. McClain (Univ. Arizona) France: D. Allard, J-N. Capdevielle, J. Dolbeau, Ph. Gorodetzky, J-J. Jaeger, E. Parizot, T. Patzak, D. Semikoz, J. Weisbard (APC Paris) Germany: M. Teshima, H. Miyamoto, T. Schweizer (MPI Munich), A. Santangelo, E. Kendziorra, F. Fenu (Univ. Tübingen), P. Biermann (MPI Bonn), K. Mannheim (Wuerzburg), J. Wilms (Univ. Erlangen), T.Tajiman (LMU & MPQ) Italy: E. Pace, M. Focardi, P. Spillantini (Univ. Firenze), V. Bratina, L. Gambicorti, A. Zuccaro (INOA/CNR Firenze), A. Anzalone, O. Catalano, G. La Rosa, M.C. Maccarone, B. Sacco (IASF- PA/INAF Palermo), G. D’Alì Staiti, D. Tegolo (Univ. Palermo), M. Casolino, M.P. De Pascale, A. Morselli, P. Picozza, R. Sparvoli (INFN and Univ. “Tor Vergata” Roma), P. Vallania (IFSI/INAF Torino), P. Galeotti, M. Bertaina, C. Vigorito (Univ. Torino), D. D’Urso, F. Guarino, F. Isgrò, S. Russo (Univ. Napoli), M. Ambrosio, C. Aramo, D. Campana, G. De Rosa, G. Osteria (INFN-Napoli), M. Ricci (INFN-Frascati) Mexico: G. Medina-Tanco, J.C. D’Olivo, J.F. Valdés (UNAM), H. Salazar, O. Martines (BUAP), L. Villaseñor (UMSNH) Poland: T. Batsch, B. Szabelska, J. Szabelski, T. Wibig (IPJ), T. Tymieniecka( Podlasie Univ.), Z. Wlodarczyk (Kielce Univ.), G. Siemieniec-Ozieblo (Jagiellonian Univ.) Republic of Korea: S. Nam, I.H. Park, J. Yang, J.H. Park, T. Chung (Ehwa W. Univ.), T.W. Kim (Ajou Univ.), S.W. Kim (Yonsei Univ.), K.K. Joo (Chonnam National Univ.) Russia: G.K. Garipov, B.A. Khrenov, P.A. Klimov, M.I. Panasyuk, I.V. Yashin (SINP MSU), D. Naumov, L. Tkachev (Dubna JINR) Slovakia: K. Kudela, R. Bucik, R. Bobik, M. Slivka (Inst. Experimental Physics, KOSICE) Spain: M.D. Rodriguez-Frias, L.Peral, J. Gutierrez, R. Gomez-Herrero (Univ. Alcala) Switzerland: A. Maurissen, V. Mitev (CSEM Neuchatel) - iii - JEM-EUSO: Extreme Universe Space Observatory onboard Japanese Experiment Module - iv - Report on the Phase A Study (Purple Book) JEM-EUSO Mission Summary Accommodated on the Japanese Experiment Module (JEM) of the International Space Station (ISS), the Extreme Universe Space Observatory JEM-EUSO will utilize the Earth atmosphere as a giant detector of the highest energy cosmic rays, the most energetic particles coming from the Universe. Looking downward the Earth from Space, JEM-EUSO will detect such particles observing the fluorescence signal produced during their pass in the atmosphere. The main objective of JEM-EUSO is the possibility of doing astronomy and astrophysics through the particle channel with extreme energies above 1020 eV, so extending, with a significant statistical evidence, the measurement of the energy spectrum of the cosmic radiation beyond the Greisen-Zatsepin-Kuzmin (GZK) cut-off. Moreover, using the atmosphere as a giant detector, JEM-EUSO could observe extremely high energy neutrinos, so opening the field of high energy neutrino astronomy. Furthermore, JEM-EUSO will contribute to the investigation of phenomena intrinsic to the Earth’s atmosphere or induced by the flux of meteoroids incoming from Space. JEM-EUSO has been designed to operate for more than 3 years onboard the International Space Station orbiting around the Earth every 90 minutes at altitude of about 400 km. JEM-EUSO is a worldwide collaborating effort of 62 research groups from 12 countries. Scientific Objectives Main Objective: Astronomy and astrophysics through particle channel with extreme energies > 1020 eV Identification of sources by the high-statistics arrival direction analysis Measurement of the energy spectra from individual sources to constrain acceleration or emission mechanisms Exploratory Objectives: Detection of extreme energy gamma-rays Detection of extreme energy neutrinos Study of the Galactic magnetic field Verification of the relativity and the quantum gravity effect in extreme energy Global of nightglows, plasma discharges and lightning Parameters of Instrument Parameters of Mission Field of View ±30° Time of launch year 2013 Observational area >1.9×105 km2 Operation period 3 years (+ 2 years) Optical bandwidth 330 ÷400 nm Launching rocket H2B Focal Surface area 4.5 m2 Transportation to ISS, non pressurized Carrier of H2 international Space Station Transfer Vehicle HTV Number of pixels ~2.0×105 Site to attach Japanese Exposure Module JEM/ Exposure Facility EF#2 Pixel size 4.5 mm Mass 1983 kg Pixel size at ground 750 m Power 926 W (operative), and spatial resolution 0.1° 352 W (non-operative) Event time sampling ≤ 2.5 µs Data transfer rate 285 kpbs Duty cycle ~20% Orbit: height , inclination ~ 400 km, 51.64° - v - JEM-EUSO: Extreme Universe Space Observatory onboard Japanese Experiment Module - vi - Report on the Phase A Study (Purple Book) Table of contents Foreword................................................................................................................... 1 1. Mission Overview............................................................................................ 3 2. Science Objectives........................................................................................... 5 2.1. Main Objective: Astronomy and Astrophysics through the Particle Channel...............5 2.1.1. Identification of sources by the high-statistics arrival direction analysis..............7 2.1.2. Measurements of the energy spectra from individual sources .............................10 2.2. Exploratory Objectives....................................................................................................15 2.2.1. Detection of extreme energy gamma rays .............................................................15 2.2.2. Detection of extreme energy neutrinos..................................................................18 2.2.3. Study of the galactic magnetic field.......................................................................20 2.2.4. Verification of the relativity and the quantum gravity effect...............................21 2.2.5. Global observation of nightglows, plasma discharges, and lightning .................21 3. Observation Principle and Requirements.................................................... 25 3.1. Observation Principle......................................................................................................25 3.2. Accuracy of Observables ................................................................................................27 3.2.1. Effective area...........................................................................................................27 3.2.2. Time resolution, collecting aperture, pixel size, Xmax...........................................27 3.2.3. Dark current and night sky background.................................................................29 3.3. Requirements ...................................................................................................................29 3.3.1. Scientific requirements ...........................................................................................29 3.3.2. Observation requirements.......................................................................................29 3.3.3. Instrument requirements .........................................................................................29 3.3.4. Miscellanea..............................................................................................................30 3.4. Success Criteria ...............................................................................................................31 4. Instrument..................................................................................................... 33 4.1. Overview..........................................................................................................................33
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