The JEM-EUSO instrument
Anno: 2015
Autori: The JEM-EUSO Collaboration Adams, J.H. Jr., Ahmad S., Albert J.-N., Allard D., Anchordoqui L., Andreev V., Anzalone A., Arai Y., Asano K., Ave Pernas M., Baragatti P., Barrillon P., Batsch T., Bayer J., Bechini R., Belenguer T., Bellotti R., Belov K., Berlind A.A., Bertaina M., Biermann P.L., Biktemerova S., Blaksley C., Blanc N., Bl?cki J., Blin-Bondil S., Bl�mer J., Bobik P., Bogomilov M., Bonamente M., Briggs M.S., Briz S., Bruno A., Cafagna F., Campana D., Capdevielle J.-N., Caruso R., Casolino M., Cassardo C., Castellinic G., Catalano C., Catalano G., Cellino A., Chikawa M., Christl M.J., Cline D., Connaughton V., Conti L., Cordero G., Crawford H.J., Cremonini R., Csorna S., Dagoret-Campagne S., de Castro A.J., De Donato C., de la Taille C., De Santis C., del Peral L., Dell�Oro A., De Simone N., Di Martino M., Distratis G., Dulucq F., Dupieux M., Ebersoldt A., Ebisuzaki T., Engel R., Falk S., Fang K., Fenu F., Fern�ndez-G�mez I., Ferrarese S., Finco D., Flamini M., Fornaro C., Franceschi A., Fujimoto J., Fukushima M., Galeotti P., Garipov G., Geary J., Gelmini G., Giraudo G., Gonchar M., Gonz�lez Alvarado C., Gorodetzky P., Guarino F., Guzm�n A., Hachisu Y., Harlov B., Haungs A., Hern�ndez Carretero J., Higashide K., Ikeda D., Ikeda H., Inoue N., Inoue S., Insolia A., Isgr� F., Itow Y., Joven E., Judd E.G., Jung A., Kajino F., Kajino T., Kaneko I., Karadzhov Y., Karczmarczyk J., Karus M., Katahira K., Kawai K., Kawasaki Y., Keilhauer B., Khrenov B.A., Kim J.-S., Kim S.-W., Kim S.-W., Kleifges M., Klimov P.A., Kolev D., Kreykenbohm I., Kudela K., Kurihara Y., Kusenko A., Kuznetsov E., Lacombe M., Lachaud C., Lee J., Licandro J., Lim H., L�pez F., Maccarone M.C., Mannheim K., Maravilla D., Marcelli L., Marini A., Martinez O., Masciantonio G., Mase K., Matev R., Medina-Tanco G., Mernik T., Miyamoto H., Miyazaki Y., Mizumoto Y., Modestino G., Monaco A., Monnier-Ragaigne D., Morales de los R�os J.A., Moretto C., Morozenko V.S., Mot B., Murakami T., Murakami M.N., Nagata M., Nagataki S., Nakamura T., Napolitano T., Naumov D., Nava R., Neronov A., Nomoto K., Nonaka T., Ogawa T., Ogio S., Ohmori H., Olinto A.V., Orleanski P., Osteria G., Panasyuk M.I., Parizot E., Park I.H., Park H.W., Pastircak B., Patzak T., Paul T., Pennypacker C., Perez Cano S., Peter T., Picozza P., Pierog T., Piotrowski L.W., Piraino S., Plebaniak Z., Pollini A., Prat P., Pr�v�t G., Prieto H., Putis M., Reardon P., Reyes M., Ricci M., Rodr�guez I., Rodr�guez Fr�as M.D., Ronga F., Roth M., Rothkaehl H., Roudil G., Rusinov I., Rybczynski M., Sabau M.D., S�ez-Cano G., Sagawa H., Saito A., Sakaki N., Sakata M., Salazar H., S�nchez S., Santangelo A., Santiago Cr�z L., Sanz Palomino M., Saprykin O., Sarazin F., Sato H., Sato M., Schanz T., Schieler H., Scotti V., Segreto A., Selmane S., Semikoz D., Serra M., Sharakin S., Shibata T., Shimizu H.M., Shinozaki K., Shirahama T., Siemieniec-Ozi?blo G., Silva L�pez H.H., Sledd J., Slominska K., Sobey A., Sugiyama T., Supanitsky D., Suzuki M., Szabelska B., Szabelski J., Tajima F., Tajima N., Tajima T., Takahashi Y., Takami H., Takeda M., Takizawa Y., Tenzer C., Tibolla O., Tkachev L., Tokuno H., Tomida T., Tone N., Toscano S., Trillaud F., Tsenov R., Tsunesada Y., Tsuno K., Tymieniecka T., Uchihori Y., Unger M., Vaduvescu O., Vald�s-Galicia J.F., Vallania P., Valore L., Vankova G., Vigorito C., Villase�or L., von Ballmoos P., Wada S., Watanabe J., Watanabe S., Watts J., Jr. Weber, M. Weiler, T.J. Wibig, T. Wiencke, L. Wille, M. Wilms, J. Wlodarczyk, Z. Yamamoto, T. Yamamoto, Y. Yang, J. Yano, H. Yashin, I.V. Yonetoku, D. Yoshida, K. Yoshida, S. Young, R. Zotov, M.Y. Zuccaro Marchi, A.
Affiliazione autori: St. Kliment Ohridski University of Sofia, Sofia, Bulgaria; LAL, Univ Paris-Sud, CNRS/IN2P3, Orsay, France; Omega, Ecole Polytechnique, CNRS/IN2P3, Palaiseau, France; APC, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs. de Paris, Sorbonne Paris Cit�, Paris, France; IRAP, Universit� de Toulouse, CNRS, Toulouse, France; ECAP, University of Erlangen-Nuremberg, Erlangen, Germany; Karlsruhe Institute of Technology (KIT), Karlsruhe, Germany; Ludwig Maximilian University, Munich, Germany; Institute for Astronomy and Astrophysics, Kepler Center, University of T�bingen, T�bingen, Germany; Institut f�r Theoretische Physik und Astrophysik, University of W�rzburg, W�rzburg, Germany; Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Bari, Italy; Universita� degli Studi di Bari Aldo Moro and INFN, Sezione di Bari, Bari, Italy; Dipartimento di Fisica e Astronomia, Universita� di Catania, Catania, Italy; Consiglio Nazionale delle Ricerche (CNR), Ist. di Fisica Applicata Nello Carrara, Firenze, Italy; Istituto Nazionale di Fisica Nucleare – Laboratori Nazionali di Frascati, Frascati, Italy; Istituto Nazionale di Fisica Nucleare – Sezione di Napoli, Naples, Italy; Dipartimento di Scienze Fisiche, Universita� di Napoli Federico II, Naples, Italy; INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Palermo, Italy; Istituto Nazionale di Fisica Nucleare – Sezione di Roma Tor Vergata, Roma, Italy; Dipartimento di Fisica, Universita� di Roma Tor Vergata, Roma, Italy; Istituto Nazionale di Fisica Nucleare – Sezione di Torino, Torino, Italy; Dipartimento di Fisica, Universit� di Torino, INFN Torino, Torino, Italy; Istituto Nazionale di Astrofisica, Osservatorio Astrofisico di Torino, Torino, Italy; Istituto Nazionale di Fisica Nucleare – Sezione di Catania, Catania, Italy; Dipartimento di Ingegneria, UTIU, Rome, Italy; DIETI, Universita� degli Studi di Napoli Federico II, Napoli, Italy; Chiba University, Chiba, Japan; National Institute of Radiological Sciences, Chiba, Japan; Fukui University of Technology, Fukui, Japan; Kinki University, Higashi-Osaka, Japan; Hiroshima University, Hiroshima, Japan; Kanazawa University, Kanazawa, Japan; Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Japan; Kobe University, Kobe, Japan; Konan University, Kobe, Japan; Kyoto University, Kyoto, Japan; Yukawa Institute, Kyoto University, Kyoto, Japan; National Astronomical Observatory, Mitaka, Japan; Nagoya University, Nagoya, Japan; Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Japan; Graduate School of Science, Osaka City University, Osaka, Japan; Institute of Space and Astronautical Science/JAXA, Sagamihara, Japan; Aoyama Gakuin University, Sagamihara, Japan; Saitama University, Saitama, Japan; Hokkaido University, Sapporo, Japan; Interactive Research Center of Science, Tokyo Institute of Technology, Tokyo, Japan; University of Tokyo, Tokyo, Japan; High Energy Accelerator Research Organization (KEK), Tsukuba, Japan; RIKEN, Wako, Japan; Korea Astronomy and Space Science Institute (KASI), Daejeon, South Korea; Ewha Womans University, Seoul, South Korea; Sungkyunkwan University, Seoul, South Korea; Center for Galaxy Evolution Research, Yonsei University, Seoul, South Korea; Universidad Nacional Aut�noma de M�xico (UNAM), Mexico City, Mexico; Universidad Michoacana de San Nicolas de Hidalgo (UMSNH), Morelia, Mexico; Benem�rita Universidad Aut�noma de Puebla (BUAP), Puebla, Mexico; Institute of Physics, Jan Kochanowski University, Kielce, Poland; Astronomical Observatory, Jagiellonian University, Krakow, Poland; National Centre for Nuclear Research, Lodz, Poland; Space Research Centre of the Polish Academy of Sciences (CBK), Warsaw, Poland; Joint Institute for Nuclear Research, Dubna, Russian Federation; Central Research Institute of Machine Building, TsNIIMash, Korolev, Russian Federation; Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russian Federation; Department of Space Physics, Institute of Experimental Physics, Kosice, Slovakia; Consejo Superior de Investigaciones Cient�ficas (CSIC), Madrid, Spain; Instituto Nacional de T�cnica Aeroespacial (INTA), Madrid, Spain; Universidad de Alcal� (UAH), Madrid, Spain; Universidad Carlos III de Madrid, Madrid, Spain; Instituto de Astrof�sica de Canarias (IAC), Tenerife, Spain; Swiss Center for Electronics and Microtechnology (CSEM), Neuch�tel, Switzerland; ISDC Data Centre for Astrophysics, Versoix, Switzerland; Institute for Atmospheric and Climate Science, ETH Z�rich, Z�rich, Switzerland; Space Science Laboratory, University of California, Berkeley, United States; University of Chicago, Chicago, United States; Colorado School of Mines, Golden, United States; University of Alabama in Huntsville, Huntsville, United States; University of California (UCLA), Los Angeles, United States; University of Wisconsin-Milwaukee, Milwaukee, United States; NASA – Marshall Space Flight Center, Madison County, United States; Vanderbilt University, Nashville, United States; RIKEN, 2-1 Hirosawa, Wako-shi, Japan; INFN University, Rome Tor Vergata, Rome, Italy; Faculty of Science and Engineering, Department of Physics, Konan University, Kobe, Japan
Abstract: In this paper we describe the main characteristics of the JEM-EUSO instrument. The Extreme Universe Space Observatory on the Japanese Experiment Module (JEM-EUSO) of the International Space Station (ISS) will observe Ultra High-Energy Cosmic Rays (UHECR) from space. It will detect UV-light of Extensive Air Showers (EAS) produced by UHECRs traversing the Earth�s atmosphere. For each event, the detector will determine the energy, arrival direction and the type of the primary particle. The advantage of a space-borne detector resides in the large field of view, using a target volume of about 10 12 tons of atmosphere, far greater than what is achievable from ground. Another advantage is a nearly uniform sampling of the whole celestial sphere. The corresponding increase in statistics will help to clarify the origin and sources of UHECRs and characterize the environment traversed during their production and propagation. JEM-EUSO is a 1.1 ton refractor telescope using an optics of 2.5 m diameter Fresnel lenses to focus the UV-light from EAS on a focal surface composed of about 5,000 multi-anode photomultipliers, for a total of ?3�10 5 channels. A multi-layer parallel architecture handles front-end acquisition, selecting and storing valid triggers. Each processing level filters the events with increasingly complex algorithms using FPGAs and DSPs to reject spurious events and reduce the data rate to a value compatible with downlink constraints.
Giornale/Rivista: EXPERIMENTAL ASTRONOMY (PRINT)
Volume: 40 (1) Da Pagina: 19 A: 44
Parole chiavi: Cosmic rays; International space station; UHECR
DOI: 10.1007/s10686-014-9418-x
Citazioni: 38
dati da “WEB OF SCIENCE” (of Thomson Reuters) aggiornati al: 2025-07-13
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