W em easured twom om entsofthelepton m om entum spectrum in B ! X ‘ ,where‘= eor ,for p‘ 1:5 G eV=c. From these we derive the Heavy Q uark Expansion (HQ E)param eters (M S)= 0:39 0:03jstat 0:06jsys 0:12jth G eV and 1 = 0:25 0:02jstat 0:05jsys 0:14jth G eV ,through order 1=M 3 B in the non-perturbative expansion and 0 2 s in the perturbative expansion. The theoreticalexpression needed to extract jVcbjfrom the m easured sem ileptonic width is evaluated using theseHQ E param eters.Com bined with theworld averageofthesem ileptonicwidth,we nd jVcbj= (40:8 0:5j sl 0:4j( 1; )exp 0:9jth) 10 .Finally,theshortrange b-quark m assm 1S b is evaluated and found to be4:82 0:07jexp 0:11jth G eV/c . Subm itted to the 31 InternationalConferenceon High Energy Physics,July 2002,Am sterdam

J. H. Adams2, R. Aloisio3, L. A. Anchordoqui4, D. R. Bergman5, M. E. Bertaina6 , P. Bertone7, M. J. Christl7, S. E. Csorna8, J. B. Eser9, F. Fenu6, E. A. Hays10, S. Hunter10, E. Judd11, I. Jun12, J. F. Krizmanic10, E. Kuznetsov2, L. M. Martinez-Sierra12, M. Mastafa2, J. N. Matthews5, J. McEnery10, J. W. Mitchell10, A. Neronov13, A. N. Otte14, E. Parizot15, T. C. Paul4,J. S. Perkins10, G. Prevot15, P. Reardon2, M. H. Reno16, F. Sarazin9, K. Shinozaki6, F. Stecker10, R. Streitmatter10, L. Wiencke9, R. M. Young7 2University of Alabama, Huntsville, AL, USA; 3Gran Sasso Science Institute, L’Aquila, Italy; 4City University of New York, Lehman College, NY, USA; 5University of Utah, Salt Lake City, Utah, USA; 6Universita di Torino, Torino, Italy; 7NASA Marshall Space Flight Center, Huntsville, AL, USA; 8Vanderbilt University, Nashville, TN, USA; 9Colorado School of Mines,

The Extreme Universe Space Observatory (EUSO) instrument is being developed for deployment on the International Space Station (ISS). Looking down from its berth on the ISS, EUSO will take high speed UV videos of Extensive Air Showers (EAS) caused by cosmic rays. Using these videos, the energy and arrival direction of each very high energy cosmic ray will be reconstructed. In order to reconstruct the energy, the absolute sensitivity of EUSO must be known. To test the EUSO instrument concept a prototype of EUSO (EUSO-TA) has been deployed on the Telescope Array (TA) site in Utah, USA. EUSO-TA takes advantage of the calibration facilities available on the TA site and the opportunity to observe extensive air showers recorded by the TA’s fluorescence detectors. In this paper we describe the use of calibrated ultraviolet (UV) light emitting diodes (LEDs) to calibrate the EUSO-TA instrument.

Ultra high energy photons and neutrinos are carriers of very important astrophysical information. They may be produced at the sites of cosmic ray acceleration or during the propagation of the cosmic rays in the intergalactic medium. In contrast to charged cosmic rays, photon and neutrino arrival directions point to the production site because they are not deflected by the magnetic fields of the Galaxy or the intergalactic medium. In this work we study the characteristics of the longitudinal development of showers initiated by photons and neutrinos at the highest energies. These studies are relevant for development of techniques for neutrino and photon identification by the JEM-EUSO telescope. In particular, we study the possibility of observing the multi-peak structure of very deep horizontal neutrino showers with JEM-EUSO. We also discuss the possibility to determine the flavor content of the incident neutrino flux by taking advantage of the different characteristics of the longitudinal profiles generated by different type of neutrinos. This is of grate importance for the study of the fundamental properties of neutrinos at the highest energies. Regarding photons, we discuss the detectability of the cosmogenic component by JEM-EUSO and also estimate the expected upper limits on the photon fraction which can be obtained from the future JEM-EUSO data for the case in which there are no photons in the samples.

Mounted on the International Space Station(ISS), the Extreme Universe Space Observatory, on-board the Japanese Experimental Module (JEM-EUSO), relies on the well established fluorescence technique to observe Extensive Air Showers (EAS) developing in the earth’s atmosphere. Focusing on the detection of Ultra High Energy Cosmic Rays (UHECR) in the decade of 1020eV, JEM-EUSO will face new challenges by applying this technique from space. The EUSO Simulation and Analysis Framework (ESAF) has been developed in this context to provide a full end-to-end simulation frame, and assess the overall performance of the detector. Within ESAF, angular reconstruction can be separated into two conceptually different steps. The first step is pattern recognition, or filtering, of the signal to separate it from the background. The second step is to perform different types of fitting in order to search for the relevant geometrical parameters that best describe the previously selected signal. In this paper, we discuss some of the techniques we have implemented in ESAF to perform the geometrical reconstruction of EAS seen by JEM-EUSO. We also conduct thorough tests to assess the performances of these techniques in conditions which are relevant to the scope of the JEM-EUSO mission. We conclude by showing the expected angular resolution in the energy range that JEM-EUSO is expected to observe.

The Extreme Universe Space Observatory is a mission to investigate the highest energy cosmic rays by recording the extensive air showers they create in the Earth’s atmosphere. This will be done by observing these showers from low Earth orbit. These observations will be used to measure the flux, energies and arrival directions of these cosmic rays. This paper describes how the accuracy of these measurements will be tested and improved during the mission using the Global Light System (consisting of calibrated xenon flash lamps and lasers) located deep in the Earth’s atmosphere.

The Extreme Universe Space Observatory is an experiment to investigate the highest energy cosmic rays by recording the extensive air showers they create in the atmosphere. This will be done by recording video clips of the development of these showers using a large high-speed video camera to be located on the Japanese Experiment Module of the International Space Station. The video clips will be used to determine the energies and arrival directions of these cosmic rays. The accuracy of these measurements depends on measuring the intrinsic luminosity and the direction of each shower accurately. This paper describes how the accuracy of these measurements will be tested and improved during the mission using a global light system consisting of calibrated flash lamps and lasers located deep in the atmosphere.

Z. Li, A. Lopez, H. Mendez, J. Ramirez, G. S. Huang, D. H. Miller, V. Pavlunin, B. Sanghi, E. I. Shibata, I. P. J. Shipsey, G. S. Adams, M. Chasse, M. Cravey, J. P. Cummings, I. Danko, J. Napolitano, Q. He, H. Muramatsu, C. S. Park, W. Park, E. H. Thorndike, T. E. Coan, Y. S. Gao, F. Liu, M. Artuso, C. Boulahouache, S. Blusk, J. Butt, E. Dambasuren, O. Dorjkhaidav, J. Li, N. Menaa, R. Mountain, R. Nandakumar, R. Redjimi, R. Sia, T. Skwarnicki, S. Stone, J. C. Wang, K. Zhang, S. E. Csorna, G. Bonvicini, D. Cinabro, M. Dubrovin, R. A. Briere, G. P. Chen, J. Chen, T. Ferguson, G. Tatishvili, H. Vogel, M. E. Watkins, J. L. Rosner, N. E. Adam, J. P. Alexander, K. Berkelman, D. G. Cassel, V. Crede, J. E. Duboscq, K. M. Ecklund, R. Ehrlich, L. Fields, R. S. Galik, L. Gibbons, B. Gittelman, R. Gray, S. W. Gray, D. L. Hartill, B. K. Heltsley, D. Hertz, L. Hsu, C. D. Jones, J. Kandaswamy, D. L. Kreinick, V. E. Kuznetsov, H. Mahlke-Kruger, T. O. Meyer, P. U. E. Onyisi, J. R. Patterson, D. Peterson, E. A. Phillips, J. Pivarski, D. Riley, A. Ryd, A. J. Sadoff, H. Schwarthoff, M. R. Shepherd, S. Stroiney, W. M. Sun, D. Urner, T. Wilksen, M. Weinberger, S. B. Athar, P. Avery, L. Breva-Newell, R. Patel, V. Potlia, H. Stoeck, J. Yelton, P. Rubin, C. Cawlfield, B. I. Eisenstein, G. D. Gollin, I. Karliner, D. Kim, N. Lowrey, P. Naik, C. Sedlack, M. Selen, J. Williams, J. Wiss, K. W. Edwards, D. Besson, T. K. Pedlar, D. Cronin-Hennessy, K. Y. Gao, D. T. Gong, Y. Kubota, T. Klein, B. W. Lang, S. Z. Li, R. Poling, A. W. Scott, A. Smith, S. Dobbs, Z. Metreveli, K. K. Seth, A. Tomaradze, P. Zweber, J. Ernst, A. H. Mahmood, H. Severini, D. M. Asner, S. A. Dytman, W. Love, S. Mehrabyan, J. A. Mueller, and V. Savinov

This document contains a summary of the workshop which took place on 22 - 24 February 2012 at the Kavli Institute of Cosmological Physics in the University of Chicago. The goal of the workshop was to discuss the physics reach of the JEM-EUSO mission and how best to implement a global ground based calibration system for the instrument to realize the physics goal of unveiling the origin of the highest energy cosmic rays.

By using 1.8x10{6} DDpairs, we have measured B(D{0}-->pi{-}e{+}nu{e})=0.299(11)(9)%, B(D{+}-->pi{0}e{+}nu{e})=0.373(22)(13)%, B(D{0}-->K{-}e{+}nu{e})=3.56(3)(9)%, and B(D{+}-->K{0}e{+}nu{e})=8.53(13)(23)% and have studied the q;{2} dependence of the form factors. By combining our results with recent lattice calculations, we obtain |V{cd}|=0.217(9)(4)(23) and |V{cs}|=1.015(10)(11)(106).