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160 results on '"Andrii Neronov"'

51. A compact pulsar wind nebula model of the γ-ray-loud binary LS I +61○303

Author: Masha Chernyakova, Andrzej A. Zdziarski, and Andrii Neronov
Subjects: Physics, Be star, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Electron, Astrophysics::Cosmology and Extragalactic Astrophysics, Orbital period, Pulsar wind nebula, Lorentz factor, symbols.namesake, Polar wind, Pulsar, Space and Planetary Science, symbols, Astrophysics::Solar and Stellar Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: We study a model of of LS I +61 303 in which its radio to TeV emission is due to interaction of a relativistic wind from a young pulsar with the wind from its companion Be star. We assume the fast polar wind is clumpy, which is typical for radiatively-driven winds. The clumpiness cause the two winds to mix. The relativistic electrons from the pulsar wind are retained in the moving clumps by inhomogeneities of the magnetic field, which explains the X-ray variability observed on time scales much shorter than the orbital period. We calculate detailed inhomogeneous spectral models reproducing the average broad-band spectrum from radio to TeVs. Given the uncertainties the form of the distribution of relativistic electrons, the X-ray spectrum could be dominated by either Compton or synchrotron emission. The recent Fermi observations constrain the high-energy cut-off in the electron distribution to be at the Lorentz factor of 2 10^4 or 10^8 in the former and latter model, respectively. We provide formulae comparing the losses of the relativistic electrons due to Compton, synchrotron and Coulomb processes vs. the distance from the Be star. We calculate the optical depth of the wind to free-free absorption, showing that it will suppress most of the radio emission within the orbit. We point out the importance of Compton and Coulomb heating of the stellar wind within and around the gamma-ray emitting region. Then, we find the most likely mechanism explaining the orbital modulation at TeV energies is anisotropy of emission., MNRAS, in press
Published: 2017

52. Long-term monitoring of bright blazars in the multi-GeV to TeV range with FACT

Author: Thomas Bretz, Karl Mannheim, Max Nöthe, Fabian Temme, Roland Walter, Wolfgang Rhode, Anton Dmytriiev, Adrian Biland, Kai Brügge, Lena Linhoff, Gareth Hughes, Julia Thaele, Matthias Bergmann, Felicitas Pauss, Dorothee Hildebrand, Sebastian Müller, Dominik Baack, Sabrina Einecke, Jens Buss, Aleksander Paravac, Christina Hempfling, J. Adam, Max Ludwig Ahnen, Michael Blank, Daniela Dorner, Amit Shukla, Andrii Neronov, Dominik Neise, and Matteo Balbo
Subjects: Active galactic nucleus, Long-term monitoring, lcsh:Astronomy, Physics::Instrumentation and Detectors, Very high energy gamma rays, Astrophysics::High Energy Astrophysical Phenomena, First G-APD Cherenkov Telescope, IACT, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, Imaging Air Cherenkov Telescope, Silicon photo multiplier, lcsh:QB1-991, Silicon photomultiplier, law, 0103 physical sciences, ddc:530, very high energy gamma rays, long-term monitoring, silicon photo multiplier, 010306 general physics, Blazar, Cherenkov radiation, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Light curve, Monitoring program
Abstract: Blazars like Markarian 421 or Markarian 501 are active galactic nuclei (AGN), with their jets orientated towards the observer. They are among the brightest objects in the very high energy (VHE) gamma ray regime (>100 GeV). Their emitted gamma-ray fluxes are extremely variable, with changing activity levels on timescales between minutes, months, and even years. Several questions are part of the current research, such as the question of the emission regions or the engine of the AGN and the particle acceleration. A dedicated longterm monitoring program is necessary to investigate the properties of blazars in detail. A densely sampled and unbiased light curve allows for observation of both high and low states of the sources, and the combination with multi-wavelength observation could contribute to the answer of several questions mentioned above. FACT (First G-APD Cherenkov Telescope) is the first operational telescope using silicon photomultiplier (SiPM, also known as Geigermode—Avalanche Photo Diode, G-APD) as photon detectors. SiPM have a very homogenous and stable longterm performance, and allow operation even during full moon without any filter, leading to a maximal duty cycle for an Imaging Air Cherenkov Telescope (IACT). Hence, FACT is an ideal device for such a longterm monitoring of bright blazars. A small set of sources (e.g., Markarian 421, Markarian 501, 1ES 1959+650, and 1ES 2344+51.4) is currently being monitored. In this contribution, the FACT telescope and the concept of longterm monitoring of bright blazars will be introduced. The results of the monitoring program will be shown, and the advantages of densely sampled and unbiased light curves will be discussed., Galaxies;5(1)
Published: 2017

53. First study of combined blazar light curves with FACT and HAWC

Author: Daniela Dorner, Sabrina Einecke, Julia Thaele, Amit Shukla, Felicitas Pauss, Michael Blank, Adrian Biland, Matthias Bergmann, Christina Hempfling, Thomas Bretz, J. Adam, Anton Dmytiiev, Max Ludwig Ahnen, Lena Linhoff, Matteo Balbo, Kai Brügge, Wolfgang Rhode, Aleksander Paravac, Dorothee Hildebrand, Sebastian Müller, Gareth Hughes, Roland Walter, R. J. Lauer, Karl Mannheim, Andrii Neronov, Dominik Neise, Dominik Baack, Maximilian Noethe, Jens Buss, and Fabian Temme
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Light curve, law.invention, Telescope, Observatory, Sky, Duty cycle, law, Astrophysics - High Energy Astrophysical Phenomena, Blazar, Cherenkov radiation, Remote sensing, media_common
Abstract: For studying variable sources like blazars, it is crucial to achieve unbiased monitoring, either with dedicated telescopes in pointing mode or survey instruments. At TeV energies, the High Altitude Water Cherenkov (HAWC) observatory monitors approximately two thirds of the sky every day. It uses the water Cherenkov technique, which provides an excellent duty cycle independent of weather and season. The First G-APD Cherenkov Telescope (FACT) monitors a small sample of sources with better sensitivity, using the imaging air Cherenkov technique. Thanks to its camera with silicon-based photosensors, FACT features an excellent detector performance and stability and extends its observations to times with strong moonlight, increasing the duty cycle compared to other imaging air Cherenkov telescopes. As FACT and HAWC have overlapping energy ranges, a joint study can exploit the longer daily coverage given that the observatories' locations are offset by 5.3 hours. Furthermore, the better sensitivity of FACT adds a finer resolution of features on hour-long time scales, while the continuous duty cycle of HAWC ensures evenly sampled long-term coverage. Thus, the two instruments complement each other to provide a more complete picture of blazar variability. In this presentation, the first joint study of light curves from the two instruments will be shown, correlating long-term measurements with daily sampling between air and water Cherenkov telescopes. The presented results focus on the study of the variability of the bright blazars Mrk 421 and Mrk 501 during the last two years featuring various flaring activities., Comment: 6 pages, 2 figures. Contribution to the 6th International Symposium on High Energy Gamma-Ray Astronomy (Gamma2016), Heidelberg, Germany. To be published in the AIP Conference Proceedings
Published: 2017

54. Cosmic ray spectrum in the local Galaxy

Author: Dmitri Semikoz, Andrii Neronov, Denys Malyshev, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Solar System, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Cosmic ray, magnetic field, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ISM: clouds, GLAST, energy dependence, gamma rays: ISM, cosmic rays, PAMELA, 0103 physical sciences, cloud, cosmic radiation: injection, AMS, 010303 astronomy & astrophysics, approximation, Astrophysics::Galaxy Astrophysics, spectrum: slope, energy: low, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, cosmic radiation: spectrum, 010308 nuclear & particles physics, Molecular cloud, turbulence, Astronomy and Astrophysics, Fermi acceleration, acceleration, solar system, Galaxy, Interstellar medium, Space and Planetary Science, gamma ray, spectral, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic radiation: flux, local insterstellar matter, Fermi Gamma-ray Space Telescope
Abstract: We study the spectral properties of the cosmic-ray spectrum in the interstellar medium within 1 kpc distance from the Sun. We used eight-year exposure data of molecular clouds of the Gould Belt obtained with the Fermi/LAT telescope to precisely measure the cosmic-ray spectrum at different locations in the local Galaxy. We compared this measurement with the direct measurements of the cosmic-ray flux in and around the solar system obtained by Voyager and AMS-02 or PAMELA. We find that the average cosmic-ray spectrum in the local Galaxy in the 1-100 GeV range is well described by a broken power-law in rigidity with a low-energy slope of $2.33^{+0.06}_{-0.08}$ and a break at $18^{+7}_{-4}$ GV, with a slope change by $0.59\pm 0.11$. This result is consistent with an earlier analysis of the gamma-ray signal from the Gould Belt clouds based on a shorter exposure of Fermi/LAT and with a different event selection. The break at 10-20 GV is also consistent with the combined Voyager + AMS-02 measurements in/around the solar system. The slope of the spectrum below the break agrees with the slope of the average cosmic-ray spectrum in the inner part of the disk of the Milky Way that was previously derived from the Fermi/LAT gamma-ray data. We conjecture that it is this slope of 2.33 and not the locally measured softer slope of 2.7-2.8 that is determined by the balance between a steady-state injection of cosmic rays with a power-law slope of 2-2.1 that is due to Fermi acceleration and the energy-dependent propagation of cosmic-ray particles through the turbulent interstellar magnetic field with a Kolmogorov turbulence spectrum. The approximation of a continuous-in-time injection of cosmic rays at a constant rate breaks down, which causes the softening of the spectrum at higher energies., to match the accepted version
Published: 2017

55. First light on a new fully digital camera based on SiPM for CTA SST-1M telescope

Author: Matthieu Heller, Mira Grudzińska, Cyril Martin Alispach, J. Borkowski, Tomasz Bulik, Jerzy Michalowski, Andrii Neronov, Dusan Mandat, Michał Ostrowski, Karol Seweryn, Etienne Lyard, K. Skowron, Franck Cadoux, D. della Volpe, Jakub Rafalski, Jacek Niemiec, Petr Travnicek, T. R. S. Njoh Ekoume, Teresa Montaruli, Pawel Rajda, K. Zietara, Yannick Favre, Roland Walter, Isaac Troyano Pujadas, P. Paśko, E. Mach, Petr Schovanek, M. Stodulska, Victor Coco, Marek Jamrozy, Łukasz Stawarz, Jerzy Kasperek, Imen Al Samarai, Miroslav Pech, Rafał Moderski, Vitalii Sliusar, Marek Stodulski, and A. Zagdański
Subjects: Physics, business.product_category, Pixel, business.industry, IACT, First light, Cherenkov Telescope Array, law.invention, Telescope, Optics, Silicon photomultiplier, law, business, Cherenkov radiation, Digital camera
Abstract: The Cherenkov Telescope Array (CTA) will explore with unprecedented precision the Universe in the gammaray domain covering an energy range from 50 GeV to more the 300 TeV. To cover such a broad range with a sensitivity which will be ten time better than actual instruments, different types of telescopes are needed: the Large Size Telescopes (LSTs), with a ∼24 m diameter mirror, a Medium Size Telescopes (MSTs), with a ∼12 m mirror and the small size telescopes (SSTs), with a ∼4 m diameter mirror. The single mirror small size telescope (SST-1M), one of the proposed solutions to become part of the small-size telescopes of CTA, will be equipped with an innovative camera. The SST-1M has a Davies-Cotton optical design with a mirror dish of 4 m diameter and focal ratio 1.4 focussing the Cherenkov light produced in atmospheric showers onto a 90 cm wide hexagonal camera providing a FoV of 9 degrees. The camera is an innovative design based on silicon photomultipliers (SiPM ) and adopting a fully digital trigger and readout architecture. The camera features 1296 custom designed large area hexagonal SiPM coupled to hollow optical concentrators to achieve a pixel size of almost 2.4 cm. The SiPM is a custom design developed with Hamamatsu and with its active area of almost 1 cm 2 is one of the largest monolithic SiPM existing. Also the optical concentrators are innovative being light funnels made of a polycarbonate substrate coated with a custom designed UV-enhancing coating. The analog signals coming from the SiPM are fed into the fully digital readout electronics, where digital data are processed by high-speed FPGAs both for trigger and readout. The trigger logic, implemented into an Virtex 7 FPGA, uses the digital data to elaborate a trigger decision by matching data against predefined patterns. This approach is extremely flexible and allows improvements and continued evolutions of the system. The prototype camera is being tested in laboratory prior to its installation expected in fall 2017 on the telescope prototype in Krakow (Poland). In this contribution, we will describe the design of the camera and show the performance measured in laboratory.
Published: 2017

56. Strong constraints on hadronic models of blazar activity from Fermi and IceCube stacking analysis

Author: Andrii Neronov, Ksenia Ptitsyna, Dmitri Semikoz, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Observatoire de Paris - Site de Paris ( OP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: electron, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], AGN: jet, Energy flux, Astrophysics, blazar: emission, 01 natural sciences, 7. Clean energy, p: acceleration, neutrino: flux, IceCube, energy: flux, Muon neutrino, 010303 astronomy & astrophysics, model: leptonic, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, neutrinos, model: hadronic, p: beam, gamma ray: emission, stacking, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Population, galaxies: active, FOS: Physical sciences, gap, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, GLAST, neutrino: production, muon, 0103 physical sciences, gamma rays: galaxies, cosmic radiation: UHE, 010306 general physics, education, Blazar, Astronomy and Astrophysics, black hole: accretion, acceleration, Black hole, 13. Climate action, Space and Planetary Science, Physics::Accelerator Physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: High-energy emission from blazars is produced by electrons which are either accelerated directly (the assumption of leptonic models of blazar activity) or produced in interactions of accelerated protons with matter and radiation fields (the assumption of hadronic models). The hadronic models predict that gamma-ray emission is accompanied by neutrino emission with comparable energy flux but with a different spectrum. We derive constraints on the hadronic models of activity of blazars imposed by non-detection of neutrino flux from a population of gamma-ray emitting blazars. We stack the gamma-ray and muon neutrino flux from 749 blazars situated in the declination strip above -5 degrees. Non-detection of neutrino flux from the stacked blazar sample rules out the proton induced cacade models in which the high-energy emission is powered by interactions of shock-accelerated proton beam in the AGN jet with the ambient matter or with the radiation field of the black hole accretion disk. The result remains valid also for the case of interactions in the scattered radiation field in the broad line region. IceCube constraint could be avoided if the spectrum of accelerated protons is sharply peaking in the ultra-high-energy cosmic ray range, as in the models of acceleration in the magnetic reconnection regions or in the vacuum gaps of black hole magnetospheres. Models based on these acceleration mechanisms are consistent with the data only if characteristic energies of accelerated protons are higher than 1e19 eV., Comment: 8 pages, 3 figures
Published: 2017

57. JEM-EUSO observational technique and exposure

Author: G. Castellinic, Markus Roth, Thomas J. Weiler, S. Perez Cano, Fausto Guarino, P. von Ballmoos, M. Ricci, Roberto Bellotti, Andreas A. Berlind, K. Kawai, M. Di Martino, A. Marini, Graciela B. Gelmini, Akinori Saito, G. Osteria, T. Tymieniecka, Barbara Szabelska, T. Peter, J. Sledd, Y. Hachisu, Y. Arai, P. L. Biermann, Ovidiu Vaduvescu, M. Lacombe, Claudio Cassardo, M. Nagata, James H. Adams, J. Fujimoto, Dmitri Semikoz, O. Martinez, Dmitry V. Naumov, Y. Yamamoto, M. I. Panasyuk, I. V. Yashin, L. Marcelli, J.N. Capdevielle, H. Ikeda, Andrii Neronov, D. Kolev, Silvia Ferrarese, I. Rusinov, T. Mernik, Gali Garipov, Yoshihiko Mizumoto, Katsuaki Asano, Guillaume Prévôt, Kenji Shinozaki, A. Bruno, H. Sato, Pierre Barrillon, Valerie Connaughton, H. H. Silva Lopez, T. Batsch, T. Shibata, S. Selmane, T. Murakami, J. Karczmarczyk, Karl Mannheim, Michael S. Briggs, A. J. de Castro, N. Inoue, L. del Peral, A. Franceschi, E. Parizot, M. Bogomilov, Pavol Bobik, Y. Karadzhov, Yoshitaka Itow, G. Distratis, Marcos Reyes, Sergei A. Sharakin, R. Young, M. Sakata, A. Anzalone, N. Tajima, T. Napolitano, David B. Cline, T. Patzak, Piero Vallania, Hanna Rothkaehl, S. Blin-Bondil, M. D. Sabau, Satoshi Wada, T. Ogawa, F. Kajino, Shigehiro Nagataki, M. Serra, F. Cafagna, G. Modestino, Luis A. Anchordoqui, E. G. Judd, Katsuhiko Tsuno, H. W. Park, J. A. Morales de los Ríos, F. Tajima, E. Joven, Massimiliano Bonamente, R. Bechini, Ralph Engel, J. Watts, K. Belov, P. Gorodetzky, Humberto Ibarguen Salazar, C. Catalano, J. Lee, C. Lachaud, S. Dagoret-Campagne, Tomás Belenguer, B. A. Khrenov, Angela V. Olinto, Fernando López, Andrea Santangelo, C. De Santis, H. Tokuno, H. Miyamoto, E. Kuznetsov, C. Pennypacker, Piergiorgio Picozza, Toshikazu Ebisuzaki, L. Santiago Crúz, J. Bayer, M. Wille, I. Kreykenbohm, Vladimir Andreev, B. Pastircak, S. Sánchez, M. Ave Pernas, Alexander Kusenko, J. Błȩcki, M. Nagano Murakami, Frederic Trillaud, Y. Uchihori, Susumu Inoue, J. N. Albert, C. Blaksley, I. Kaneko, Toshiyuki Nonaka, P. Prat, K. Słomińska, C. de la Taille, Alfonso Monaco, Thomas Schanz, Shigeto Watanabe, Ke Fang, I. Fernández-Gómez, H. Prieto, R. Cremonini, B. Mot, R. Tsenov, K. Katahira, S. Ahmad, Livio Conti, N. Tone, Z. Włodarczyk, H. Lim, M. C. Maccarone, J. F. Valdés-Galicia, L. G. Tkachev, M. Dupieux, F. Dulucq, A. Pollini, Pavel Klimov, Patrick J. Reardon, Toshiki Tajima, A. Zuccaro Marchi, M. Karus, D. Monnier-Ragaigne, A. Segreto, Daisuke Yonetoku, S. Csorna, G. Vankova, H. J. Crawford, Taka Tomida, Jörn Wilms, Yukihiro Takahashi, G. Siemieniec-Oziȩbło, Yoshimasa Kurihara, O. A. Saprykin, A. Dell’Oro, Toshitaka Kajino, H. Schieler, N. Blanc, G. Masciantonio, Hitoshi Ohmori, Domenico Finco, J. Hernández Carretero, D. Supanitsky, M. Yu. Zotov, M. Unger, S. Biktemerova, Yoshiya Kawasaki, K. Higashide, C. Moretto, Tokonatsu Yamamoto, P. Galeotti, Susana Briz, G. Catalano, Hiroyuki Sagawa, C. González Alvarado, Mitsuteru Sato, Shoichi Ogio, C. Tenzer, Marco Casolino, Claudio Fornaro, M. Putis, D. Allard, A. Guzmán, A. Sobey, M. E. Bertaina, D. Campana, C. De Donato, A. Insolia, M. Kleifges, Soon-Wook Kim, Ken'ichi Nomoto, T. Sugiyama, A. Ebersoldt, Tadeusz Wibig, M. Sanz Palomino, Maxim Gonchar, Inkyu Park, Hirohiko M. Shimizu, J. Geary, S. Falk, A. Haungs, S. Piraino, Hajime Yano, N. De Simone, Y. Miyazaki, G. Roudil, L. Villaseñor, M. Suzuki, B. Harlov, Carlo Vigorito, K. Kudela, J. S. Kim, G. Sáez-Cano, Mark Christl, O. Tibolla, V. S. Morozenko, Yoshiki Tsunesada, M. Rybczyński, Lech Wiktor Piotrowski, A. Jung, T. Paul, K. Yoshida, P. Baragatti, G. Cordero, Valentina Scotti, Hajime Takami, Masaki Fukushima, G. Medina-Tanco, S. Yoshida, J. Szabelski, T. Nakamura, R. Nava, N. Sakaki, R. Matev, M. D. Rodríguez Frías, Z. Plebaniak, J. Blümer, L. Valore, Rossella Caruso, Michiyuki Chikawa, Simona Toscano, Alberto Cellino, L. R. Wiencke, K. Mase, G. Giraudo, Francesco Fenu, D. Ikeda, I. Rodríguez, F. Sarazin, Marc Weber, M. Flamini, Y. Takizawa, T. Shirahama, Francesco Isgrò, Piotr Orleanski, B. Keilhauer, Frederic Jean Ronga, Javier Licandro, T. Pierog, J. Watanabe, M. Takeda, D. Maravilla, Jianyi Yang, Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blümer, 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., Fernández Gómez, 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., González Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmán, A., Hachisu, Y., Harlov, B., Haungs, A., Hernández Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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., 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., López, 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 Ríos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Murakami, M. Nagano, 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., Orleański, 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., Prévôt, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodríguez, I., Rodríguez Frías, M. D., Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., Sáez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sánchez, S., Santangelo, A., Santiago Crúz, 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 Oziȩbło, G., Silva López, H. H., Sledd, J., Słomińska, 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., Valdés Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseñor, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., and Zuccaro Marchi, A.
Subjects: Aperture, Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Extensive air shower, JEM-EUSO, ultra-high energy cosmic rays, Cosmic ray, Astrophysics, Atmosphere, Altitude, International Space Station, Nadir, Extensive air showers, extensive air showers, Ultra-high energy cosmic ray, Physics::Atmospheric and Oceanic Physics, media_common, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Ultra-high energy cosmic rays, Astronomy and Astrophysic, Universe, Astronomía, Tilt (optics), Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, CIENCIAS NATURALES Y EXACTAS
Abstract: Designed as the first mission to explore the ultra-high energy universe from space, JEM-EUSO observes the Earth’s atmosphere at night to record the ultraviolet tracks generated by the extensive air showers. We present the expected geometrical aperture and annual exposure in the nadir and tilt modes for ultra-high energy cosmic rays observation as a function of the altitude of the International Space Station. Fil: Bertaina, M.. Istituto Nazionale di Fisica Nucleare; Italia Fil: Bobik, P.. Institute of Experimental Physics; Eslovaquia Fil: Fenu, F.. University of Tubingen; Alemania Fil: Shinozaki, K.. RIKEN; Japón Fil: Adams, J. H.. University of Alabama in Huntsville; Estados Unidos Fil: Ahmad, S.. Ecole Polytechnique; Francia Fil: Albert, J. N.. Univ Paris-Sud; Francia Fil: Allard, D.. Univ Paris Diderot; Francia Fil: Anchordoqui, L.. University of Wisconsin-Milwaukee; Estados Unidos Fil: Andreev, V.. University of California; Estados Unidos Fil: Anzalone, A.. Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo; Italia Fil: Arai, Y.. High Energy Accelerator Research Organization (KEK); Japón Fil: Asano, K.. Tokyo Institute of Technology; Japón Fil: Ave Pernas, M.. Universidad de Alcalá; España Fil: Baragatti, P.. UTIU, Dipartimento di Ingegneria; Italia Fil: Barrillon, P.. Univ Paris-Sud; Francia Fil: Batsch, T.. National Centre for Nuclear Research; Polonia Fil: Bayer, J.. University of Tubingen; Alemania Fil: Bechini, R.. Istituto Nazionale di Fisica Nucleare; Italia Fil: Belenguer, T.. Instituto Nacional de Tecnica Aeroespacial (INTA); España Fil: Bellotti, R.. Istituto Nazionale di Fisica Nucleare; Italia Fil: Belov, K.. University of California; Estados Unidos Fil: Berlind, A. A.. Vanderbilt University; Estados Unidos Fil: Biermann, P. L.. Karlsruhe Institute of Technology (KIT); Alemania Fil: Biktemerova, S.. Joint Institute for Nuclear Research; Rusia Fil: Blaksley, C.. Univ Paris Diderot; Francia Fil: Blanc, N.. Swiss Center for Electronics and Microtechnology (CSEM); Suiza Fil: Blecki, J.. Space Research Centre of the Polish Academy of Sciences (CBK); Polonia Fil: Supanitsky, Alberto Daniel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: The JEM-EUSO Collaboration.
Published: 2014

58. An exploration of hadronic interactions in blazars using multi-messenger data

Author: Andrii Neronov, C. Tchernin, Juanan Aguilar, and Teresa Montaruli
Subjects: Physics, Nuclear and High Energy Physics, Spectral index, Cosmic neutrinos, Soft photon, Astrophysics::High Energy Astrophysical Phenomena, Flux, Synchrotron radiation, Astrophysics, ddc:500.2, Hadrons, 7. Clean energy, ActiveGalacticNuclei, Neutrino detector, 13. Climate action, Neutrino, Blazar, Instrumentation, Blazars, Fermi Gamma-ray Space Telescope
Abstract: High energy photon and neutrino emissions are expected from the interactions of high energy protons with matter and/or radiation in the blazars environment. In these proceedings we use the sensitivity of the IceCube neutrino detector estimated for different neutrino spectral indices (derived in Tchernin et al. (2013) [12]) to show that already in its 40 string configuration (IC 40) the sensitivity of the IceCube neutrino telescope is already at the level of constraining the parameter space of purely hadronic scenarios of blazar activity. As a result using the full detector sensitivity those constraints should be about a factor of 3 better than what discussed here. Assuming that the ? ray flux observed by Fermi can be explained with purely hadronic interactions we estimate the expected neutrino flux from blazars based on the combination of the ? ray flux observed by Fermi with the simultaneous IC 40 observations. We consider separately the cases where the proton–proton or proton–? interactions are dominant. In both cases we set some constraints on the primary proton spectrum. In the case where pp interactions dominate the tightest constraints are set for the source 3C 454.3 for which the high energy part of the spectrum is constrained to be harder than E-2 and the cut off energy larger than 1018 eV. Alternatively in the case where the dominant channel is the interaction of the high energy protons with the soft radiation fields the magnitude of the constraints depends on the radiation field energy distribution. For the source 3C 273 the most constrained source of our sample for the p? interaction the cut off energy is constrained to be View the MathML sourceEcut?1018eV for any spectral index and for different soft photon fields including the radiation from the accretion disk (Big Blue Bump) the broad line region or the synchrotron radiation from the jet.
Published: 2014

59. Erratum to: Performances of JEM-EUSO: angular reconstruction

Author: H. Sato, A. Guzman, David B. Cline, E. G. Judd, Katsuhiko Tsuno, I. Rodríguez, Roberto Bellotti, James H. Adams, I. Kreykenbohm, M. Ave Pernas, Vladimir Andreev, K. Mase, R. Young, M. Sakata, N. Tone, S. Ahmad, Massimiliano Bonamente, Ovidiu Vaduvescu, Yoshihiko Mizumoto, Katsuaki Asano, Toshikazu Ebisuzaki, T. Shirahama, C. González Alvarado, Francesco Fenu, M. Lacombe, N. Inoue, L. del Peral, A. Franceschi, E. Parizot, F. Tajima, E. Kuznetsov, Andreas A. Berlind, Daisuke Yonetoku, Claudio Cassardo, Graciela B. Gelmini, J. N. Capdevielle, L. Santiago Crúz, M. Wille, M. Nagano Murakami, Y. Uchihori, Alexander Kusenko, J. Hernández Carretero, B. Mot, M. Di Martino, A. Marini, Y. Hachisu, G. Osteria, Satoshi Wada, T. Ogawa, Silvia Ferrarese, Francesco Isgrò, F. Dulucq, T. Tymieniecka, J. Błȩcki, H. Prieto, H. Lim, M. C. Maccarone, M. Sanz Palomino, Y. Arai, N. Tajima, T. Murakami, J. Sledd, Shigehiro Nagataki, D. Kolev, H. Ikeda, R. Cremonini, B. Keilhauer, G. Prévôt, J. A. Morales de los Ríos, J. Karczmarczyk, Yukihiro Takahashi, J. Watts, M. Unger, M. Yu. Zotov, Susana Briz, J. N. Albert, Ke Fang, Thomas Schanz, K. Słomińska, C. Pennypacker, B. Pastircak, Barbara Szabelska, T. Peter, Susumu Inoue, Piotr Orleanski, Frederic Jean Ronga, D. Ikeda, Livio Conti, Y. Yamamoto, A. Zuccaro Marchi, Valerie Connaughton, H. H. Silva Lopez, G. Distratis, Angela V. Olinto, Fernando López, Andrea Santangelo, Jörn Wilms, O. A. Saprykin, M. Nagata, Marco Casolino, Claudio Fornaro, Hanna Rothkaehl, I. Fernández-Gómez, M. Karus, Pierre Barrillon, M. Bogomilov, C. De Donato, F. Sarazin, Marc Weber, Alberto Cellino, Soon-Wook Kim, Gali Garipov, Domenico Finco, Dmitry V. Naumov, Andrii Neronov, G. Roudil, J. S. Kim, P. L. Biermann, F. Cafagna, G. Modestino, E. Joven, M. I. Panasyuk, L. R. Wiencke, V. S. Morozenko, A. Jung, M. Putis, F. Kajino, A. Sobey, Hiroyuki Sagawa, B. Harlov, Carlo Vigorito, C. Lachaud, S. Dagoret-Campagne, Yoshitaka Itow, I. Rusinov, T. Mernik, M. Flamini, G. Giraudo, K. Higashide, A. Insolia, M. Kleifges, P. Picozza, J. Lee, K. Kudela, T. Paul, K. Yoshida, M. Dupieux, Thomas J. Weiler, D. Maravilla, H. W. Park, S. Perez Cano, Y. Takizawa, C. Blaksley, T. Shibata, J. F. Valdés-Galicia, L. G. Tkachev, Y. Karadzhov, K. Shinozaki, Marcos Reyes, S. Csorna, G. Vankova, R. Nava, N. Sakaki, Maxim Gonchar, Hirohiko M. Shimizu, Z. Włodarczyk, G. Medina-Tanco, A. Dell’Oro, Toshitaka Kajino, L. Valore, S. Biktemerova, M. Rybczyński, Rossella Caruso, K. Kawai, S. Sánchez, G. Castellinic, Alfonso Monaco, Toshiyuki Nonaka, C. Moretto, P. Galeotti, Akinori Saito, Markus Roth, R. Bechini, Simona Toscano, C. Tenzer, T. Sugiyama, P. Gorodetzky, G. Cordero, J. Geary, Tadeusz Wibig, Ralph Engel, N. De Simone, Fausto Guarino, P. von Ballmoos, M. Ricci, Jianyi Yang, Taka Tomida, Shigeto Watanabe, Javier Licandro, P. Prat, A. Haungs, Yoshimasa Kurihara, Hajime Yano, S. Selmane, Lech Wiktor Piotrowski, H. Schieler, S. Piraino, Tokonatsu Yamamoto, P. Baragatti, Mitsuteru Sato, I. V. Yashin, S. Yoshida, J. Szabelski, Humberto Ibarguen Salazar, Frederic Trillaud, G. Catalano, R. Matev, T. Pierog, J. Watanabe, L. Marcelli, M. Takeda, C. De Santis, H. Tokuno, M. Suzuki, D. Campana, A. Anzalone, T. Napolitano, D. Monnier-Ragaigne, A. Segreto, Inkyu Park, T. Patzak, Y. Miyazaki, M. D. Rodríguez Frías, Mark Christl, O. Martinez, O. Tibolla, Tomás Belenguer, Patrick J. Reardon, A. Bruno, Z. Plebaniak, J. Blümer, R. Tsenov, K. Belov, C. Catalano, N. Blanc, Toshiki Tajima, G. Siemieniec-Oziȩbło, S. Falk, A. Pollini, G. Masciantonio, Hitoshi Ohmori, Pavel Klimov, Karl Mannheim, Michael S. Briggs, A. J. de Castro, Michiyuki Chikawa, Yoshiya Kawasaki, H. J. Crawford, D. Semikoz, L. Villaseñor, D. Allard, G. Sáez-Cano, M. Serra, Luis A. Anchordoqui, S. A. Sharakin, M. E. Bertaina, T. Batsch, S. Blin-Bondil, Ken'ichi Nomoto, I. Kaneko, Piero Vallania, D. Supanitsky, M. D. Sabau, J. Bayer, C. de la Taille, K. Katahira, A. Ebersoldt, Shoichi Ogio, Yoshiki Tsunesada, Hajime Takami, Masaki Fukushima, T. Nakamura, B. A. Khrenov, H. Miyamoto, J. Fujimoto, P. Bobik, and Valentina Scotti
Subjects: Physics, Particle physics, Space and Planetary Science, Astronomy and Astrophysics, Astrophysics
Abstract: The online version of the original article can be found at http://dx.doi.org/10.1007/s10686-013-9371-0 .
Published: 2015

60. Cosmic ray composition measurements and cosmic ray background free gamma-ray observations with Cherenkov telescopes

Author: Razmik Mirzoyan, Dmitri Semikoz, Ievgen Vovk, Andrii Neronov, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: air, Astrophysics::High Energy Astrophysical Phenomena, halo, FOS: Physical sciences, Cosmic ray, Astrophysics, KAMIOKANDE, Astrophysics::Cosmology and Extragalactic Astrophysics, Cherenkov counter: atmosphere, 01 natural sciences, Luminosity, law.invention, Telescope, Observatory, law, muon, 0103 physical sciences, Cherenkov: emission, luminosity, cosmic radiation: UHE, gamma ray: flux, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, Pierre Auger Observatory, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), Muon, cosmic radiation: spectrum, showers: atmosphere, 010308 nuclear & particles physics, background, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, imaging, sensitivity, Auger, observatory, 13. Climate action, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, cosmic radiation: flux
Abstract: Muon component of extensive air showers (EAS) initiated by cosmic ray particles carries information on the primary particle identity. We show that the muon content of EAS could be measured in a broad energy range from 10-100 TeV up to ultra-high-energy cosmic ray range using wide field-of-view imaging atmospheric Cherenkov telescopes observing strongly inclined or nearly horizontal EAS from the ground of from high altitude. Cherenkov emission from muons in such EAS forms a distinct component (halo or tail) of the EAS image in the telescope camera. We show that detection of the muon signal could be used to measure composition of the cosmic ray spectrum in the energy ranges of the knee, the ankle and of the Galactic-to-extragalactic transition. It could also be used to veto the cosmic ray background in gamma-ray observations. This technique provides a possibility for up to two orders of magnitude improvement of sensitivity for gamma-ray flux in the energy band above 10 PeV, compared to KASCADE-Grande, and an order-of-magnitude improvement of sensitivity in the multi-EeV energy band, compared to Pierre Auger Observatory., 11 pages, 12 figures
Published: 2016

61. FACT - First Energy Spectrum from a SiPM Cherenkov Telescope

Author: Thomas Bretz, A.-K. Overkemping, Wolfgang Rhode, Felicitas Pauss, Matthias Bergmann, G. Hughes, Matteo Balbo, Simona Toscano, Christina Hempfling, Adrian Biland, Dominik Neise, Aylin Wilbert, Werner Lustermann, Sebastian Achim Mueller, J. Freiwald, Julia Thaele, Patrick Vogler, Aleksander Paravac, Christian Bockermann, Karl Mannheim, Max Ludwig Ahnen, Dorothee Hildebrand, Roland Walter, Kai Brügge, K. Meier, Andrii Neronov, Daniela Dorner, Sabrina Einecke, Katharina Morik, Fabian Temme, Jens Buss, and Maximilian Noethe
Subjects: Telescope, Physics, Silicon photomultiplier, Cherenkov detector, law, Energy spectrum, Astronomy, Cherenkov radiation, law.invention
Abstract: The 34th International Cosmic Ray Conference : ICRC2015 : 30 July- 6 August, 2015, The Hague, The Netherlands / IUPAP The 34th International Cosmic Ray Conference, ICRC2015, The Hague, Netherlands, 30 Jul 2015 - 6 Aug 2015; Trieste, Italy : Sissa Medialab srl, Proceedings of science 236, 707 pp. (2016). doi:10.22323/1.236.0707, Published by Sissa Medialab srl, Trieste, Italy
Published: 2016

62. FACT -- Novel mirror alignment using Bokeh and enhancement of the VERITAS SCCAN alignment method

Author: Adrian Biland, Matthias Bergmann, Maximilian Noethe, Patrick Vogler, Fabian Temme, A.-K. Overkemping, Simona Toscano, Christina Hempfling, Werner Lustermann, Felicitas Pauss, Jens Buss, G. Hughes, Julia Thaele, Daniela Dorner, Andrii Neronov, Dominik Neise, Sebastian Achim Mueller, K. Meier, Matteo Balbo, Dorothee Hildebrand, Sabrina Einecke, Karl Mannheim, J. Freiwald, Max Ludwig Ahnen, Aylin Wilbert, Thomas Bretz, Aleksander Paravac, Wolfgang Rhode, and Roland Walter
Subjects: Physics, Beam diameter, Muon, Optics, Bokeh, business.industry, Resolution (electron density), Cosmic ray, Star (graph theory), business
Published: 2016

63. New concept of very high energy cosmic ray observation by wide field-of-view telescope

Author: Andrea Santangelo, Kenji Shinozaki, Andrii Neronov, and Simona Toscano
Subjects: Physics, Telescope, Acceleration, High energy, law, Astronomy, Flux, Cosmic ray, Wide field, law.invention
Published: 2016

64. The Atmospheric Science of JEM-EUSO

Author: Maria Rodriguez Frias, Pavel Klimov, Javier Licandro, Pavol Bobik, Lawrence Wiencke, Karel Kudela, José Luis Sánchez, Luis del Peral, Andrii Neronov, Mikhail Panasyuk, Lola Sabau-Graziati, Toshikazu Ebisuzaki, and James H. Adams
Subjects: Physics, Lidar, Infrared, Background analysis, Cosmic ray, Monitoring system, Light system, Space weather, Remote sensing
Abstract: An Atmospheric Monitoring System (AMS) is critical suite of instruments for JEM-EUSO whose aim is to detect Ultra-High Energy Cosmic Rays (UHECR) and (EHECR) from Space. The AMS comprises an advanced space qualified infrared camera and a LIDAR with cross checks provided by a ground-based and airborne Global Light System Stations. Moreover the Slow Data Mode of JEM-EUSO has been proven crucial for the UV background analysis by comparing the UV and IR images. It will also contribute to the investigation of atmospheric effects seen in the data from the GLS or even to our understanding of Space Weather.
Published: 2016

65. Camera calibration strategy of the SST-1M prototype of the Cherenokov Telescope Array

Author: Etienne Lyard, Enrico Junior Schioppa, M. Heller, Andrii Neronov, and Elisa Prandini
Subjects: Physics, Pixel, Physics::Instrumentation and Detectors, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Cherenkov Telescope Array, law.invention, Telescope, Optics, Silicon photomultiplier, law, Calibration, Focus (optics), business, Cherenkov radiation, Camera resectioning
Abstract: The SST-1M telescope is one of the prototypes under construction proposed to be part of the future Cherenkov Telescope Array. It uses a standard Davis-Cotton design for the optics and telescope structure, with a dish diameter of 4 meters and a large field-of-view of 9 degrees. The innovative camera design is composed of a photo-detection plane with 1296 pixels including entrance window, light concentrators, Silicon Photomultipliers (SiPMs), and pre-amplifier stages together with a fully digital readout and trigger electronics, DigiCam. In this contribution we give a general description of the analysis chain designed for the SST-1M prototype. In particular we focus on the calibration strategy used to convert the SiPM signals registered by DigiCam to the quantities needed for Cherenkov image analysis. The calibration is based on an online feedback system to stabilize the gain of the SiPMs, as well as dedicated events (dark count, pedestal, and light flasher events) to be taken during the normal operation of the prototype.
Published: 2016

66. Bokeh mirror alignment for Cherenkov telescopes

Author: A. Shukla, Michael Blank, Dominik Neise, Dorothee Hildebrand, Sabrina Einecke, Jens Buss, Christina Hempfling, J. Adam, K. Bruegge, Max Ludwig Ahnen, Daniela Dorner, Andrii Neronov, Thomas Bretz, Fabian Temme, Wolfgang Rhode, Anton Dmytriiev, Matteo Balbo, Adrian Biland, Karl Mannheim, Aleksander Paravac, Julia Thaele, Lena Linhoff, Roland Walter, Dominik Baack, Maximilian Noethe, Matthias Bergmann, Felicitas Pauss, Sebastian Achim Mueller, and G. Hughes
Subjects: Physics, Measurement method, Reflector (photography), Bokeh, 010308 nuclear & particles physics, business.industry, IACT, Cherenkov Telescope Array, 01 natural sciences, Optics, 0103 physical sciences, business, 010303 astronomy & astrophysics, Cherenkov radiation
Abstract: Segmented imaging reflectors are a great choice for Imaging Atmospheric Cherenkov Telescopes (IACTs). However, the alignment of the individual mirror facets is challenging. We align a segmented reflector by observing and optimizing its Bokeh function. Bokeh alignment can already be done with very little resources and little preparation time. Further, Bokeh alignment can be done anytime, even during the day. We present a first usage of Bokeh alignment on FACT, a 4m IACT on Canary Island La Palma, Spain and further a first Bokeh alignment test on the CTA MST IACT prototype in Brelin Adlershof.
Published: 2016

67. FACT: status and experience from four years of operation of the first G-APD Cherenkov Telescope

Author: Daniela Dorner, Andrii Neronov, Dominik Neise, Thomas Bretz, Kai Brügge, Karl Mannheim, Michael Blank, Anton Dmytriiev, Fabian Temme, Adrian Biland, Max Nöthe, Matthias Bergmann, Wolfgang Rhode, Julia Thaele, Matteo Balbo, J. Buss, Lena Linhoff, Felicitas Pauss, Gareth Hughes, Sabrina Einecke, Dominik Baack, Dorothee Hildebrand, Jablonski Adam, Sebastian Müller, Christina Hempfling, Max Ludwig Ahnen, A. Shukla, Aleksander Paravac, and Roland Walter
Subjects: Physics, Pixel, 010308 nuclear & particles physics, business.industry, Electrical engineering, Avalanche photodiode, 01 natural sciences, law.invention, Telescope, Silicon photomultiplier, Optics, law, 0103 physical sciences, Calibration, Electronics, business, Energy source, 010303 astronomy & astrophysics, Cherenkov radiation
Abstract: The First G-APD Cherenkov Telescope (FACT) is pioneering the usage of novel Geiger-mode operated Avalanche Photo Diodes (G-APD, nowadays usually called SiPM) for Cherenkov Telescopes. The camera consists of 1440 pixels with dedicated electronics operated at 2 GHz and is installed on a refurbished telescope with a mirror area of ≈ 9:5 m2 at the Canary Island La Palma. The camera was installed in October 2011, and data are taken almost every night since then. The very stable and reliable operation allows to operate FACT from remote without the need of a data taking crew on-site. Over the years, operation became more and more automatic, and the next step will be to switch to fully automatic operation. This results in a very high data taking efficiency. The operation of FACT allows monitoring the long-term behavior of few variable extra-galactic very-high energy sources with unprecedented sampling density as well as testing the behavior of the sensors under harsh conditions. Despite operating also under strong moonlight conditions and therefore collecting far more signals than during dark nights, the G-APDs show no change in their performance or any indication for ageing. Understanding the behavior of the G-APDs under all the varying conditions allows to operate FACT without the need of any external calibration device. The properties of the sensors themselves allow for a high precision self-calibration of the camera.
Published: 2016

68. Decaying dark matter search with NuSTAR deep sky observations

Author: Denys Malyshev, Andrii Neronov, and Dominique Eckert
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Sterile neutrino, 010308 nuclear & particles physics, Milky Way, Hot dark matter, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Scalar field dark matter, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Dark matter halo, Baryonic dark matter, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: We present the results of the search for decaying dark matter with particle mass in the 6--40 keV range with NuSTAR deep observations of COSMOS and ECDFS empty sky fields. We show that the main contribution to the decaying dark matter signal from the Milky Way galaxy comes through the aperture of the NuSTAR detector, rather than through the focusing optics. The high sensitivity of the NuSTAR detector, combined with the large aperture and large exposure times of the two observation fields, allows us to improve previously existing constraints on the dark matter decay time by up to an order of magnitude in the mass range 10--30 keV. In the particular case of the $\ensuremath{\nu}\mathrm{MSM}$ sterile neutrino dark matter, our constraints impose an upper bound $ml20\text{ }\text{ }\mathrm{keV}$ on the dark matter particle mass. We report detection of four unidentified spectral lines (including the line at 3.51 keV) in our data set. These line detections are either due to the systematic effects (uncertainties of calibrations of the NuSTAR detectors) or have an astrophysical origin. We discuss different possibilities for testing the nature of the detected lines.
Published: 2016

69. LIC and LID considerations in the design and implementation of the MEMS laser pointing mechanism for the EUSO UV laser altimeter

Author: Enrico Bozzo, Arno Hoogerwerf, Clemens Heese, Vincent Revol, Alessandra Ciapponi, R. Stanley, Thomas Burch, Andrii Neronov, and Nicholas Lan
Subjects: Microelectromechanical systems, Physics, Photon, business.industry, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Night sky, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Laser, Universe, law.invention, Telescope, law, Altimeter, Ultra-high-energy cosmic ray, Aerospace engineering, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common
Abstract: The EUSO (Extreme Universe Space Observatory) project is developing a new mission concept for the scientific research of Ultra High Energy Cosmic Rays (UHECRs) from space. The EUSO wide-field telescope will look down from space onto the Earth night sky to detect UV photons emitted from air showers generated by UHECRs in our atmosphere. In this article we concentrate on the mitigation strategies agreed so far, and in particular on the implementation of a careful early selection and testing of subsystem materials (including optics), design and interfaces of the subsystem and an optimization of the instrument operational concept., Comment: Proceedings of the SPIE, 2016, Paper No. 9983-50
Published: 2016

70. Sensitivity of a proposed space-based Cerenkov astrophysical-neutrino telescope (CHANT)

Author: James H. Adams, Angela V. Olinto, Dmitri Semikoz, Luis A. Anchordoqui, Andrii Neronov, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: air, Physics::Instrumentation and Detectors, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Cosmic ray, Astrophysics, cosmic radiation: interaction, Cherenkov counter: atmosphere, Space (mathematics), 01 natural sciences, neutrino: flux, horizon, law.invention, Telescope, law, 0103 physical sciences, surface, cosmic radiation: UHE, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Cherenkov radiation, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Range (particle radiation), showers: atmosphere, 010308 nuclear & particles physics, Horizon, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, Astronomy, sensitivity, neutrino: detector, 13. Climate action, Physics::Space Physics, High Energy Physics::Experiment, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Neutrinos with energies in the PeV to EeV range produce upgoing extensive air showers when they interact underground close enough to the surface of the Earth. We study the possibility for detection of such showers with a system of very wide field-of-view imaging atmospheric Cherenkov telescopes, named CHANT for CHerenkov from Astrophysical Neutrinos Telescope, pointing down to a strip below the Earth's horizon from space. We find that CHANT provides sufficient sensitivity for the study of the astrophysical neutrino flux in a wide energy range, from 10 PeV to 10 EeV. A space-based CHANT system can discover and study in detail the cosmogenic neutrino flux originating from interactions of ultra-high-energy cosmic rays in the intergalactic medium., 15 pages, 8 figures, accepted to Phys. Rev. D
Published: 2016

71. Abundances of 59Co and 59Ni in the cosmic ray flux

Author: Andrii Neronov and G. Meynet
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Cosmic ray, Superbubble, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Nucleosynthesis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, Stellar rotation, Astronomy and Astrophysics, Supernova, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Two main hypotheses for the origin of Galactic cosmic rays are the "supernova" and "superbubble" origin hypotheses. We analyse the evidence for the superbubble hypothesis provided by the measurements of the relativive abundances of isotopes of cobalt and nickel in the cosmic ray flux. We compare the measured upper limit on the abundance of 59Ni in the cosmic ray flux with the 59Ni abundance predictions of the up-to-date stellar evolution models. Non-detection of 59Ni in the cosmic ray flux has previously been attributed to a large time delay of the order of 1e5 yr between the moment of supernova explosion and the onset of particle acceleration process. This large time delay was considered as an argument in favour of the "superbubble" scenario. We show that the recent calculation of the 59Ni yield of massive stars, which takes into account the initial mass range up to 120 solar masses and includes stellar rotation, results in prediction of low 59Ni abundance relative to its decay product 59Co. The predicted abundance is consistent with the upper bound on 59Ni abundance in the cosmic ray flux for the supernova parameters assumed. This result removes the necessity of decay of 59Ni in the time interval between the supernova explosion and the onset of acceleration process and restores the consistency of measurements of 59Ni / 59Co abundances with the "supernova" hypothesis of the CR origin., 6 pages, 3 figures, accepted to A&A
Published: 2016

72. Bokeh Mirror Alignment for Cherenkov Telescopes

Author: Julia Thaele, Patrick Vogler, Dominik Neise, Michael Blank, Felicitas Pauss, Matteo Balbo, Max Ludwig Ahnen, K. Bruegge, A. Shukla, Daniela Dorner, Matthias Bergmann, G. Hughes, Aylin Wilbert, Sebastian Achim Mueller, Adrian Biland, Dorothee Hildebrand, Christina Hempfling, M. Domke, Simona Toscano, Andrii Neronov, A.-K. Overkemping, Thomas Bretz, Wolfgang Rhode, Werner Lustermann, Roland Walter, Dominik Baack, Maximilian Noethe, Sabrina Einecke, Jens Buss, Karl Mannheim, Fabian Temme, and Aleksander Paravac
Subjects: Point spread function, Bokeh, Aperture, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 01 natural sciences, law.invention, Telescope, Optics, law, 0103 physical sciences, Focal length, Image sensor, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Computer Science::Computer Vision and Pattern Recognition, Focus (optics), business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Imaging Atmospheric Cherenkov Telescopes (IACTs) need imaging optics with large apertures and high image intensities to map the faint Cherenkov light emitted from cosmic ray air showers onto their image sensors. Segmented reflectors fulfill these needs, and composed from mass production mirror facets they are inexpensive and lightweight. However, as the overall image is a superposition of the individual facet images, alignment remains a challenge. Here we present a simple, yet extendable method, to align a segmented reflector using its Bokeh. Bokeh alignment does not need a star or good weather nights but can be done even during daytime. Bokeh alignment optimizes the facet orientations by comparing the segmented reflectors Bokeh to a predefined template. The optimal Bokeh template is highly constricted by the reflector's aperture and is easy accessible. The Bokeh is observed using the out of focus image of a near by point like light source in a distance of about 10 focal lengths. We introduce Bokeh alignment on segmented reflectors and demonstrate it on the First Geiger-mode Avalanche Cherenkov Telescope (FACT) on La Palma, Spain., Comment: accepted for publication in Astroparticle Physics
Published: 2016
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73. FACT - Calibration of Imaging Atmospheric Cerenkov Telescopes with Muon Rings

Author: Adrian Biland, Wolfgang Rhode, A.-K. Overkemping, Jens Buss, Felicitas Pauss, Werner Lustermann, Christina Hempfling, Fabian Temme, Daniela Dorner, Aylin Wilbert, Aleksander Paravac, Max Ludwig Ahnen, Andrii Neronov, Dominik Neise, Sabrina Einecke, Karl Mannheim, Patrick Vogler, Matteo Balbo, Maximilian Noethe, Gareth Hughes, Sebastian Achim Mueller, Simona Toscano, Roland Walter, Christian Bockermann, J. Freiwald, Kai Brügge, K. Meier, Katharina Morik, Matthias Bergmann, Dorothee Hildebrand, Julia Thaele, and Thomas Bretz
Subjects: Nuclear physics, Physics, Muon, Calibration, Time resolution, Astrophysics
Abstract: The 34th International Cosmic Ray Conference : ICRC2015 : 30 July- 6 August, 2015, The Hague, The Netherlands / IUPAP The 34th International Cosmic Ray Conference, ICRC2015, The Hague, Netherlands, 30 Jul 2015 - 6 Aug 2015; Trieste, Italy : Sissa Medialab srl, Proceedings of science 236, 733 pp. (2016). doi:10.22323/1.236.0733, Published by Sissa Medialab srl, Trieste, Italy
Published: 2016
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74. Neutrinos from Extra-Large Hadron Collider in the Milky Way

Author: Andrii Neronov, D.V. Semikoz, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics, 7. Clean energy, 01 natural sciences, IceCube, High Energy Physics - Phenomenology (hep-ph), Ultra-high-energy cosmic ray, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, cosmic radiation: spectrum, p: spectrum, Astrophysics::Instrumentation and Methods for Astrophysics, acceleration: shock waves, High Energy Physics - Phenomenology, p: UHE, neutrino: detector, Neutrino detector, cosmic radiation: galaxy, slope, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, magnetic field: galaxy, cosmic ray physics, nucleus: cosmic radiation, gamma ray: energy spectrum, neutrino astronomy, neutrino: spectrum, gamma-ray astronomy, 0103 physical sciences, gamma ray: detector, cosmic radiation: injection, 010306 general physics, Astrophysics::Galaxy Astrophysics, turbulence, Astronomy, Astronomy and Astrophysics, Galaxy, 13. Climate action, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], spectral, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], hadron, Neutrino astronomy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], multi-messenger astronomy, Fermi Gamma-ray Space Telescope
Abstract: Neutrino telescope IceCube has recently discovered astrophysical neutrinos with energies in the TeV-PeV range. We use the data of Fermi gamma-ray telescope to demonstrate that the neutrino signal has significant contribution from the Milky Way galaxy. Matching the gamma-ray and neutrino spectra we find that TeV-PeV Galactic cosmic rays form a powerlaw spectrum with the slope p~2.45. This spectral slope is consistent with the average cosmic ray spectrum in the disks of the Milky Way and Large Magellanic Cloud galaxies. It is also consistent with the theoretical model of cosmic ray injection by diffusive shock acceleration followed by escape through the Galactic magnetic field with Kolmogorov turbulence. The locally observed TeV-PeV cosmic ray proton spectrum is softer than the average Galactic cosmic ray spectrum. This could be readily explained by variability of injection of cosmic rays in the local interstellar medium over the past 1e7 yr and discreetness of the cosmic ray source distribution., 6 pages 3 figures, accepted to Astroparticle Physics
Published: 2016

75. Front-end and slow control electronics for large area SiPMs used for the single mirror Small Size Telescope (SST-1M) of the Cherenkov Telescope Array (CTA)

Author: Etienne Lyard, Jerzy Michalowski, M. Heller, A. Marszałek, V. Sliusar, M. Sowiński, Frank Raphael Cadoux, M. Więcek, A. Christov, I. Troyano Pujadas, Jerzy Kasperek, Marek Stodulski, Leszek Bogacz, Simona Toscano, Pawel Rajda, Petr Schovanek, Michał Ostrowski, M. Stodulska, J. Blocki, P. Paśko, B. Idźkowski, A. Frankowski, Miroslav Pech, Andrii Neronov, Teresa Montaruli, Karol Seweryn, Łukasz Stawarz, K. Lalik, W. Bilnik, Ł. Grudniki, Dusan Mandat, Marek Jamrozy, M. Grudzińska, K. Skowron, E. jr. Schioppa, A. Porcelli, Jacek Niemiec, J. Borkowski, Michal Dyrda, E. Prandini, P. Żychowski, Mateusz Janiak, K. Zietara, Tomasz Bulik, E. Mach, R. Walter, Mohamed Rameez, A. Zagdański, R. Moderski, J. A. Aguilar, Yannick Favre, M. Curyło, D. della Volpe, Aguilar, J. A., Bilnik, W., Borkowski, J., Cadoux, F., Christov, A., Della Volpe, D., Favre, Y., Heller, M., Kasperek, J., Lyard, E., Marszalek, A., Moderski, R., Montaruli, T., Porcelli, A., Prandini, E., Rajda, P., Rameez, M., Schioppa, E. J., Troyano Pujadas, I., Zitara, K., Blocki, J., Bogacz, L., Bulik, T., Curyo, M., Dyrda, M., Frankowski, A., Grudniki, A., Grudzinska, M., Idkowski, B., Jamrozy, M., Janiak, M., Lalik, K., Mach, E., Mandat, D., Michalowski, J., Neronov, A., Niemiec, J., Ostrowski, M., Pako, P., Pech, M., Schovanek, P., Seweryn, K., Skowron, K., Sliusar, V., Sowinski, M., Stawarz, A., Stodulska, M., Stodulski, M., Toscano, S., Walter, R., Wicek, M., Zagdaski, A., and Zychowski, P.
Subjects: Physics::Instrumentation and Detectors, Preamplifier, SiPM, Astrophysics::High Energy Astrophysical Phenomena, compensation loop, SST-1M, 01 natural sciences, 7. Clean energy, law.invention, CTA, front-end, preamplifier, slow-control, Telescope, Front and back ends, Optics, Silicon photomultiplier, law, 0103 physical sciences, 010303 astronomy & astrophysics, Cherenkov radiation, Physics, 010308 nuclear & particles physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Active surface, Cherenkov Telescope Array, Resistor, business
Abstract: The single mirror Small Size Telescope (SST-1M) project proposes a design among others for the smallest type of telescopes (SST), that will compose the south observatory of the Cherenkov Telescope Array (CTA). The SST camera collecting the Cherenkov light resulting from very high energy gamma-ray interactions in the atmosphere proposes to use Silicon PhotoMultipliers (SiPM). The SST-1M design has led to the use of unique pixel shape and size that required a dedicated development by the University of Geneva and Hamamatsu. An active surface of ~94 mm2 and a resulting total capacitance of ~3.4 nF combined with the stringent requirements of the CTA project on timing and charge resolution have led the University of Geneva to develop a custom preamplifier stage and slow-control system. The design and performance of the tailor made preamplifier stage and of the slow control electronics will be briefly described. The bias circuit of the sensor contains a resistor meant to prevent the sensor from drawing high current. However this resistor also introduces a voltage drop at the sensor input impacting the stability of its operation. A model has been developed in order to derive the parameters needed to account for it at the data analysis level. A solution based on the SST-1M front-end and digital readout is proposed to compensate for the voltage drop at the sensor cathode.
Published: 2016

76. Normalized and Asynchronous Mirror Alignment for Cherenkov Telescopes

Author: Aylin Wilbert, A. Shukla, Werner Lustermann, Dominik Neise, Adrian Biland, Patrick Vogler, Jens Buss, G. Hughes, Andrii Neronov, Fabian Temme, K. Bruegge, Max Ludwig Ahnen, Simona Toscano, Sebastian Achim Mueller, Roland Walter, Karl Mannheim, A.-K. Overkemping, Matthias Bergmann, Michael Blank, Sabrina Einecke, Dominik Baack, Christina Hempfling, M. Domke, Maximilian Noethe, Thomas Bretz, Matteo Balbo, Daniela Dorner, Wolfgang Rhode, Felicitas Pauss, Dorothee Hildebrand, Aleksander Paravac, and Julia Thaele
Subjects: Point spread function, Facet (geometry), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Tracking (particle physics), 01 natural sciences, law.invention, Telescope, Optics, law, 0103 physical sciences, Image sensor, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Beam diameter, 010308 nuclear & particles physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Reflection (physics), business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Imaging Atmospheric Cherenkov Telescopes (IACTs) need imaging optics with large apertures and high image intensities to map the faint Cherenkov light emitted from cosmic ray air showers onto their image sensors. Segmented reflectors fulfill these needs, and as they are composed from mass production mirror facets they are inexpensive and lightweight. However, as the overall image is a superposition of the individual facet images, alignment is a challenge. Here we present a computer vision based star tracking alignment method, which also works for limited or changing star light visibility. Our method normalizes the mirror facet reflection intensities to become independent of the reference star's intensity or the cloud coverage. Using two CCD cameras, our method records the mirror facet orientations asynchronously of the telescope drive system, and thus makes the method easy to integrate into existing telescopes. It can be combined with remote facet actuation, but does not require one to work. Furthermore, it can reconstruct all individual mirror facet point spread functions without moving any mirror. We present alignment results on the 4 meter First Geiger-mode Avalanche Cherenkov Telescope (FACT)., Comment: accepted for publication in Astroparticle Physics
Published: 2016
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77. The single mirror small size telescope (SST-1M) of the Cherenkov Telescope Array

Author: Miroslav Pech, K. Zietara, Mohamed Rameez, E. Mach, Teresa Montaruli, A. Zagdański, E. Prandini, B. Idźkowski, W. Bilnik, A. Christov, M. Heller, Frank Raphael Cadoux, A. Frankowski, Marek Jamrozy, Mateusz Janiak, Jacek Niemiec, Jerzy Kasperek, J. Blocki, Marek Stodulski, M. Stodulska, Etienne Lyard, Simona Toscano, Lukasz Stawarz, Michał Ostrowski, Dusan Mandat, R. Moderski, A. Porcelli, K. Skowron, E. jr. Schioppa, A. Marszałek, K. Lalik, Karol Seweryn, Juanan Aguilar, Jerzy Michalowski, R. Walter, I. Troyano Pujadas, D. della Volpe, M. Wiȩcek, Yannick Favre, P. Paśko, J. Borkowski, Leszek Bogacz, Pawel Rajda, Vitalii Sliusar, Andrii Neronov, Petr Schovanek, M. Grudzińska, Tomasz Bulik, Aguilar, J. A., Bilnik, W., Borkowski, J., Cadoux, F., Christov, A., Dellavolpe, D., Favre, Y., Heller, M., Kasperek, J., Lyard, E., Marszalek, A., Moderski, R., Montaruli, T., Porcelli, A., Prandini, E., Rajda, P., Rameez, M., Schioppa, E., Troyano Pujadas, I., Zietara, K., Locki, J. B., Bogacz, L., Bulik, T., Frankowski, A., Grudzinska, M., Idzkowski, B., Jamrozy, M., Janiak, M., Lalik, K., Mach, E., Mandat, D., Michalowski, J., Neronov, A., Niemiec, J., Ostrowski, M., Pasko, P., Pech, M., Schovanek, P., Seweryn, K., Skowron, K., Sliusar, V., Stawarz, L., Stodulska, M., Stodulski, M., Toscano, S., Walter, R., Wiecek, M., and Zagdanski, A.
Subjects: Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, SiPM, Field of view, SST-1M, 01 natural sciences, law.invention, Telescope, Optics, Silicon photomultiplier, law, 0103 physical sciences, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, Cherenkov radiation, Physics, CTA, 010308 nuclear & particles physics, business.industry, Hexagonal crystal system, IACT, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Cherenkov Telescope Array, business
Abstract: The Small Size Telescope with Single Mirror (SST-1M) is one of the proposed types of Small Size Telescopes (SST) for the Cherenkov Telescope Array (CTA). The CTA south array will be composed of about 100 telescopes, out of which about 70 are of SST class, which are optimized for the detection of gamma rays in the energy range from 5 TeV to 300 TeV. The SST-1M implements a Davies-Cotton optics with a 4 m dish diameter with a field of view of 9°. The Cherenkov light produced in atmospheric showers is focused onto a 88 cm wide hexagonal photo-detection plane, composed of 1296 custom designed large area hexagonal silicon photomultipliers (SiPM) and a fully digital readout and trigger system. The SST-1M camera has been designed to provide high performance in a robust as well as compact and lightweight design. In this contribution, we review the different steps that led to the realization of the telescope prototype and its innovative camera.
Published: 2016

78. FACT-Tools: Streamed Real-Time Data Analysis

Author: Kai Brügge, K. Meier, G. Hughes, Thomas Bretz, A.-K. Overkemping, J. Freiwald, Daniela Dorner, Maximilian Nöthe, Aylin Wilbert, Wolfgang Rhode, Fabian Temme, Werner Lustermann, Adrian Biland, Andrii Neronov, Christian Bockermann, Roland Walter, Felicitas Pauss, Julia Thaele, Katharina Morik, Jens Buss, Sabrina Einecke, Dorothee Hildebrand, Matthias Bergmann, Matteo Balbo, Dominik Neise, Aleksander Paravac, Sebastian Müller, Max Ludwig Ahnen, Simona Toscano, Karl Mannheim, Patrick Vogler, and Christina Hempfling
Subjects: Computer science, Real-time computing, Real-time data
Abstract: The 34th International Cosmic Ray Conference : ICRC2015 : 30 July- 6 August, 2015, The Hague, The Netherlands / IUPAP The 34th International Cosmic Ray Conference, ICRC2015, The Hague, Netherlands, 30 Jul 2015 - 6 Aug 2015; Trieste, Italy : Sissa Medialab srl, Proceedings of science 236, 865 pp. (2016). doi:10.22323/1.236.0865, Published by Sissa Medialab srl, Trieste, Italy
Published: 2016
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79. The front-end electronics and slow control of large area SiPM for the SST-1M camera developed for the CTA experiment

Author: Yannick Favre, Marek Stodulski, M. Heller, M. Wiȩcek, I. Troyano Pujadas, A. Christov, Juanan Aguilar, A. Porcelli, Łukasz Stawarz, D. della Volpe, Jerzy Michalowski, Etienne Lyard, M. Janiak, Rafał Moderski, Michal Dyrda, A. Frankowski, M. Stodulska, Mohamed Rameez, B. Idźkowski, M. Curyło, A. Zagdański, Jacek Niemiec, J. Blocki, M. Sowiński, K. Ziȩtara, Tomasz Bulik, Miroslav Pech, Leszek Bogacz, Jerzy Kasperek, P. Żychowski, R. Walter, Dusan Mandat, Frank Raphael Cadoux, Teresa Montaruli, Vitalii Sliusar, Pawel Rajda, P. Paśsko, Petr Schovanek, K. Skowron, Enrico Junior Schioppa, Karol Seweryn, E. Mach, Ł. Grudniki, Andrii Neronov, J. Borkowski, M. Grudzińska, W. Bilnik, Michał Ostrowski, Marek Jamrozy, Elisa Prandini, K. Lalik, A. Marszałek, Simona Toscano, Aguilar, J. A., Bilnik, W., Borkowski, J., Cadoux, F., Christov, A., Della Volpe, D., Favre, Y., Heller, M., Kasperek, J., Lyard, E., Marszalek, A., Moderski, R., Montaruli, T., Porcelli, A., Prandini, E., Rajda, P., Rameez, M., Schioppa, E., Troyano Pujadas, I., Zitara, K., Blocki, J., Bogacz, L., Bulik, T., Curylo, M., Dyrda, M., Frankowski, A., Grudniki, L., Grudzinska, M., Idzkowski, B., Jamrozy, M., Janiak, M., Lalik, K., Mach, E., Mandat, D., Michalowski, J., Neronov, A., Niemiec, J., Ostrowski, M., Passko, P., Pech, M., Schovanek, P., Seweryn, K., Skowron, K., Sliusar, V., Sowinski, M., Stawarz, L., Stodulska, M., Stodulski, M., Toscano, S., Walter, R., Wicek, M., Zagdanski, A., and Zychowski, P.
Subjects: Physics, Slow-control, Nuclear and High Energy Physics, Pixel, CTA, 010308 nuclear & particles physics, Preamplifier, SiPM, G-APD, Cherenkov Telescope Array, 01 natural sciences, Electronic circuit simulation, law.invention, Front and back ends, Telescope, compensation, preamplifier, front-end, Silicon photomultiplier, law, 0103 physical sciences, Electronic engineering, Electronics, 010306 general physics, Instrumentation
Abstract: The single mirror Small Size Telescope (SST-1M) is one of the proposed designs for the smallest type of telescopes, SSTs that will compose the Cherenkov Telescope Array (CTA). The SST-1M camera will use Silicon PhotoMultipliers (SiPM) which are nowadays commonly used in High Energy Physics experiments and many imaging applications. However the unique pixel shape and size have required a dedicated development by the University of Geneva and Hamamatsu. The resulting sensor has a surface of ∼94 mm2 and a total capacitance of ∼3.4 nF. These unique characteristics, combined with the stringent requirements of the CTA project on timing and charge resolution have led the University of Geneva to develop custom front-end electronics. The preamplifier stage has been tailored in order to optimize the signal shape using measurement campaigns and electronic simulation of the sensor. A dedicated trans-impedance pre-amplifier topology is used resulting in a power consumption of 400 mW per pixel and a pulse width 30 ns . The measurements that have led to the choice of the different components and the resulting performance are detailed in this paper. The slow control electronics was designed to provide the bias voltage with 6.7 mV precision and to correct for temperature variation with a forward feedback compensation with 0.17 °C resolution. It is fully configurable and can be monitored using CANbus interface. The architecture and the characterization of the various elements are presented.
Published: 2016

80. Galactic and extragalactic contributions to the astrophysical muon neutrino signal

Author: Dmitry V. Semikoz, Andrii Neronov, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Solar neutrino, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, anisotropy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, neutrino: flux, IceCube, Galactic halo, galaxy: halo, muon, 0103 physical sciences, Muon neutrino, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Solar neutrino problem, Neutrino detector, gamma ray, 13. Climate action, spectral, Measurements of neutrino speed, High Energy Physics::Experiment, Neutrino, Neutrino astronomy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract: Spectral and anisotropy properties of IceCube astrophysical neutrino signal reveal an evidence for a significant Galactic contribution to the neutrino flux in Southern hemisphere. We check if the Galactic contribution is detectable in the astrophysical muon neutrino flux observed from a low positive declinations region of the Northern sky. Estimating the Galactic neutrino flux in this part of the sky from gamma-ray and Southern sky neutrino data, we find that the Northern sky astrophysical muon neutrino signal shows an excess over the Galactic flux. This points to the presence of an additional hard spectrum (extragalactic or large scale Galactic halo) component of astrophysical neutrino flux. We show that the Galactic flux component should still be detectable in the muon neutrino data in a decade long IceCube exposure., Comment: 4 pages, 3 figures
Published: 2016
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81. Prospect on intergalactic magnetic field measurements with gamma-ray instruments

Author: Lisa Fallon, Jim Hinton, Catherine Boisson, Helene Sol, Susumu Inoue, Elisabete M. de Gouveia Dal Pino, Andrii Neronov, Richard White, Henric Krawczynski, and Andreas Zech
Subjects: Physics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Intergalactic travel, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gamma-ray astronomy, Magnetic field
Abstract: Observing high-energy gamma-rays from Active Galactic Nuclei (AGN) offers a unique potential to probe extremely tiny values of the intergalactic magnetic field (IGMF), a long standing question of astrophysics, astroparticle physics and cosmology. Very high energy (VHE) photons from blazars propagating along the line of sight interact with the extragalactic background light (EBL) and produce e+e− pairs. Through inverse-Compton interaction, mainly on the cosmic microwave background (CMB), these pairs generate secondary GeV-TeV components accompanying the primary VHE signal. Such secondary components would be detected in the gamma-ray range as delayed “pair echos” for very weak IGMF (B < 10−16G), while they should result in a spatially extended gamma-ray emission around the source for higher IGMF values (B > 10−16G). Coordinated observations with space (i.e. Fermi) and ground-based gamma-ray instruments, such as the present Cherenkov experiments H.E.S.S., MAGIC and VERITAS, the future Cherenkov Telescope Array (CTA) Observatory, and the wide-field detectors such as HAWC and LHAASO, should allow to analyze and finally detect such echos, extended emission or pair halos, and to further characterize the IGMF.
Published: 2012

82. Searching for decaying dark matter in deep XMM-Newton observation of the Draco dwarf spheroidal

Author: Esra Bulbul, Oleg Ruchayskiy, Andrii Neronov, Alexey Boyarsky, Jeroen Franse, Dominique Eckert, Maxim Markevitch, Dmytro Iakubovskyi, and Denys Malyshev
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Dwarf galaxy problem, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, 01 natural sciences, dark matter, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Hot dark matter, Astronomy, Astronomy and Astrophysics, galaxies: dwarf, Galaxy, Dwarf spheroidal galaxy, Dark matter halo, High Energy Physics - Phenomenology, Space and Planetary Science, Dark galaxy, Astrophysics - High Energy Astrophysical Phenomena, line: identification
Abstract: We present results of a search for the 3.5 keV emission line in our recent very long (~ 1.4 Ms) XMM-Newton observation of the Draco dwarf spheroidal galaxy. The astrophysical X-ray emission from such dark matter-dominated galaxies is faint, thus they provide a test for the dark matter origin of the 3.5 keV line previously detected in other massive, but X-ray bright objects, such as galaxies and galaxy clusters. We do not detect a statistically significant emission line from Draco; this constrains the lifetime of a decaying dark matter particle to tau > (7-9) x 10^27 s at 95% CL (combining all three XMM-Newton cameras; the interval corresponds to the uncertainty of the dark matter column density in the direction of Draco). The PN camera, which has the highest sensitivity of the three, does show a positive spectral residual (above the carefully modeled continuum) at E = 3.54 +/- 0.06 keV with a 2.3 sigma significance. The two MOS cameras show less-significant or no positive deviations, consistently within 1 sigma with PN. Our Draco limit on tau is consistent with previous detections in the stacked galaxy clusters, M31 and the Galactic Center within their 1-2 sigma uncertainties, but is inconsistent with the high signal from the core of the Perseus cluster (which has itself been inconsistent with the rest of the detections). We conclude that this Draco observation does not exclude the dark matter interpretation of the 3.5 keV line in those objects., 10 pages, 5 figures. Accepted by MNRAS
Published: 2015

83. Studying the long-time variability of the Seyfert 2 galaxy NGC 4388 with INTEGRAL and Swift

Author: Volker Beckmann, Simona Soldi, Andrii Neronov, and E. V. Fedorova
Subjects: Physics, Spectral shape analysis, Active galactic nucleus, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Power law, Galaxy, Exponential function, law.invention, Telescope, Space and Planetary Science, law, 0103 physical sciences, Spectral slope, Basso continuo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We present analysis results on the Seyfert 2 galaxy NGC 4388 based on 6 yr of INTEGRAL data combined with Swift/Burst Alert Telescope survey and Swift/X-Ray Telescope pointed observations. These data, taken from 2003 to 2009, allow us to study the broad-band properties of this active galactic nucleus in the 0.3–300 keV energy range. The continuum emission of NGC 4388 is well represented by an absorbed power-law model with exponential cut-off at high energies and an upper limit on the reflection component of R < 0.5. We find slow strong variations of the hard X-ray emission, indicating both flux and spectral slope changes on the 3–6 months time-scale. In comparison with previous results on NGC 4388, the source shows a complex variability behaviour, i.e. the spectral shape and the 20–60 keV flux vary independently.
Published: 2011

84. 2003–2005INTEGRALandXMM-Newtonobservations of 3C 273

Author: M. Stuhlinger, Volker Beckmann, K. L. Page, Simona Soldi, Thierry J.-L. Courvoisier, Maria Chernyakova, Andrii Neronov, Ruediger Staubert, Ian M. McHardy, P. Lubinski, Marc Türler, R. Walter, ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], INTEGRAL Science Data Center (ISDC), Geneva Observatory, University of Geneva [Switzerland]-University of Geneva [Switzerland], NASA Goddard Space Flight Center (GSFC), Department of Physics and Astronomy [Leicester], University of Leicester, Agence Spatiale Européenne (ESA), European Space Agency (ESA), Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, School of Physics and Astronomy [Southampton], and University of Southampton
Subjects: Physics, Photon, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Quasar, Astrophysics, 01 natural sciences, Power law, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], quasars: individual: 3C 273, Space and Planetary Science, 0103 physical sciences, Broadband, Reflection (physics), Black-body radiation, Blazar, 010303 astronomy & astrophysics
Abstract: The aim of this paper is to study the evolution of the broadband spectrum of one of the brightest and nearest quasars 3C 273. We analyze the data obtained during quasi-simultaneous INTEGRAL and XMM monitoring of the blazar 3C 273 in 2003--2005 in the UV, X-ray and soft gamma-ray bands and study the results in the context of the long-term evolution of the source. The 0.2-100 keV spectrum of the source is well fitted by a combination of a soft cut-off power law and a hard power law. No improvement of the fit is achieved if one replaces the soft cut-off power law by either a blackbody, or a disk reflection model. During the observation period the source has reached the historically softest state in the hard X-ray domain with a photon index $\Gamma=1.82\pm 0.01$. Comparing our data with available archived X-ray data from previous years, we find a secular evolution of the source toward softer X-ray emission (the photon index has increased by $\Delta\Gamma\simeq 0.3-0.4$ over the last thirty years). We argue that existing theoretical models have to be significantly modified to account for the observed spectral evolution of the source., Comment: 11 pages, accepted to A&A
Published: 2007

85. Performances of JEM-EUSO: angular reconstruction The JEM-EUSO Collaboration

Author: Roberto Bellotti, P. Baragatti, Lech Wiktor Piotrowski, J. N. Albert, Yoshihiko Mizumoto, G. Distratis, Thomas Schanz, James H. Adams, F. Tajima, Livio Conti, Andreas A. Berlind, S. Yoshida, J. Szabelski, T. Murakami, J. Karczmarczyk, A. Zuccaro Marchi, Jörn Wilms, Alberto Cellino, Katsuaki Asano, O. A. Saprykin, I. Kreykenbohm, M. Ave Pernas, R. Nava, D. Kolev, P. Gorodetzky, Tomás Belenguer, Alfonso Monaco, Vladimir Andreev, F. Cafagna, G. Modestino, T. Shibata, Hanna Rothkaehl, E. Joven, Valerie Connaughton, A. Anzalone, N. Sakaki, L. Valore, S. Ahmad, Satoshi Wada, L. R. Wiencke, Rossella Caruso, Piero Vallania, M. D. Sabau, T. Napolitano, Ovidiu Vaduvescu, H. H. Silva Lopez, J. Hernández Carretero, M. Unger, J. Watts, M. Lacombe, Claudio Cassardo, T. Ogawa, Taka Tomida, D. Maravilla, Dmitri Semikoz, J. F. Valdés-Galicia, L. G. Tkachev, S. Csorna, A. Ebersoldt, C. Pennypacker, N. Inoue, L. del Peral, A. Franceschi, E. Parizot, B. Pastircak, P. Picozza, J. Lee, Angela V. Olinto, Fernando López, Graciela B. Gelmini, Pavol Bobik, G. Giraudo, G. Vankova, R. Bechini, P. Prat, H. Sato, C. Lachaud, D. Campana, H. J. Crawford, Andrea Santangelo, M. Rybczyński, J. Bayer, C. De Donato, S. Dagoret-Campagne, M. Wille, Inkyu Park, M. Nagata, Soon-Wook Kim, S. Biktemerova, I. Fernández-Gómez, T. Mernik, Tokonatsu Yamamoto, K. Belov, David B. Cline, C. Catalano, Y. Hachisu, G. Garipov, Y. Arai, Y. Miyazaki, M. Nagano Murakami, J. A. Morales de los Ríos, Y. Uchihori, P. L. Biermann, Yoshitaka Itow, G. Cordero, M. Karus, C. de la Taille, G. Castellinic, Markus Roth, Thomas J. Weiler, K. Katahira, C. González Alvarado, Mark Christl, O. Tibolla, S. Perez Cano, G. Catalano, J. S. Kim, E. G. Judd, Katsuhiko Tsuno, V. S. Morozenko, Fausto Guarino, P. von Ballmoos, M. Ricci, Y. Yamamoto, Susumu Inoue, Dmitry V. Naumov, J.N. Capdevielle, Silvia Ferrarese, Andrii Neronov, Patrick J. Reardon, Domenico Finco, Shigeto Watanabe, Toshiki Tajima, I. Rodríguez, R. Young, K. Kawai, Akinori Saito, M. Sakata, G. Siemieniec-Oziȩbło, Pierre Barrillon, S. Selmane, G. Masciantonio, Hitoshi Ohmori, R. Matev, Yoshiya Kawasaki, Francesco Isgrò, F. Dulucq, N. Tajima, B. Keilhauer, Barbara Szabelska, A. Jung, J. Błȩcki, S. Falk, T. Peter, Hiroyuki Sagawa, T. Shirahama, Yoshiki Tsunesada, I. Rusinov, D. Allard, H. Lim, Frederic Jean Ronga, M. C. Maccarone, T. Paul, K. Yoshida, S. A. Sharakin, M. E. Bertaina, Toshikazu Ebisuzaki, M. Sanz Palomino, Shigehiro Nagataki, Jianyi Yang, A. Guzmán, Ken'ichi Nomoto, C. Blaksley, H. Ikeda, M. Putis, G. Medina-Tanco, A. Sobey, Ke Fang, M. I. Panasyuk, Maxim Gonchar, Hirohiko M. Shimizu, A. Insolia, M. Kleifges, Humberto Ibarguen Salazar, M. Dupieux, A. Haungs, S. Piraino, Piotr Orleanski, C. De Santis, L. Villaseñor, H. Tokuno, G. Sáez-Cano, J. Geary, Javier Licandro, N. De Simone, L. Santiago Crúz, Y. Karadzhov, Hajime Takami, Yoshimasa Kurihara, H. Schieler, Mitsuteru Sato, Masaki Fukushima, M. Suzuki, R. Tsenov, T. Pierog, J. Watanabe, Valentina Scotti, A. Dell’Oro, H. Prieto, M. Takeda, Toshitaka Kajino, R. Cremonini, T. Nakamura, A. Pollini, Pavel Klimov, M. Di Martino, K. Higashide, C. Moretto, P. Galeotti, A. Marini, Marcos Reyes, G. Osteria, T. Tymieniecka, J. Sledd, C. Tenzer, M. Serra, T. Sugiyama, Tadeusz Wibig, Luis A. Anchordoqui, T. Batsch, S. Sánchez, N. Tone, G. Roudil, Daisuke Yonetoku, I. Kaneko, B. Harlov, Carlo Vigorito, M. Yu. Zotov, K. Kudela, Susana Briz, Toshiyuki Nonaka, M. D. Rodríguez Frías, Z. Plebaniak, J. Blümer, Michiyuki Chikawa, D. Monnier-Ragaigne, A. Segreto, Hajime Yano, N. Blanc, S. Blin-Bondil, Massimiliano Bonamente, E. Kuznetsov, Alexander Kusenko, K. Słomińska, Guillaume Prévôt, J. Fujimoto, M. Bogomilov, Ralph Engel, Frederic Trillaud, B. Mot, Yukihiro Takahashi, F. Kajino, Marco Casolino, Claudio Fornaro, H. W. Park, Z. Włodarczyk, Simona Toscano, I. V. Yashin, L. Marcelli, Kenji Shinozaki, A. Bruno, Karl Mannheim, Michael S. Briggs, A. J. de Castro, T. Patzak, B. A. Khrenov, H. Miyamoto, O. Martinez, K. Mase, Francesco Fenu, D. Ikeda, F. Sarazin, Marc Weber, D. Supanitsky, Shoichi Ogio, M. Flamini, Y. Takizawa, Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blümer, 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., Fernández Gómez, 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., González Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmán, A., Hachisu, Y., Harlov, B., Haungs, A., Hernández Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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., 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., López, 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 Ríos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Murakami, M. Nagano, 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., Orleański, 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., Prévôt, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodríguez, I., Rodríguez Frías, M. D., Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., Sáez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sánchez, S., Santangelo, A., Santiago Crúz, 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 Oziȩbło, G., Silva López, H. H., Sledd, J., Słomińska, 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., Valdés Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseñor, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., and Zuccaro Marchi, A.
Subjects: Physics, business.industry, Ciencias Físicas, Frame (networking), Detector, JEM-EUSO, Astronomy and Astrophysics, Context (language use), Astronomy and Astrophysic, Angular reconstruction, Astronomía, Optics, Space and Planetary Science, International Space Station, Pattern recognition (psychology), Angular resolution, Ultra-high-energy cosmic ray, Aerospace engineering, business, Energy (signal processing), CIENCIAS NATURALES Y EXACTAS
Abstract: Mounted on the International Space Station(ISS), the Extreme UniverseSpace 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 10 20 eV, 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 haveimplemented 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. Fil: Adams, J. H.. University of Alabama in Huntsville; Estados Unidos Fil: Ahmad, S.. Ecole Polytechnique; Francia Fil: Albert, J. N.. Univ Paris-Sud; Francia Fil: Allard, D.. Univ Paris Diderot; Francia Fil: Anchordoqui, L.. University of Wisconsin-Milwaukee; Estados Unidos Fil: Andreev, V.. University of California; Estados Unidos Fil: Anzalone, A.. INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo; Italia Fil: Arai, Y.. High Energy Accelerator Research Organization; Japón Fil: Asano, K.. Tokyo Institute of Technology; Japón Fil: Ave Pernas, M.. Universidad de Alcala (UAH); España Fil: Barrillon, P.. Univ Paris-Sud; Francia Fil: Batsch, T.. National Centre for Nuclear Research; Polonia Fil: Bayer, J.. University of Tübingen; Alemania Fil: Bechini, R.. Universita’ di Torino; Italia Fil: Belenguer, T.. Instituto Nacional de Técnica Aeroespacial ; España Fil: Bellotti, R.. Istituto Nazionale di Fisica Nucleare; Italia Fil: Belov, K.. University of California; Estados Unidos Fil: Berlind, A. A.. Vanderbilt University; Estados Unidos Fil: Bertaina, M.. Istituto Nazionale di Fisica Nucleare; Italia Fil: Biermann, P. L.. Karlsruhe Institute of Technology; Alemania Fil: Biktemerova, S.. Joint Institute for Nuclear Research; Rusia Fil: Blaksley, C.. Univ Paris Diderot; Francia Fil: Blanc, N.. Swiss Center for Electronics and Microtechnology; Suiza Fil: Blecki, J.. Space Research Centre of the Polish Academy of Sciences; Polonia Fil: Blin-bondil, S.. Ecole Polytechnique; Francia Fil: Blumer, J.. Karlsruhe Institute of Technology; Alemania Fil: Bobik, P.. Institute of Experimental Physics; Eslovaquia Fil: Bogomilov, M.. University of Sofia; Bulgaria Fil: Bonamente, M.. University of Alabama in Huntsville; Estados Unidos Fil: Supanitsky, Alberto Daniel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Guzman, A.. Institut f ur Astronomie und Astrophysik Tübingen; Alemania Fil: Mernik, T.. Institut fur Astronomie und Astrophysik Tübingen; Alemania Fil: The JEM-EUSO Collaboration.
Published: 2015

86. The EUSO-Balloon pathfinder

Author: N. Tone, Daisuke Yonetoku, H. Ikeda, K. Mase, Francesco Isgrò, B. Keilhauer, Francesco Fenu, I. V. Yashin, Frederic Jean Ronga, L. Santiago Crúz, M. Yu. Zotov, Silvia Ferrarese, L. Marcelli, Susana Briz, I. Kreykenbohm, Vladimir Andreev, F. Dulucq, D. Ikeda, F. Sarazin, Andreas A. Berlind, A. Bruno, Patrick J. Reardon, Toshiki Tajima, G. Siemieniec-Oziȩbło, D. Kolev, Karl Mannheim, Valerie Connaughton, H. H. Silva Lopez, Marc Weber, K. Shinozaki, G. Masciantonio, Hitoshi Ohmori, Tomás Belenguer, G. Castellinic, H. Prieto, R. Cremonini, P. L. Biermann, Yoshiya Kawasaki, R. Nava, Michael S. Briggs, A. J. de Castro, N. Sakaki, I. Rusinov, S. Ahmad, Markus Roth, M. D. Rodríguez Frías, Alberto Cellino, Fausto Guarino, P. von Ballmoos, M. Ricci, L. Valore, I. Rodríguez, D. Allard, Rossella Caruso, T. Patzak, Toshiyuki Nonaka, Alfonso Monaco, M. E. Bertaina, Thomas J. Weiler, Yoshihiko Mizumoto, Taka Tomida, Z. Plebaniak, J. Blümer, Marcos Reyes, Tokonatsu Yamamoto, G. Roudil, M. Putis, A. Sobey, T. Murakami, O. Martinez, T. Shirahama, S. Sánchez, G. Catalano, Ken'ichi Nomoto, J. Karczmarczyk, J. N. Albert, Thomas Schanz, B. A. Khrenov, H. Miyamoto, S. Perez Cano, H. J. Crawford, L. R. Wiencke, G. Giraudo, A. Insolia, M. Kleifges, Humberto Ibarguen Salazar, C. De Santis, H. Tokuno, M. Flamini, Hanna Rothkaehl, Michiyuki Chikawa, Y. Takizawa, Livio Conti, M. Serra, A. Haungs, C. De Donato, Soon-Wook Kim, B. Harlov, Luis A. Anchordoqui, S. Piraino, Carlo Vigorito, T. Batsch, Hajime Yano, S. Falk, K. Kudela, Yoshimasa Kurihara, H. Schieler, M. Nagata, Piotr Orleanski, J. Geary, J. S. Kim, T. Shibata, I. Kaneko, K. Kawai, Akinori Saito, A. Zuccaro Marchi, V. S. Morozenko, Jörn Wilms, Roberto Bellotti, Dmitry V. Naumov, Y. Karadzhov, Mitsuteru Sato, N. De Simone, R. Young, O. A. Saprykin, M. Sakata, B. Mot, Javier Licandro, J.N. Capdevielle, Z. Włodarczyk, P. Picozza, Andrii Neronov, J. Lee, James H. Adams, J. Błȩcki, G. Distratis, A. Ebersoldt, J. F. Valdés-Galicia, L. Villaseñor, Yukihiro Takahashi, R. Bechini, Piero Vallania, R. Tsenov, H. Lim, N. Tajima, M. C. Maccarone, M. D. Sabau, Toshikazu Ebisuzaki, M. Suzuki, L. G. Tkachev, G. Sáez-Cano, A. Jung, S. Csorna, T. Pierog, J. Watanabe, Gali Garipov, Shigehiro Nagataki, Yoshiki Tsunesada, Simona Toscano, A. Pollini, Pavel Klimov, D. Supanitsky, M. Takeda, F. Cafagna, T. Paul, K. Yoshida, Marco Casolino, Claudio Fornaro, J. Bayer, G. Modestino, E. Joven, K. Higashide, Lech Wiktor Piotrowski, G. Vankova, Shigeto Watanabe, C. de la Taille, Ovidiu Vaduvescu, M. Lacombe, K. Katahira, Claudio Cassardo, Massimiliano Bonamente, M. Rybczyński, Valentina Scotti, H. Sato, Shoichi Ogio, Dmitri Semikoz, Yoshitaka Itow, Graciela B. Gelmini, Hajime Takami, A. Guzman, Jianyi Yang, Masaki Fukushima, C. Lachaud, E. Kuznetsov, G. Medina-Tanco, S. Biktemerova, T. Mernik, Y. Hachisu, Y. Arai, S. Dagoret-Campagne, D. Maravilla, G. Cordero, N. Inoue, L. del Peral, A. Franceschi, E. Parizot, David B. Cline, T. Nakamura, Y. Yamamoto, Katsuaki Asano, Alexander Kusenko, C. González Alvarado, J. A. Morales de los Ríos, Pierre Barrillon, S. Yoshida, J. Szabelski, K. Słomińska, E. G. Judd, Sergei A. Sharakin, Katsuhiko Tsuno, Susumu Inoue, Guillaume Prévôt, Satoshi Wada, M. Di Martino, A. Marini, A. Dell’Oro, Toshitaka Kajino, T. Ogawa, G. Osteria, C. Blaksley, T. Tymieniecka, J. Sledd, M. Sanz Palomino, Angela V. Olinto, Fernando López, Andrea Santangelo, R. Matev, M. Bogomilov, F. Tajima, F. Kajino, Ralph Engel, C. Moretto, P. Galeotti, M. Ave Pernas, H. W. Park, P. Gorodetzky, C. Tenzer, T. Sugiyama, Tadeusz Wibig, Ke Fang, Frederic Trillaud, M. Wille, M. Nagano Murakami, Y. Uchihori, J. Hernández Carretero, M. Unger, M. Dupieux, Barbara Szabelska, T. Peter, M. I. Panasyuk, S. Selmane, A. Anzalone, T. Napolitano, K. Belov, C. Catalano, D. Monnier-Ragaigne, A. Segreto, N. Blanc, S. Blin-Bondil, J. Fujimoto, P. Bobik, Hiroyuki Sagawa, Maxim Gonchar, Hirohiko M. Shimizu, P. Baragatti, J. Watts, C. Pennypacker, B. Pastircak, P. Prat, I. Fernández-Gómez, M. Karus, Domenico Finco, D. Campana, Inkyu Park, Y. Miyazaki, Mark Christl, O. Tibolla, APC - Astrophysique des Hautes Energies (APC - AHE), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blã¼mer, 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., FernÃ¡ndez GÃ³mez, 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., GonzÃ¡lez Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmã¡n, A., Hachisu, Y., Harlov, B., Haungs, A., HernÃ¡ndez Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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., 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., Lã³pez, 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 RÃos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Murakami, M. Nagano, 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., Orleański, 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., Prã©vã´t, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodrãguez, I., RodrÃguez FrÃas, M. D., Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., SÃ¡ez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sã¡nchez, S., Santangelo, A., Santiago CrÃºz, 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 Oziȩbło, G., Silva LÃ³pez, H. H., Sledd, J., Słomińska, 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., ValdÃ©s Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseã±or, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., Zuccaro Marchi, A., Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)
Subjects: Ciencias Físicas, JEM-EUSO, cosmic-rays, Cosmic ray, 01 natural sciences, law.invention, Telescope, Observatory, law, 0103 physical sciences, International Space Station, Ultraviolet light, Air-fluorescence, Balloon experiment, UHECR, Astronomy and Astrophysics, Space and Planetary Science, 010303 astronomy & astrophysics, Remote sensing, Physics, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Astronomy and Astrophysic, Near space, Astronomía, Pathfinder, [SDU]Sciences of the Universe [physics], Temporal resolution, UHECR, Air-fluorescence, JEM-EUSO, Balloon experiment, EUSO-Balloon, CIENCIAS NATURALES Y EXACTAS
Abstract: 注記: The JEM-EUSO Collaboration 289名 [所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS) 池田, 博一; 鈴木, 睦; 矢野, 創], Accepted: 2015-06-11, Note: The JEM-EUSO Collaboration 289members [Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS) Ikeda, Hirokazu; Suzuki, Makoto; Yano, Hajime], 資料番号: SA1150237000
Published: 2015

87. Signatures of a Two Million Year Old Supernova in the Spectra of Cosmic Ray Protons, Antiprotons, and Positrons

Author: Andrii Neronov, M. Kachelrieß, and D. V. Semikoz
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Isotope, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Physics and Astronomy, Astronomy, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Near-Earth supernova, Spectral line, Supernova, Positron, Antiproton, Ultra-high-energy cosmic ray, Astrophysics - High Energy Astrophysical Phenomena, Nuclear Experiment
Abstract: The locally observed cosmic ray spectrum has several puzzling features, such as the excess of positrons and antiprotons above $\sim 20$ GeV and the discrepancy in the slopes of the spectra of cosmic ray protons and heavier nuclei in the TeV-PeV energy range. We show that these features are consistently explained by a nearby source which was active $\sim 2$ Myr ago and has injected $(1-2)\times 10^{50}$ erg in cosmic rays. The transient nature of the source and its overall energy budget point to the supernova origin of this local cosmic ray source. The age of the supernova suggests that the local cosmic ray injection was produced by the same supernova that has deposited $^{60}$Fe isotopes in the deep ocean crust., Comment: 5+2 pages, 3+1 eps figures; v2: reshuffled figures, minor rewording and added supplementary material; to appear in PRL
Published: 2015

88. Unified model for cosmic rays above1017 eVand the diffuse gamma-ray and neutrino backgrounds

Author: D.V. Semikoz, G. Giacinti, Andrii Neronov, Oleg Kalashev, and M. Kachelriess
Subjects: Physics, Nuclear and High Energy Physics, Active galactic nucleus, Proton, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Unified Model, Galaxy, 13. Climate action, Neutrino, Gamma-ray burst, Astrophysics::Galaxy Astrophysics
Abstract: We investigate how the extragalactic proton component derived within the "escape model" can be explained by astrophysical sources. We consider as possible cosmic ray (CR) sources normal/starburst galaxies and radio-loud active galactic nuclei (AGN). We find that the contribution to the total extragalactic proton flux from normal and starburst galaxies is only subdominant and does not fit the spectral shape deduced in the escape model. In the case of radio-loud AGN, we show that the complete extragalactic proton spectrum can be explained by a single source population, BL Lac/FR I, for any of the potential acceleration sites in these sources. We calculate the diffuse neutrino and $\gamma$-ray fluxes produced by these CR protons interacting with gas inside their sources. For a spectral slope of CRs close to $\alpha=2.1-2.2$ as suggested by shock acceleration, we find that these UHECR sources contribute the dominant fraction of both the isotropic $\gamma$-ray background and of the extragalactic part of the astrophysical neutrino signal observed by IceCube.
Published: 2015

89. Night time measurement of the UV background by EUSO-Balloon

Author: Kenji Shinozaki, Jorge F. Soriano, C. Moretto, G. Sáez-Cano, Andrii Neronov, C. Catalano, S. Bacholle, Pavol Bobik, S. Mackovjak, Luis del Peral, M. Putis, Maria Rodriguez Frias, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Physics, Astronomy, Balloon, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience; A precise characterization of the Earth’s UV background during night is essential for the observation of ultra-high-energy cosmic ray induced extensive air showers (EAS) from space. We have analyzed data from the flight of the EUSO-Balloon pathfinder mission that took place near Timmins (Canada) in the moonless night from 24 to 25 August 2014. The EUSO-Balloon telescope imaged the UV background in the wavelength range of 290 – 430 nm from an altitude of ∼ 38 km with an 1 m2 refractor telescope with ∼ 11◦ field-of-view pointed in nadir direction. The UV data were complemented by the data of the Infrared camera onboard EUSO-Balloon, which was operating in the wavelength ranges of 10.37 – 11.22 µm and 11.57 – 12.42 µm. We have combined the UV and IR images to study the upward UV radiance from the Earth’s surface and Earth’s atmosphere. This allowed us to estimate the level of UV background in clear atmosphere conditions without man-made light and also to investigate the influence of clouds on the UV background. Comparison of the UV and IR images reveals an evident dependence of the upward UV radiance on the atmospheric conditions. This opens a possibility to use the UV albedo measurement for characterization of the cloud coverage. The efficiency of detection of EAS from space by EUSO like detectors varies depending on the level of the UV background. Using the available EUSOBalloon data, we discuss the role of UV background variations due to clouds and man-made light on the exposure and effective area of EAS observations.
Published: 2015

90. The Atmospheric Monitoring System of the JEM-EUSO space mission

Author: M. D. Rodríguez Frías, Enrico Bozzo, Simona Toscano, L. del Peral, Andrii Neronov, and Satoshi Wada
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), media_common.quotation_subject, Physics, QC1-999, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Cosmic ray, Field of view, Généralités, law.invention, Telescope, Air shower, Lidar, Spitzer Space Telescope, law, Sky, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM), Optical depth, Remote sensing, media_common
Abstract: An Atmospheric Monitoring System (AMS) is a mandatory and key device of a space-based mission which aims to detect Ultra-High Energy Cosmic Rays (UHECR) and Extremely-High Energy Cosmic Rays (EHECR) from Space. JEM-EUSO has a dedicated atmospheric monitoring system that plays a fundamental role in our understanding of the atmospheric conditions in the Field of View (FoV) of the telescope. Our AMS consists of a very challenging space infrared camera and a LIDAR device, that are being fully designed with space qualification to fulfil the scientific requirements of this space mission. The AMS will provide information of the cloud cover in the FoV of JEM-EUSO, as well as measurements of the cloud top altitudes with an accuracy of 500? m and the optical depth profile of the atmosphere transmittance in the direction of each air shower with an accuracy of 0.15 degree and a resolution of 500? m. This will ensure that the energy of the primary UHECR and the depth of maximum development of the EAS (Extensive Air Shower) are measured with an accuracy better than 30% primary energy and 120? g/cm2 depth of maximum development for EAS occurring either in clear sky or with the EAS depth of maximum development above optically thick cloud layers. Moreover a very novel radiometric retrieval technique considering the LIDAR shots as calibration points, that seems to be the most promising retrieval algorithm is under development to infer the Cloud Top Height (CTH) of all kind of clouds, thick and thin clouds in the FoV of the JEM-EUSO space telescope., SCOPUS: cp.p, info:eu-repo/semantics/published
Published: 2015

91. Microlensing constraint on the size of the gamma-ray emission region in blazar B0218+357

Author: Ievgen Vovk and Andrii Neronov
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Blazar, 010303 astronomy & astrophysics
Abstract: Context. Observations of the effect of microlensing in gravitationally lensed quasars could potentially be used to study the structure of the source on distance scales down to the size of the supermassive black hole powering the quasar activity. Aims. We search for the microlensing effect in the gamma-ray band using the signal from a gravitationally lensed blazar B0218+357. Methonds. We develop a method of deconvolution of contributions of two images of the source into the gamma-ray band flaring lightcurve. We use this method to study the evolution of the magnification factor ratio between the two images throughout the flaring episodes. We interpret the time variability of the ratio as a signature of the microlensing effect and derive constraints on the physical parameters of the gamma-ray source by comparing the observed variability properties of the magnification factor ratio with those derived from numerical simulations of the microlensing caustics networks. Results. We find that the magnification factor ratio has experienced a change characteristic for a microlensing caustic crossing event during a 100 d flaring period in 2012. It has further changed between 2012 and a recent flaring episode in 2014. We use the measurement of the maximal magnification and duration of the caustic crossing event to derive an estimate of the projected size of the gamma-ray emission region in B0218+357, $R_\gamma \sim 10^{14}$ cm. This estimate is compatible with a complementary estimate found from the minimal variability time scale. The microlensing / minimal variability time scale measurements of the source size suggest that the gamma-ray emission is produced at the base of the blazar jet, in the direct vicinity of the central supermassive black hole., Comment: 7 pages, 5 figures
Published: 2015
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92. The JEM-EUSO mission : an introduction

Author: J. Karczmarczyk, A. Haungs, T. Murakami, Tomás Belenguer, Piero Vallania, M. D. Sabau, M. Serra, J. Bayer, C. de la Taille, K. Katahira, Luis A. Anchordoqui, T. Batsch, D. Supanitsky, Hanna Rothkaehl, R. Nava, N. Sakaki, Y. Karadzhov, I. Kaneko, K. Mase, J. Watts, L. Valore, Rossella Caruso, H. J. Crawford, C. Pennypacker, I. Rodríguez, Shoichi Ogio, Patrick J. Reardon, Toshiki Tajima, G. Siemieniec-Oziȩbło, G. Masciantonio, Hitoshi Ohmori, Yoshiya Kawasaki, D. Allard, G. Castellini, M. E. Bertaina, Ken'ichi Nomoto, Silvia Ferrarese, Toshiyuki Nonaka, P. Prat, R. Young, M. Sakata, A. Guzmán, I. V. Yashin, T. Shirahama, T. Shibata, Alberto Cellino, P. Picozza, J. Lee, I. Fernández-Gómez, P. Baragatti, L. Marcelli, Ralph Engel, M. Karus, G. Sáez Cano, M. Nagata, A. Ebersoldt, L. Villaseñor, A. Bruno, Jeong-Sook Kim, L. R. Wiencke, J. Błȩcki, Karl Mannheim, D. Ikeda, D. Monnier-Ragaigne, A. Segreto, F. Tajima, Lech Wiktor Piotrowski, M. Rybczyński, Michael S. Briggs, A. J. de Castro, F. Sarazin, Domenico Finco, H. Lim, Frederic Trillaud, P. Gorodetzky, Dmitry V. Naumov, R. Bechini, Marc Weber, Katsuaki Asano, G. Cordero, M. C. Maccarone, Piotr Orleanski, N. Blanc, S. Piraino, J.N. Capdevielle, T. Patzak, S. Yoshida, J. Szabelski, Francesco Fenu, Yoshiki Tsunesada, Hiroyuki Sagawa, M. Wille, Andrii Neronov, Y. Uchihori, R. Matev, G. Giraudo, M. Suzuki, Satoshi Wada, H. Sato, C. De Donato, Markus Roth, J. N. Albert, T. Ogawa, Hajime Takami, B. A. Khrenov, G. Distratis, Fausto Guarino, O. Martinez, Masaki Fukushima, Thomas Schanz, Soon-Wook Kim, Takuji Nakamura, Jianyi Yang, Yoshitaka Itow, Shigeto Watanabe, H. Miyamoto, D. Maravilla, P. von Ballmoos, M. Ricci, K. Shinozaki, Angela V. Olinto, Fernando López, Andrea Santangelo, S. Selmane, Livio Conti, J. Fujimoto, A. Anzalone, Barbara Szabelska, T. Peter, David B. Cline, A. Zuccaro Marchi, Maxim Gonchar, Hirohiko M. Shimizu, M. D. Rodríguez Frías, F. Cafagna, G. Modestino, E. Joven, D. Campana, Francesco Isgrò, F. Dulucq, Z. Plebaniak, J. Blümer, Valentina Scotti, B. Keilhauer, Graciela B. Gelmini, M. Flamini, P. L. Biermann, Jörn Wilms, Javier Licandro, M. I. Panasyuk, J. F. Valdés-Galicia, L. G. Tkachev, O. A. Saprykin, Michiyuki Chikawa, B. Mot, Y. Hachisu, Inkyu Park, Frederic Jean Ronga, M. Dupieux, S. Csorna, T. Napolitano, S. Perez Cano, Y. Takizawa, L. Santiago Crúz, M. Putis, Humberto Ibarguen Salazar, Y. Arai, G. Vankova, I. Rusinov, A. Sobey, Y. Miyazaki, S. Blin-Bondil, C. De Santis, H. Tokuno, Y. Yamamoto, A. Insolia, M. Kleifges, Yukihiro Takahashi, B. Pastirčák, E. G. Judd, T. Pierog, M. Ave Pernas, Katsuhiko Tsuno, H. Prieto, R. Cremonini, S. Biktemerova, J. Watanabe, Pierre Barrillon, Mark Christl, O. Tibolla, Osvaldo Catalano, Gali Garipov, K. Kawai, I. Kreykenbohm, Sergei A. Sharakin, R. Tsenov, Vladimir Andreev, Marcos Reyes, Marco Casolino, Claudio Fornaro, K. Belov, C. Catalano, A. Pollini, J. Hernández Carretero, Pavel Klimov, M. Unger, C. Lachaud, S. Dagoret-Campagne, M. Di Martino, A. Marini, Toshikazu Ebisuzaki, T. J. Weiler, G. Osteria, S. Sánchez, S. Ahmad, Yoshimasa Kurihara, T. Tymieniecka, J. Sledd, H. Schieler, Mitsuteru Sato, C. González Alvarado, Alfonso Monaco, C. Blaksley, N. Tone, Ke Fang, M. Nagano, Taka Tomida, Daisuke Yonetoku, Roberto Bellotti, Andreas A. Berlind, M. Sanz Palomino, Tokonatsu Yamamoto, James H. Adams, M. Yu. Zotov, D. Kolev, Valerie Connaughton, H. H. Silva Lopez, Susana Briz, S. Falk, H. Ikeda, V. S. Morozenko, Hajime Yano, A. Dell’Oro, Toshitaka Kajino, K. Higashide, C. Moretto, P. Galeotti, C. Tenzer, T. Sugiyama, Tadeusz Wibig, K. Kudela, G. Roudil, B. Harlov, Carlo Vigorito, N. Tajima, M. Takeda, Shigehiro Nagataki, Guillaume Prévôt, M. Bogomilov, F. Kajino, H. W. Park, Massimiliano Bonamente, E. Kuznetsov, Alexander Kusenko, K. Słomińska, Akinori Saito, Ovidiu Vaduvescu, M. Lacombe, Claudio Cassardo, Dmitri Semikoz, Sug-Whan Kim, T. Mernik, Z. Włodarczyk, Simona Toscano, N. Inoue, L. del Peral, A. Franceschi, E. Parizot, Pavol Bobik, J. A. Morales de los Ríos, Susumu Inoue, A. Jung, T. Paul, K. Yoshida, G. Medina-Tanco, J. Geary, N. De Simone, Yoshihiko Mizumoto, Organisation de Micro-Électronique Générale Avancée (OMEGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratori Nazionali del Sud (LNS), Istituto Nazionale di Fisica Nucleare (INFN), Division of Biology, Kansas State University, Kansas State University, CTC, Università degli studi di Bari Aldo Moro = University of Bari Aldo Moro (UNIBA), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universities Space Research Association (USRA), Regione Emilia Romagna, Servizio Tecnico Bacini Enza e sinistra Secchia, Institute for Data Processing and Electronics (IPE), Karlsruhe Institute of Technology (KIT), Institute for Ecology, Universität Greifswald - University of Greifswald, Tokushima research center, Department of Physics and Astronomy [UCLA, Los Angeles], University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (INFN, Sezione di Torino), Institute of Applied Biotechnology and Basic Sciences, Rzeszow University, Department of Mechanical System (Hiroshima University), Hiroshima University, Nagoya University, Department of Pathology, Ludwig-Maximilians-Universität München (LMU), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Institute of Experimental Physics of Kosice, Slovak Academy of Sciences (SAS), KEK (High energy accelerator research organization), iMagX/MIRO, Université Catholique de Louvain = Catholic University of Louvain (UCL), Instituto de Astrofisica de Canarias (IAC), The Open University of Japan [Chiba] (OUJ), Tohoku University [Sendai], Department of Earth and Planetary Science [Tokyo], Graduate School of Science [Tokyo], The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), Department of Electrical Engineering and Computer Sciences, University of Hyogo, INTEGRAL Science Data Center (ISDC), Geneva Observatory, Université de Genève = University of Geneva (UNIGE)-Université de Genève = University of Geneva (UNIGE), Service de dermatologie et vénéréologie (CHUV Lausanne), Centre Hospitalier Universitaire Vaudois [Lausanne] (CHUV), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Institute for Surgical Technology and Biomechanics [Bern] (ISTB), University of Bern, Centre IRMf de Marseille, Université de la Méditerranée - Aix-Marseille 2, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Centre d'étude spatiale des rayonnements (CESR), Center for Mathematics and Physics, University of Aizu, Centre de recherche sur la Paléobiodiversité et les Paléoenvironnements (CR2P), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Colorado School of Mines, Department of Physics (Department of Physics), Tokyo Metropolitan University [Tokyo] (TMU), Department of Radiation-Oncology, Università degli Studi di Firenze = University of Florence (UniFI), Graduate School of Materials Science, Nara Institute os Science and Technology, Observatoire océanologique de Banyuls (OOB), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Vrije Universiteit Brussel (VUB), Laboratoire de Génie Electrique de Grenoble (G2ELab), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Institute of Sensor and Actuator Systems, Vienna University of Technology (TU Wien), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Luxembourg Institute of Science and Technology (LIST), Dr. Karl-Remeis-Sternwarte, Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU)-Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Kyoto University, University of Connecticut (UCONN), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), National Institute for Nuclear Physics (INFN), University of Bari and INFN section of Bari, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), University of California-University of California, Université Catholique de Louvain (UCL), The University of Tokyo, University of Geneva [Switzerland]-University of Geneva [Switzerland], Polska Akademia Nauk (PAN), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Tokyo Metropolitan University [Tokyo], University of Florence (UNIFI), High Energy Accelerator Research Organization (KEK), University of Tsukuba, Vrije Universiteit [Brussels] (VUB), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Technical University of Vienna [Vienna] (TU WIEN), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Kyoto University [Kyoto], Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blã¼mer, 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., Castellini, G., Catalano, C., Catalano, O., 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., FernÃ¡ndez GÃ³mez, 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., GonzÃ¡lez Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmã¡n, A., Hachisu, Y., Harlov, B., Haungs, A., HernÃ¡ndez Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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, Jeong Sook, Kim, Soon Wook, Kim, Sug Whan, 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., Lã³pez, 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 RÃos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Nagano, M., 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., Orleański, 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., Prã©vã´t, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodrãguez, I., Frãas, M. D. RodrÃguez, Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., SÃ¡ez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sã¡nchez, S., Santangelo, A, Santiago CrÃºz, 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 Oziȩbło, G., Silva LÃ³pez, H. H., Sledd, J., Słomińska, 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., ValdÃ©s Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseã±or, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., Zuccaro Marchi, A., École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Università degli studi di Bari Aldo Moro (UNIBA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), The University of Tokyo (UTokyo), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Firenze = University of Florence [Firenze] (UNIFI), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology, Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Photon, Aperture, Ciencias Físicas, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Cosmic ray, ultra-high energy cosmic rays, Astrophysics, law.invention, Telescope, Atmosphere, law, International Space Station, Neutrino, Ultra-high energy cosmic rays, Neutrinos, Neutrinos, Ultra-high energy cosmic ray, ComputingMilieux_MISCELLANEOUS, media_common, Physics, [PHYS]Physics [physics], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, neutrinos, Astronomy and Astrophysics, Ultra-high energy cosmic rays, Astronomy and Astrophysic, Universe, Astronomía, Space and Planetary Science, Physics::Space Physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CIENCIAS NATURALES Y EXACTAS
Abstract: 注記: The JEM-EUSO Collaboration 288名 [所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS) 池田, 博一; 鈴木, 睦; 矢野, 創], Accepted: 2015-10-19, Note: The JEM-EUSO Collaboration 288members [Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS) Ikeda, Hirokazu; Suzuki, Makoto; Yano, Hajime], 資料番号: SA1150231000
Published: 2015

93. Calibration aspects of the JEM-EUSO mission

Author: Humberto Ibarguen Salazar, C. De Santis, H. Tokuno, Katsuaki Asano, Alfonso Monaco, M. Rybczyński, Alberto Cellino, R. Tsenov, Taka Tomida, H. Sato, P. Baragatti, Gali Garipov, A. Pollini, Pavel Klimov, G. Cordero, L. R. Wiencke, Tokonatsu Yamamoto, Barbara Szabelska, David B. Cline, Yoshimasa Kurihara, H. Schieler, Mitsuteru Sato, Silvia Ferrarese, M. Di Martino, G. Giraudo, A. Marini, T. Peter, Satoshi Wada, R. Matev, T. Ogawa, E. G. Judd, G. Catalano, Katsuhiko Tsuno, G. Osteria, T. Tymieniecka, J. Sledd, C. Lachaud, M. I. Panasyuk, B. A. Khrenov, H. Miyamoto, M. Suzuki, S. Dagoret-Campagne, D. Campana, Valentina Scotti, Ovidiu Vaduvescu, M. Lacombe, Claudio Cassardo, M. Ave Pernas, S. Falk, Graciela B. Gelmini, Y. Hachisu, Inkyu Park, F. Dulucq, Angela V. Olinto, Y. Arai, Fernando López, Andrea Santangelo, Massimiliano Bonamente, Y. Yamamoto, Francesco Isgrò, A. Guzmán, B. Keilhauer, J. N. Albert, Dmitri Semikoz, Pierre Barrillon, Sergei A. Sharakin, Y. Miyazaki, Thomas Schanz, J. Geary, Y. Karadzhov, Roberto Bellotti, R. Young, J. Watts, M. Sakata, Yoshitaka Itow, Andreas A. Berlind, M. D. Rodríguez Frías, E. Kuznetsov, Toshikazu Ebisuzaki, C. Pennypacker, Frederic Jean Ronga, Toshiyuki Nonaka, Z. Plebaniak, James H. Adams, B. Pastircak, N. De Simone, J. Blümer, M. Putis, Mark Christl, O. Tibolla, Livio Conti, P. Prat, L. Villaseñor, A. Zuccaro Marchi, P. L. Biermann, T. Mernik, I. Kreykenbohm, H. Ikeda, M. Flamini, Vladimir Andreev, F. Tajima, Michiyuki Chikawa, J. Hernández Carretero, P. Gorodetzky, I. Rusinov, I. Fernández-Gómez, A. Sobey, Ralph Engel, Yoshihiko Mizumoto, M. Unger, A. Insolia, M. Kleifges, Alexander Kusenko, Thomas J. Weiler, C. Blaksley, G. Sáez-Cano, Y. Takizawa, M. Wille, Jörn Wilms, D. Kolev, I. V. Yashin, S. Perez Cano, M. Nagano Murakami, Y. Uchihori, M. Karus, O. A. Saprykin, S. Ahmad, T. Shibata, L. Marcelli, K. Słomińska, Marcos Reyes, J. F. Valdés-Galicia, L. G. Tkachev, Domenico Finco, T. Murakami, Kenji Shinozaki, J. Karczmarczyk, R. Bechini, M. Serra, N. Inoue, Luis A. Anchordoqui, Ke Fang, J. Błȩcki, L. del Peral, A. Franceschi, E. Parizot, S. Sánchez, Pavol Bobik, Valerie Connaughton, H. H. Silva Lopez, S. Csorna, T. Batsch, A. Bruno, G. Vankova, Frederic Trillaud, Hiroyuki Sagawa, K. Mase, Karl Mannheim, Michael S. Briggs, A. J. de Castro, D. Maravilla, H. Lim, K. Kawai, Akinori Saito, S. Biktemerova, Francesco Fenu, M. C. Maccarone, Shigeto Watanabe, T. Patzak, I. Kaneko, Hajime Yano, Z. Włodarczyk, Piero Vallania, J. A. Morales de los Ríos, M. D. Sabau, M. Dupieux, Tomás Belenguer, Hanna Rothkaehl, Maxim Gonchar, Hirohiko M. Shimizu, G. Distratis, D. Supanitsky, Susumu Inoue, D. Ikeda, Lech Wiktor Piotrowski, D. Monnier-Ragaigne, A. Segreto, C. González Alvarado, N. Tone, F. Sarazin, Simona Toscano, J. Bayer, A. Ebersoldt, S. Selmane, Marc Weber, Daisuke Yonetoku, F. Cafagna, G. Modestino, E. Joven, Shoichi Ogio, P. Picozza, J. Lee, Guillaume Prévôt, S. Yoshida, J. Szabelski, C. de la Taille, M. Yu. Zotov, A. Jung, Javier Licandro, Susana Briz, A. Anzalone, T. Napolitano, H. J. Crawford, Yoshiki Tsunesada, T. Paul, K. Katahira, K. Yoshida, O. Martinez, B. Mot, Yukihiro Takahashi, N. Blanc, G. Castellinic, Markus Roth, R. Nava, Hajime Takami, M. Bogomilov, N. Sakaki, Patrick J. Reardon, T. Pierog, J. Watanabe, Toshiki Tajima, G. Siemieniec-Oziȩbło, Fausto Guarino, P. von Ballmoos, M. Ricci, L. Valore, Masaki Fukushima, M. Sanz Palomino, T. Nakamura, G. Medina-Tanco, M. Takeda, K. Belov, Marco Casolino, Claudio Fornaro, C. Catalano, Rossella Caruso, F. Kajino, G. Masciantonio, Hitoshi Ohmori, Yoshiya Kawasaki, I. Rodríguez, H. W. Park, T. Shirahama, D. Allard, M. E. Bertaina, Piotr Orleanski, C. De Donato, Soon-Wook Kim, Ken'ichi Nomoto, J. S. Kim, V. S. Morozenko, A. Haungs, S. Piraino, J. Fujimoto, S. Blin-Bondil, L. Santiago Crúz, H. Prieto, R. Cremonini, Jianyi Yang, M. Nagata, Dmitry V. Naumov, J.N. Capdevielle, Andrii Neronov, G. Roudil, B. Harlov, Carlo Vigorito, K. Kudela, N. Tajima, Shigehiro Nagataki, A. Dell’Oro, Toshitaka Kajino, K. Higashide, C. Moretto, P. Galeotti, C. Tenzer, T. Sugiyama, Tadeusz Wibig, Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blã¼mer, 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., FernÃ¡ndez GÃ³mez, 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., GonzÃ¡lez Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmã¡n, A., Hachisu, Y., Harlov, B., Haungs, A., HernÃ¡ndez Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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., 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., Lã³pez, 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 RÃos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Murakami, M. Nagano, 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., Orleański, 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., Prã©vã´t, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodrãguez, I., RodrÃguez FrÃas, M. D., Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., SÃ¡ez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sã¡nchez, S., Santangelo, A., Santiago CrÃºz, 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 Oziȩbło, G., Silva LÃ³pez, H. H., Sledd, J., Słomińska, 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., ValdÃ©s Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseã±or, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., and Zuccaro Marchi, A.
Subjects: Photon, Ciencias Físicas, JEM-EUSO, Phase (waves), Air-Shower fluorescence telescope, Calibration, Space-Based experiment, Astronomy and Astrophysics, Space and Planetary Science, computer science, law.invention, Telescope, Optics, law, Transmittance, observations and techniques, space-based experiment, Remote sensing, Physics, business.industry, Detector, air-shower fluorescence telescope, Albedo, Astronomy and Astrophysic, calibration, chemistry and earth sciences, Air-Shower fluorescence telescope, JEM-EUSO, Calibration, Space-Based experiment, Astronomía, astronomy, statistics for engineering, Focal surface, business, physics, CIENCIAS NATURALES Y EXACTAS
Abstract: he JEM-EUSO telescope will be, after calibration, a very accurate instrument which yields the number of received photons from the number of measured photo-electrons. The project is in phase A (demonstration of the concept) including already operating prototype instruments, i.e. many parts of the instrument have been constructed and tested. Calibration is a crucial part of the instrument and its use. The focal surface (FS) of the JEM-EUSO telescope will consist of about 5000 photo-multiplier tubes (PMTs), which have to be well calibrated to reach the required accuracy in reconstructing the air-shower parameters. The optics system consists of 3 plastic Fresnel (double-sided) lenses of 2.5 m diameter. Theaim of the calibration system is to measure the efficiencies (transmittances) of the optics and absolute efficiencies of the entire focal surface detector. The system consists of 3 main components: (i) Pre-flight calibration devices on ground, where the efficiency and gain of the PMTs will be measured absolutely and also the transmittance of the optics will be. (ii) On-board relative calibration system applying twomethods: a) operating during the day when the JEM-EUSO lid will be closed with small light sources on board. b) operating during the night, together with data taking: the monitoring of the background rate over identical sites. (iii) Absolute in-flight calibration, again, applying two methods: a) measurement of the moon light, reflected on high altitude, high albedo clouds. b) measurements of calibrated flashes and tracks produced by the Global Light System (GLS). Some details of each calibration method will be described in this paper. Fil: Adams, J. H.. University of Alabama in Huntsville; Estados Unidos Fil: Ahmad, S.. Ecole Polytechnique; Francia Fil: Albert, J. N.. Univ Paris-Sud; Francia Fil: Allard, D.. Univ Paris Diderot; Francia Fil: Anchordoqui, L.. University of Wisconsin-Milwaukee; Estados Unidos Fil: Andreev, V.. University of California; Estados Unidos Fil: Anzalone, A.. INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo; Italia Fil: Arai, Y.. High Energy Accelerator Research Organization (KEK); Japón Fil: Asano, K.. Tokyo Institute of Technology; Japón Fil: Ave Pernas, M.. Universidad de Alcala (UAH); España Fil: Barrillon, P.. Univ Paris-Sud; Francia Fil: Batsch, T.. National Centre for Nuclear Research; Polonia Fil: Bayer, J.. University of Tubingen; Alemania Fil: Bechini, R.. Universita’ di Torino; Italia Fil: Belenguer, T.. Instituto Nacional de Tecnica Aeroespacial (INTA); España Fil: Bellotti, R.. Istituto Nazionale di Fisica Nucleare; Italia Fil: Belov, K.. University of California; Estados Unidos Fil: Berlind, A. A.. Vanderbilt University; Estados Unidos Fil: Bertaina, M.. Istituto Nazionale di Fisica Nucleare; Italia Fil: Biermann, P. L.. Karlsruhe Institute of Technology (KIT); Alemania Fil: Biktemerova, S.. Joint Institute for Nuclear Research; Rusia Fil: Blaksley, C.. Univ Paris Diderot; Francia Fil: Blanc. N.. Swiss Center for Electronics and Microtechnology (CSEM); Suiza Fil: Blecki, J.. Space Research Centre of the Polish Academy of Sciences (CBK); Polonia Fil: Blin-Bondil, S.. Ecole Polytechnique; Francia Fil: Blumer, J.. Karlsruhe Institute of Technology (KIT); Alemania Fil: Bobik, P.. Institute of Experimental Physics; Eslovaquia Fil: Bogomilov, M.. University of Sofia; Bulgaria Fil: Bonamente, M.. University of Alabama in Huntsville; Estados Unidos Fil: Supanitsky, Alberto Daniel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: The JEM-EUSO Collaboration.
Published: 2015

94. The JEM-EUSO observation in cloudy conditions

Author: J. Fujimoto, Humberto Ibarguen Salazar, C. De Santis, H. Tokuno, A. Anzalone, B. Mot, T. Napolitano, P. L. Biermann, F. Tajima, Andrii Neronov, I. Rusinov, Toshiyuki Nonaka, J. Watts, R. Tsenov, Yukihiro Takahashi, P. Gorodetzky, Piero Vallania, M. D. Sabau, T. Shibata, Jianyi Yang, C. Pennypacker, B. Pastircak, Javier Licandro, A. Pollini, Pavel Klimov, P. Prat, D. Monnier-Ragaigne, A. Segreto, Alberto Cellino, Marco Casolino, Claudio Fornaro, I. Fernández-Gómez, Ovidiu Vaduvescu, M. Lacombe, Claudio Cassardo, M. Di Martino, A. Marini, G. Osteria, J. N. Albert, Alfonso Monaco, N. Blanc, J. Bayer, B. A. Khrenov, Andreas A. Berlind, M. Wille, M. Nagano Murakami, Y. Uchihori, Thomas Schanz, R. Bechini, T. Tymieniecka, J. Sledd, M. Karus, Marcos Reyes, L. R. Wiencke, Katsuaki Asano, Taka Tomida, Dmitri Semikoz, H. Miyamoto, C. de la Taille, K. Katahira, M. D. Rodríguez Frías, C. De Donato, D. Kolev, Z. Plebaniak, Domenico Finco, S. Blin-Bondil, Soon-Wook Kim, J. Blümer, Livio Conti, G. Giraudo, Valerie Connaughton, H. H. Silva Lopez, L. Santiago Crúz, Tokonatsu Yamamoto, Shigeto Watanabe, Patrick J. Reardon, Toshiki Tajima, G. Siemieniec-Oziȩbło, Michiyuki Chikawa, S. Sánchez, K. Belov, C. Catalano, Hiroyuki Sagawa, J. S. Kim, T. Pierog, M. Flamini, A. Zuccaro Marchi, V. S. Morozenko, J. Watanabe, M. Takeda, Ralph Engel, Jörn Wilms, Y. Karadzhov, G. Catalano, F. Dulucq, G. Roudil, R. Young, G. Masciantonio, Hitoshi Ohmori, M. Sakata, Yoshiya Kawasaki, H. Prieto, R. Cremonini, Satoshi Wada, M. Serra, T. Mernik, B. Harlov, T. Ogawa, Luis A. Anchordoqui, Carlo Vigorito, Y. Takizawa, O. A. Saprykin, T. Batsch, Yoshitaka Itow, Hajime Yano, K. Kudela, P. Baragatti, Z. Włodarczyk, Frederic Trillaud, D. Allard, M. E. Bertaina, S. Falk, Francesco Isgrò, J. Błȩcki, I. Kaneko, Angela V. Olinto, Fernando López, Andrea Santangelo, Thomas J. Weiler, B. Keilhauer, S. Perez Cano, H. Lim, Maxim Gonchar, Hirohiko M. Shimizu, M. Putis, M. C. Maccarone, A. Sobey, Ken'ichi Nomoto, Barbara Szabelska, T. Peter, A. Insolia, M. Kleifges, I. V. Yashin, Frederic Jean Ronga, A. Ebersoldt, N. Tone, L. Marcelli, N. Tajima, Shigehiro Nagataki, D. Maravilla, A. Haungs, Simona Toscano, S. Piraino, Daisuke Yonetoku, Gali Garipov, M. Nagata, Kenji Shinozaki, R. Nava, K. Kawai, S. Selmane, N. Sakaki, Akinori Saito, H. Ikeda, A. Bruno, M. Yu. Zotov, Karl Mannheim, Michael S. Briggs, A. J. de Castro, Yoshiki Tsunesada, M. I. Panasyuk, Dmitry V. Naumov, L. Valore, Rossella Caruso, Massimiliano Bonamente, Susana Briz, J.N. Capdevielle, Hajime Takami, E. Kuznetsov, G. Distratis, Masaki Fukushima, T. Nakamura, O. Martinez, I. Rodríguez, T. Patzak, A. Dell’Oro, Toshitaka Kajino, C. Lachaud, S. Dagoret-Campagne, T. Shirahama, K. Higashide, C. Moretto, P. Galeotti, C. Tenzer, F. Cafagna, G. Modestino, E. Joven, T. Sugiyama, Tadeusz Wibig, Toshikazu Ebisuzaki, K. Mase, Alexander Kusenko, Francesco Fenu, Piotr Orleanski, K. Słomińska, Guillaume Prévôt, C. González Alvarado, C. Blaksley, D. Campana, Ke Fang, D. Ikeda, Inkyu Park, D. Supanitsky, F. Sarazin, Marc Weber, M. Bogomilov, Y. Miyazaki, M. Dupieux, F. Kajino, Shoichi Ogio, Mark Christl, O. Tibolla, M. Sanz Palomino, H. W. Park, J. F. Valdés-Galicia, L. G. Tkachev, S. Csorna, G. Vankova, S. Biktemerova, Silvia Ferrarese, Lech Wiktor Piotrowski, G. Castellinic, S. Yoshida, J. Szabelski, Markus Roth, Fausto Guarino, P. von Ballmoos, M. Ricci, Yoshihiko Mizumoto, T. Murakami, J. Karczmarczyk, M. Ave Pernas, M. Suzuki, Hanna Rothkaehl, P. Picozza, J. Lee, J. Hernández Carretero, Valentina Scotti, M. Unger, Graciela B. Gelmini, Y. Hachisu, Y. Arai, Y. Yamamoto, N. Inoue, Pierre Barrillon, L. del Peral, A. Franceschi, E. Parizot, Pavol Bobik, Sergei A. Sharakin, J. A. Morales de los Ríos, Susumu Inoue, Yoshimasa Kurihara, H. Schieler, A. Jung, Mitsuteru Sato, T. Paul, K. Yoshida, G. Medina-Tanco, H. Sato, J. Geary, N. De Simone, David B. Cline, E. G. Judd, Katsuhiko Tsuno, A. Guzmán, L. Villaseñor, Roberto Bellotti, G. Sáez-Cano, M. Rybczyński, James H. Adams, I. Kreykenbohm, Vladimir Andreev, G. Cordero, S. Ahmad, R. Matev, Tomás Belenguer, H. J. Crawford, Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blümer, 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., Fernández Gómez, 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., González Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmán, A., Hachisu, Y., Harlov, B., Haungs, A., Hernández Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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., 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., López, 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 Ríos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Murakami, M. Nagano, 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., Orleański, 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., Prévôt, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodríguez, I., Rodríguez Frías, M. D., Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., Sáez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sánchez, S., Santangelo, A., Santiago Crúz, 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 Oziȩbło, G., Silva López, H. H., Sledd, J., Słomińska, 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., Valdés Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseñor, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., and Zuccaro Marchi, A.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Ciencias Físicas, Extensive air shower, JEM-EUSO, Cloud computing, Ultra-high energy cosmic ray, Astronomy and Astrophysics, Space and Planetary Science, Observatory, International Space Station, Ultra-high-energy cosmic ray, Optical depth, Remote sensing, Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysic, Astronomía, Air shower, JEM-EUSO, Ultra-high energy cosmic ray, Extensive air shower, Physics::Space Physics, Orbit (dynamics), Satellite, business, CIENCIAS NATURALES Y EXACTAS
Abstract: 注記: The JEM-EUSO Collaboration 288名 [所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS) 池田, 博一; 鈴木, 睦; 矢野, 創], Accepted: 2014-02-26, Note: The JEM-EUSO Collaboration 288members [Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS) Ikeda, Hirokazu; Suzuki, Makoto; Yano, Hajime], 資料番号: SA1150234000
Published: 2015

95. Toward the full test of the nuMSM sterile neutrino dark matter model with Athena

Author: Denys Malyshev and Andrii Neronov
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Particle physics, Sterile neutrino, 010308 nuclear & particles physics, Hot dark matter, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, High Energy Physics::Phenomenology, Scalar field dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Warm dark matter, High Energy Physics::Experiment, Neutrino, 010306 general physics, Neutrino oscillation, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Light dark matter, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract: We discuss the potential of Athena X-ray telescope, in particular of its X-ray Integral Field Unit (X-IFU), for detection of the signal from the light-weight decaying dark matter with mass in the keV range. We show that high energy resolution and large collection area of X-IFU will provide an improvement of sensitivity which will be sufficient for the full test of the neutrino Minimal extension of the Standard Model (nuMSM). Search for the narrow spectral line produced by the decay of the dark matter sterile neutrino in the spectra of dwarf spheroidal galaxies with X-IFU will explore the whole allowed range masses and mixing angles of the nuMSM lightest sterile neutrino and in this way either to find the dark matter signal or rule out the nuMSM model., Comment: To match the accepted version
Published: 2015
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96. Performances of JEM–EUSO : energy and X_{max} reconstruction

Author: I. V. Yashin, L. Marcelli, B. A. Khrenov, H. Miyamoto, Kenji Shinozaki, A. Bruno, Karl Mannheim, Michael S. Briggs, A. J. de Castro, D. Supanitsky, Shoichi Ogio, M. Rybczyński, F. Dulucq, Graciela B. Gelmini, Andreas A. Berlind, A. Jung, Massimiliano Bonamente, Javier Licandro, T. Paul, N. Tone, Daisuke Yonetoku, M. Ave Pernas, F. Tajima, H. Sato, David B. Cline, Gali Garipov, C. De Donato, Soon-Wook Kim, G. Cordero, M. Yu. Zotov, K. Yoshida, Susana Briz, S. Selmane, Y. Hachisu, Y. Arai, Y. Yamamoto, Piero Vallania, M. D. Sabau, Alfonso Monaco, Taka Tomida, J. Bayer, E. Kuznetsov, J. Hernández Carretero, P. Baragatti, Hiroyuki Sagawa, D. Kolev, J. S. Kim, M. Putis, A. Sobey, A. Insolia, M. Kleifges, C. de la Taille, E. G. Judd, K. Katahira, M. Unger, T. Pierog, J. Watanabe, M. Wille, M. Nagano Murakami, Y. Uchihori, M. Takeda, J. F. Valdés-Galicia, P. Gorodetzky, G. Distratis, V. S. Morozenko, C. Lachaud, Katsuhiko Tsuno, G. Castellinic, Katsuaki Asano, J. Fujimoto, Tokonatsu Yamamoto, Patrick J. Reardon, Toshiki Tajima, G. Siemieniec-Oziȩbło, G. Masciantonio, Hitoshi Ohmori, Yoshiya Kawasaki, S. Dagoret-Campagne, Pierre Barrillon, L. G. Tkachev, S. Csorna, Valerie Connaughton, Toshikazu Ebisuzaki, T. Shibata, I. Kreykenbohm, D. Allard, M. E. Bertaina, Alexander Kusenko, G. Vankova, H. H. Silva Lopez, Jianyi Yang, Vladimir Andreev, R. Matev, J. N. Albert, M. Di Martino, Markus Roth, G. Medina-Tanco, Ken'ichi Nomoto, Francesco Isgrò, A. Marini, D. Campana, M. Nagata, Thomas Schanz, Hajime Yano, Fausto Guarino, P. von Ballmoos, M. Ricci, Satoshi Wada, G. Catalano, P. Prat, A. Haungs, S. Piraino, K. Słomińska, B. Keilhauer, G. Prévôt, S. Biktemerova, T. Ogawa, Yoshihiko Mizumoto, T. Patzak, Lech Wiktor Piotrowski, R. Nava, Inkyu Park, Dmitry V. Naumov, R. Bechini, N. Sakaki, Livio Conti, Ke Fang, S. Ahmad, T. Murakami, J. Karczmarczyk, A. Zuccaro Marchi, Y. Karadzhov, L. Valore, F. Cafagna, Frederic Jean Ronga, Sergei A. Sharakin, G. Modestino, Rossella Caruso, Angela V. Olinto, Fernando López, Jörn Wilms, E. Joven, G. Osteria, Andrea Santangelo, T. Tymieniecka, J. Sledd, D. Maravilla, Y. Miyazaki, A. Dell’Oro, Toshitaka Kajino, S. Yoshida, J. Szabelski, Silvia Ferrarese, O. A. Saprykin, P. L. Biermann, Maxim Gonchar, S. Falk, S. Blin-Bondil, Hirohiko M. Shimizu, R. Young, M. Sakata, I. Rusinov, M. Dupieux, Z. Włodarczyk, Hanna Rothkaehl, Shigeto Watanabe, Mark Christl, O. Tibolla, J. N. Capdevielle, L. Santiago Crúz, A. Anzalone, T. Napolitano, Thomas J. Weiler, K. Higashide, C. Moretto, J. Geary, P. Galeotti, Alberto Cellino, A. Guzmán, S. Perez Cano, C. González Alvarado, Marcos Reyes, P. Picozza, J. Błȩcki, Roberto Bellotti, H. Prieto, J. Lee, Simona Toscano, Barbara Szabelska, T. Peter, C. Tenzer, I. Rodríguez, H. Lim, L. R. Wiencke, R. Cremonini, M. C. Maccarone, N. De Simone, T. Sugiyama, J. Watts, S. Sánchez, Tadeusz Wibig, T. Shirahama, Toshiyuki Nonaka, C. Pennypacker, James H. Adams, Andrii Neronov, B. Pastircak, H. Ikeda, L. Villaseñor, G. Giraudo, G. Sáez-Cano, N. Inoue, I. Fernández-Gómez, K. Kawai, L. del Peral, A. Franceschi, E. Parizot, Pavol Bobik, M. Sanz Palomino, M. Bogomilov, D. Monnier-Ragaigne, A. Segreto, M. Karus, M. I. Panasyuk, Akinori Saito, M. Suzuki, Piotr Orleanski, Domenico Finco, K. Belov, C. Catalano, F. Kajino, J. A. Morales de los Ríos, Yoshitaka Itow, Ovidiu Vaduvescu, G. Roudil, M. Lacombe, Tomás Belenguer, Claudio Cassardo, B. Harlov, Susumu Inoue, H. W. Park, Carlo Vigorito, K. Kudela, H. J. Crawford, Valentina Scotti, Humberto Ibarguen Salazar, C. De Santis, H. Tokuno, N. Tajima, T. Mernik, Shigehiro Nagataki, R. Tsenov, A. Pollini, Pavel Klimov, Yoshimasa Kurihara, H. Schieler, Ralph Engel, Mitsuteru Sato, Frederic Trillaud, B. Mot, Yukihiro Takahashi, Marco Casolino, Claudio Fornaro, M. Flamini, Y. Takizawa, C. Blaksley, K. Mase, M. D. Rodríguez Frías, Z. Plebaniak, J. Blümer, Michiyuki Chikawa, D. Ikeda, A. Ebersoldt, F. Sarazin, Marc Weber, Yoshiki Tsunesada, O. Martinez, N. Blanc, Francesco Fenu, D. Semikoz, Hajime Takami, Masaki Fukushima, T. Nakamura, M. Serra, Luis A. Anchordoqui, T. Batsch, I. Kaneko, Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blümer, 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., Fernández Gómez, 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., González Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmán, A., Hachisu, Y., Harlov, B., Haungs, A., Hernández Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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., 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., López, 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 Ríos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Murakami, M. Nagano, 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., Orleański, 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., Prévôt, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodríguez, I., Rodríguez Frías, M. D., Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., Sáez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sánchez, S., Santangelo, A., Santiago Crúz, 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 Oziȩbło, G., Silva López, H. H., Sledd, J., Słomińska, 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., Valdés Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseñor, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., and Zuccaro Marchi, A.
Subjects: reconstruction, Ciencias Físicas, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, JEM-EUSO, X (max) reconstruction, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Cosmic ray, X_{max} reconstruction, Astrophysics, law.invention, Energy reconstruction, JEM–EUSO, Xmax reconstruction, Astronomy and Astrophysics, Space and Planetary Science, Telescope, law, International Space Station, Ultra-high-energy cosmic ray, max, media_common, energy reconstruction, Physics, Resolution (electron density), Astrophysics::Instrumentation and Methods for Astrophysics, X-max reconstruction, Astronomy, Universe, Astronomía, JEM-EUSO, Energy reconstruction, X-max reconstruction, Event (particle physics), CIENCIAS NATURALES Y EXACTAS, Energy (signal processing)
Abstract: 注記: The JEM-EUSO Collaboration 288名 [所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS) 池田, 博一; 鈴木, 睦; 矢野, 創], Accepted: 2014-10-13, Note: The JEM-EUSO Collaboration 288members [Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS) Ikeda, Hirokazu; Suzuki, Makoto; Yano, Hajime], 資料番号: SA1150235000
Published: 2015

97. The infrared camera onboard JEM-EUSO

Author: Gali Garipov, Andreas A. Berlind, D. Kolev, Valerie Connaughton, H. H. Silva Lopez, C. Lachaud, S. Dagoret-Campagne, Patrick J. Reardon, Barbara Szabelska, Toshiki Tajima, T. Peter, G. Siemieniec-Oziȩbło, G. Masciantonio, Hitoshi Ohmori, Yoshiya Kawasaki, Yoshihiko Mizumoto, D. Allard, N. Tajima, Shigehiro Nagataki, Andrii Neronov, J. N. Albert, T. Murakami, M. Di Martino, Thomas Schanz, M. E. Bertaina, A. Marini, Alfonso Monaco, M. I. Panasyuk, J. Karczmarczyk, J. F. Valdés-Galicia, L. G. Tkachev, Ken'ichi Nomoto, S. Csorna, N. Tone, G. Vankova, D. Maravilla, Livio Conti, Daisuke Yonetoku, G. Osteria, A. Zuccaro Marchi, Taka Tomida, S. Biktemerova, Tokonatsu Yamamoto, Tomás Belenguer, T. Shibata, Hanna Rothkaehl, A. Anzalone, T. Napolitano, Jörn Wilms, O. A. Saprykin, M. Yu. Zotov, Y. Karadzhov, T. Tymieniecka, J. Sledd, Piero Vallania, Massimiliano Bonamente, Thomas J. Weiler, M. Flamini, G. Catalano, Katsuaki Asano, S. Perez Cano, Y. Takizawa, Hiroyuki Sagawa, M. Serra, Luis A. Anchordoqui, T. Batsch, Silvia Ferrarese, L. Santiago Crúz, M. D. Sabau, J. Bayer, C. de la Taille, Susana Briz, P. Picozza, J. Lee, Jianyi Yang, K. Katahira, K. Belov, C. Catalano, I. Kaneko, E. Kuznetsov, R. Bechini, Satoshi Wada, I. Rodríguez, T. Shirahama, R. Nava, N. Sakaki, L. Valore, H. Prieto, R. Cremonini, Rossella Caruso, F. Tajima, Alexander Kusenko, S. Falk, T. Ogawa, K. Słomińska, Roberto Bellotti, Humberto Ibarguen Salazar, Hajime Yano, Angela V. Olinto, K. Mase, K. Kawai, Akinori Saito, H. Ikeda, R. Young, M. Sakata, P. Gorodetzky, Fernando López, Andrea Santangelo, Piotr Orleanski, C. De Santis, H. Tokuno, Francesco Fenu, James H. Adams, Z. Włodarczyk, Maxim Gonchar, Hirohiko M. Shimizu, Shigeto Watanabe, M. Wille, Ovidiu Vaduvescu, M. Lacombe, Claudio Cassardo, H. J. Crawford, M. Rybczyński, M. Nagano Murakami, S. Selmane, Lech Wiktor Piotrowski, Y. Uchihori, G. Cordero, G. Castellinic, Javier Licandro, M. Nagata, Dmitri Semikoz, Markus Roth, F. Dulucq, M. D. Rodríguez Frías, J. Błȩcki, P. L. Biermann, Simona Toscano, D. Ikeda, Dmitry V. Naumov, Z. Plebaniak, S. Yoshida, J. Szabelski, R. Tsenov, Fausto Guarino, I. Rusinov, P. von Ballmoos, M. Ricci, J. Blümer, Guillaume Prévôt, F. Sarazin, J. Watts, J.N. Capdevielle, H. Lim, H. Sato, M. C. Maccarone, C. Pennypacker, A. Pollini, Marc Weber, B. Pastircak, M. Ave Pernas, Pavel Klimov, Michiyuki Chikawa, M. Bogomilov, P. Prat, T. Pierog, J. Watanabe, I. Fernández-Gómez, R. Matev, Toshikazu Ebisuzaki, M. Putis, A. Sobey, David B. Cline, Marcos Reyes, M. Takeda, M. Karus, Yoshitaka Itow, O. Martinez, A. Insolia, M. Kleifges, F. Kajino, A. Ebersoldt, T. Mernik, C. De Donato, S. Sánchez, Domenico Finco, Soon-Wook Kim, H. W. Park, J. Hernández Carretero, M. Unger, C. Blaksley, A. Guzmán, E. G. Judd, Ke Fang, J. S. Kim, Katsuhiko Tsuno, V. S. Morozenko, Yoshiki Tsunesada, G. Distratis, I. Kreykenbohm, L. Villaseñor, G. Sáez-Cano, M. Dupieux, Vladimir Andreev, Hajime Takami, S. Ahmad, F. Cafagna, Masaki Fukushima, T. Nakamura, G. Modestino, E. Joven, C. González Alvarado, M. Sanz Palomino, A. Dell’Oro, Toshitaka Kajino, K. Higashide, C. Moretto, P. Galeotti, C. Tenzer, T. Sugiyama, Tadeusz Wibig, G. Roudil, B. Harlov, Carlo Vigorito, K. Kudela, Francesco Isgrò, B. Keilhauer, Frederic Jean Ronga, Alberto Cellino, L. R. Wiencke, G. Giraudo, B. A. Khrenov, Toshiyuki Nonaka, H. Miyamoto, D. Monnier-Ragaigne, A. Segreto, Ralph Engel, N. Blanc, S. Blin-Bondil, Frederic Trillaud, B. Mot, Yukihiro Takahashi, D. Supanitsky, Marco Casolino, Claudio Fornaro, Shoichi Ogio, I. V. Yashin, L. Marcelli, J. Fujimoto, Kenji Shinozaki, A. Bruno, Karl Mannheim, Michael S. Briggs, A. J. de Castro, J. Geary, T. Patzak, N. De Simone, A. Jung, T. Paul, K. Yoshida, P. Baragatti, G. Medina-Tanco, N. Inoue, L. del Peral, A. Franceschi, E. Parizot, Pavol Bobik, D. Campana, J. A. Morales de los Ríos, Inkyu Park, Susumu Inoue, Y. Miyazaki, Mark Christl, O. Tibolla, Graciela B. Gelmini, Y. Hachisu, Y. Arai, Y. Yamamoto, Pierre Barrillon, Sergei A. Sharakin, A. Haungs, S. Piraino, M. Suzuki, Valentina Scotti, Yoshimasa Kurihara, H. Schieler, Mitsuteru Sato, Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blümer, 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., Fernández Gómez, 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., González Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmán, A., Hachisu, Y., Harlov, B., Haungs, A., Hernández Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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., 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., López, 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 Ríos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Murakami, M. Nagano, 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., Orleański, 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., Prévôt, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodríguez, I., Rodríguez Frías, M. D., Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., Sáez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sánchez, S., Santangelo, A., Santiago Crúz, 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 Oziȩbło, G., Silva López, H. H., Sledd, J., Słomińska, 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., Valdés Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseñor, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., and Zuccaro Marchi, A.
Subjects: Ciencias Físicas, Astrophysics::High Energy Astrophysical Phenomena, JEM-EUSO, Cloud computing, Cosmic ray, Atmosphere, IR-camera, Space observatory, Ultra-High Energy Cosmic Rays (UHECR), Astronomy and Astrophysics, Space and Planetary Science, International Space Station, Calibration, JEM-EUSO, Space observatory, IR-camera, Ultra-High Energy Cosmic Rays (UHECR), Remote sensing, Physics, Calorimeter (particle physics), business.industry, Cloud top, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysic, Astronomía, Lidar, Physics::Space Physics, business, CIENCIAS NATURALES Y EXACTAS
Abstract: 注記: The JEM-EUSO Collaboration 288名 [所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS) 池田, 博一; 鈴木, 睦; 矢野, 創], Accepted: 2014-06-12, Note: The JEM-EUSO Collaboration 288members [Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS) Ikeda, Hirokazu; Suzuki, Makoto; Yano, Hajime], 資料番号: SA1150233000
Published: 2015

98. Comparison of the expected and observed supernova remnant counts with Fermi/LAT

Author: Andrii Neronov, Ie. Vovk, and D. Malyshev
Subjects: Physics, education.field_of_study, Astrophysics::High Energy Astrophysical Phenomena, QC1-999, Population, Astronomy, Cosmic ray, Observable, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Stars, Supernova, Supernova remnant, education, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: SNRs are commonly believed to be the accelerators of the galactic cosmic rays – mainly protons – and are expected to produce γ-rays through the inelastic proton-proton collisions. Fermi/LAT was expected to detect many of those, but only a dozen is listed in the recent Fermi/LAT 2nd Source catalogue. To test whether the observed number of SNRs is in agreement with the above assumption, we use a simplified model of an SNR and calculate the predicted amount of the observable remnants taking into account their distribution in the Galaxy and the sensitivity of Fermi/LAT. We find that the observed number of SNRs agrees with the prediction of our model if we assume a low, ≪ 1 cm−3 , number density of the SNR's ambient medium. The result, presented here, suggests, that on average the supernova explosions happen in the under-dense regions, such as bubbles, creating by the winds of the progenitor stars. Under this natural supposition our result finds an agreement with the assumption, that the observed population of supernovae remnants is indeed responsible for the production of the galactic cosmic rays.
Published: 2015

99. Science of atmospheric phenomena with JEM-EUSO

Author: Yoshihiko Mizumoto, Toshiyuki Nonaka, T. Murakami, A. Guzmán, J. Karczmarczyk, J. Watts, C. Pennypacker, B. Pastircak, P. Prat, I. Fernández-Gómez, M. Karus, Domenico Finco, Hiroyuki Sagawa, M. Suzuki, M. Flamini, Hanna Rothkaehl, D. Monnier-Ragaigne, A. Segreto, Maxim Gonchar, Hirohiko M. Shimizu, L. Villaseñor, Y. Takizawa, Javier Licandro, P. Picozza, Alberto Cellino, Roberto Bellotti, J. Lee, F. Dulucq, Lech Wiktor Piotrowski, Valentina Scotti, J. N. Albert, N. Blanc, Thomas Schanz, Toshikazu Ebisuzaki, G. Sáez-Cano, M. Rybczyński, Andreas A. Berlind, L. R. Wiencke, James H. Adams, H. Ikeda, M. Di Martino, S. Yoshida, J. Szabelski, A. Marini, T. Pierog, J. Watanabe, G. Cordero, M. Takeda, G. Castellinic, Livio Conti, C. De Donato, A. Zuccaro Marchi, G. Giraudo, Soon-Wook Kim, Katsuaki Asano, S. Blin-Bondil, Markus Roth, A. Dell’Oro, Toshitaka Kajino, A. Haungs, S. Piraino, Jörn Wilms, D. Kolev, G. Osteria, Massimiliano Bonamente, O. A. Saprykin, Fausto Guarino, P. von Ballmoos, M. Ricci, J. Słomiński, T. Tymieniecka, H. Sato, J. Sledd, Valerie Connaughton, H. H. Silva Lopez, E. Kuznetsov, M. Putis, P. Baragatti, K. Higashide, C. Moretto, P. Galeotti, A. Sobey, Barbara Szabelska, R. Matev, Satoshi Wada, M. Nagata, T. Ogawa, Alexander Kusenko, A. Insolia, M. Kleifges, Gali Garipov, Ralph Engel, David B. Cline, J. F. Valdés-Galicia, L. G. Tkachev, S. Csorna, C. Tenzer, J. S. Kim, D. Maravilla, Yoshimasa Kurihara, T. Peter, H. Schieler, T. Sugiyama, G. Vankova, O. Martinez, K. Słomińska, V. S. Morozenko, Mitsuteru Sato, Francesco Isgrò, Angela V. Olinto, Tadeusz Wibig, Fernando López, Andrea Santangelo, E. G. Judd, B. Keilhauer, Katsuhiko Tsuno, Alfonso Monaco, Graciela B. Gelmini, D. Campana, T. Shibata, Taka Tomida, C. Blaksley, Frederic Trillaud, Y. Hachisu, Dmitry V. Naumov, Y. Arai, I. Kreykenbohm, Vladimir Andreev, Tokonatsu Yamamoto, K. Mase, R. Young, Frederic Jean Ronga, I. Rodríguez, Tomás Belenguer, S. Biktemerova, M. Sakata, C. Lachaud, Inkyu Park, S. Dagoret-Campagne, B. Mot, Y. Yamamoto, T. Shirahama, J.N. Capdevielle, Francesco Fenu, G. Catalano, S. Ahmad, N. Tajima, Piero Vallania, Y. Miyazaki, M. D. Sabau, Shigehiro Nagataki, J. Fujimoto, S. Falk, R. Bechini, Yukihiro Takahashi, M. Ave Pernas, C. González Alvarado, Pierre Barrillon, Ke Fang, Mark Christl, O. Tibolla, Marco Casolino, Claudio Fornaro, Z. Włodarczyk, Humberto Ibarguen Salazar, D. Ikeda, F. Sarazin, Piotr Orleanski, Silvia Ferrarese, H. J. Crawford, J. Bayer, Sergei A. Sharakin, J. Hernández Carretero, Mikhail Panasyuk, M. Unger, C. De Santis, Marc Weber, Shigeto Watanabe, J. Błȩcki, H. Tokuno, C. de la Taille, G. Roudil, B. Harlov, H. Lim, Carlo Vigorito, M. C. Maccarone, K. Kudela, M. Sanz Palomino, K. Katahira, L. Santiago Crúz, Jianyi Yang, M. Dupieux, Patrick J. Reardon, Toshiki Tajima, G. Siemieniec-Oziȩbło, G. Masciantonio, Hitoshi Ohmori, R. Nava, Y. Karadzhov, N. Sakaki, M. Serra, Luis A. Anchordoqui, L. Valore, Rossella Caruso, Yoshiya Kawasaki, Simona Toscano, T. Batsch, H. Prieto, R. Cremonini, R. Tsenov, D. Allard, Guillaume Prévôt, Andrii Neronov, S. Selmane, M. E. Bertaina, A. Pollini, Pavel Klimov, I. Kaneko, Ken'ichi Nomoto, F. Tajima, Yoshitaka Itow, P. Gorodetzky, A. Anzalone, M. Bogomilov, T. Napolitano, M. Wille, M. Nagano Murakami, Y. Uchihori, K. Belov, F. Kajino, A. Ebersoldt, C. Catalano, H. W. Park, Yoshiki Tsunesada, Hajime Takami, Masaki Fukushima, T. Nakamura, N. Tone, Daisuke Yonetoku, M. Yu. Zotov, Susana Briz, M. D. Rodríguez Frías, Z. Plebaniak, J. Blümer, Michiyuki Chikawa, Hajime Yano, P. L. Biermann, D. Supanitsky, I. Rusinov, J. Geary, N. De Simone, Marcos Reyes, Shoichi Ogio, A. Jung, T. Paul, K. Yoshida, S. Sánchez, B. A. Khrenov, H. Miyamoto, G. Medina-Tanco, N. Inoue, L. del Peral, A. Franceschi, E. Parizot, Pavol Bobik, J. A. Morales de los Ríos, Susumu Inoue, Ovidiu Vaduvescu, M. Lacombe, Claudio Cassardo, Dmitri Semikoz, T. Mernik, I. V. Yashin, L. Marcelli, Thomas J. Weiler, S. Perez Cano, Kenji Shinozaki, A. Bruno, Karl Mannheim, Michael S. Briggs, A. J. de Castro, K. Kawai, T. Patzak, Akinori Saito, G. Distratis, F. Cafagna, G. Modestino, E. Joven, Adams, J. H., 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., Błȩcki, J., Blin Bondil, S., Blã¼mer, 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., FernÃ¡ndez GÃ³mez, 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., GonzÃ¡lez Alvarado, C., Gorodetzky, P., Guarino, Fausto, Guzmã¡n, A., Hachisu, Y., Harlov, B., Haungs, A., HernÃ¡ndez Carretero, J., Higashide, K., Ikeda, D., Ikeda, H., Inoue, N., Inoue, S., Insolia, A., Isgro', Francesco, 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., 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., Lã³pez, 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 RÃos, J. A., Moretto, C., Morozenko, V. S., Mot, B., Murakami, T., Murakami, M. Nagano, 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., Orleański, 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., Prã©vã´t, G., Prieto, H., Putis, M., Reardon, P., Reyes, M., Ricci, M., Rodrãguez, I., RodrÃguez FrÃas, M. D., Ronga, F., Roth, M., Rothkaehl, H., Roudil, G., Rusinov, I., Rybczyński, M., Sabau, M. D., SÃ¡ez Cano, G., Sagawa, H., Saito, A., Sakaki, N., Sakata, M., Salazar, H., Sã¡nchez, S., Santangelo, A., Santiago CrÃºz, 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 Oziȩbło, G., Silva LÃ³pez, H. H., Sledd, J., Słomińska, 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., ValdÃ©s Galicia, J. F., Vallania, P., Valore, Laura, Vankova, G., Vigorito, C., Villaseã±or, L., von Ballmoos, P., Wada, S., Watanabe, J., Watanabe, S., Watts, J., Weber, M., Weiler, T. J., Wibig, T., Wiencke, L., Wille, M., Wilms, J., Włodarczyk, Z., Yamamoto, T., Yamamoto, Y., Yang, J., Yano, H., Yashin, I. V., Yonetoku, D., Yoshida, K., Yoshida, S., Young, R., Zotov, M. Y. u., Zuccaro Marchi, A., and Słomiński, J.
Subjects: Atmospheric physics, Ciencias Físicas, Space Shuttle, Cosmic ray, Elves, Jets - Atmospheric phenomena, Sprites, Transient Luminous Events, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, ELVES, Elve, Transient Luminous Events, Elves, Sprites, Jets - Atmospheric phenomena, law.invention, Telescope, purl.org/becyt/ford/1 [https], law, International Space Station, Ultra-high-energy cosmic ray, Astrophysique, Physics, Astronomy, purl.org/becyt/ford/1.3 [https], Astronomie, Astronomy and Astrophysic, Sciences de l'espace, Astronomía, Moment (physics), Sprite, Satellite, Transient Luminous Event, CIENCIAS NATURALES Y EXACTAS
Abstract: 注記: The JEM-EUSO Collaboration 289名 [所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS) 池田, 博一; 鈴木, 睦; 矢野, 創], Accepted: 2014-11-17, Note: The JEM-EUSO Collaboration 289members [Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS) Ikeda, Hirokazu; Suzuki, Makoto; Yano, Hajime], 資料番号: SA1150236000
Published: 2015

100. INTEGRAL and XMM-Newton observations of LSI +61 303

Author: R. Walter, Maria Chernyakova, and Andrii Neronov
Subjects: Physics, Spectral index, Photon, Be star, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Compact star, Rotation, Neutron star, Pulsar, Space and Planetary Science
Abstract: LSI +61 303 is one of the few X-ray binaries with Be star companion from which both radio and high-energy gamma-ray emission have been observed. We present XMM-Newton and INTEGRAL observations which reveal variability of the X-ray spectral index of the system. The X-ray spectrum is hard (photon index ~ 1.5) during the orbital phases of both high and low X-ray flux. However, the spectrum softens at the moment of transition from high to low X-ray state. The spectrum of the system in the hard X-ray band does not reveal the presence of a cut-off (or, at least a spectral break) at 10-60 keV energies, expected if the compact object is an accreting neutron star. The observed spectrum and spectral variability can be explained if the compact object in the system is a rotation powered pulsar., Comment: 8 pages, accepted to MNRAS
Published: 2006

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