P. Galeotti - INFN-Torino & Univ.Torino, Italy

P. Galeotti
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Name
P. Galeotti
Affiliation
INFN-Torino & Univ.Torino, Italy
City
Turin
Country
Italy

Pubs By Year

Pub Categories

 
High Energy Astrophysical Phenomena (9)
 
Astrophysics (9)
 
High Energy Physics - Experiment (7)
 
High Energy Physics - Phenomenology (4)
 
Instrumentation and Methods for Astrophysics (4)
 
General Relativity and Quantum Cosmology (2)
 
Physics - Instrumentation and Detectors (1)
 
Physics - General Physics (1)
 
Solar and Stellar Astrophysics (1)

Publications Authored By P. Galeotti

The Extreme Energy Events Project is a synchronous sparse array of 52 tracking detectors for studying High Energy Cosmic Rays (HECR) and Cosmic Rays-related phenomena. The observatory is also meant to address Long Distance Correlation (LDC) phenomena: the network is deployed over a broad area covering 10 degrees in latitude and 11 in longitude. An overview of a set of preliminary results is given, extending from the study of local muon flux dependance on solar activity to the investigation of the upward-going component of muon flux traversing the EEE stations; from the search for anisotropies at the sub-TeV scale to the hints for observations of km-scale Extensive Air Shower (EAS). Read More

Two major problems, still associated with the SN1987A, are: a) the signals observed with the gravitational waves detectors, b) the duration of the collapse. Indeed, a) the sensitivity of the gravitational wave detectors seems to be small for detecting gravitational waves and, b) while some experimental data indicate a duration of order of hours, most theories assume that the collapse develops in a few seconds. Since recent data of the X-ray NuSTAR satellite show a clear evidence of an asymmetric collapse, we have revisited the experimental data recorded by the underground and gravitational wave detectors running during the SN1987A. Read More

The Large Volume Detector (LVD) has been continuously taking data since 1992 at the INFN Gran Sasso National Laboratory. LVD is sensitive to neutrino bursts from gravitational stellar collapses with full detection probability over the Galaxy. We have searched for neutrino bursts in LVD data taken in 7335 days of operation. Read More

2013Nov
Affiliations: 1LVD Collaboration, 2LVD Collaboration, 3LVD Collaboration, 4LVD Collaboration, 5LVD Collaboration, 6LVD Collaboration, 7LVD Collaboration, 8LVD Collaboration, 9LVD Collaboration, 10LVD Collaboration, 11LVD Collaboration, 12LVD Collaboration, 13LVD Collaboration, 14LVD Collaboration, 15LVD Collaboration, 16LVD Collaboration, 17LVD Collaboration, 18LVD Collaboration, 19LVD Collaboration, 20LVD Collaboration, 21LVD Collaboration, 22LVD Collaboration, 23LVD Collaboration, 24LVD Collaboration, 25LVD Collaboration, 26LVD Collaboration, 27LVD Collaboration, 28LVD Collaboration, 29LVD Collaboration, 30LVD Collaboration, 31LVD Collaboration

The charge ratio ${k \equiv \mu^+/\mu^-}$ for atmospheric muons has been measured using Large Volume Detector (LVD) in the INFN Gran Sasso National Laboratory, Italy (minimal depth is 3000 m w.e.). Read More

2013May
Authors: J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, M. Ambrosio, L. Anchordoqui, A. Anzalone, Y. Arai, C. Aramo, K. Asano, M. Ave, P. Barrillon, T. Batsch, J. Bayer, T. Belenguer, R. Bellotti, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, V. Connaughton, J. F. Cortes, H. J. Crawford, R. Cremonini, S. Csorna, J. C. D'Olivo, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, L. del Peral, A. Dell'Oro, M. P. De Pascale, M. Di Martino, G. Distratis, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, A. Franceschi, J. Fujimoto, P. Galeotti, G. Garipov, J. Geary, U. G. Giaccari, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, T. Iguchi, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgrio, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, S. H. Ko, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, E. Kuznetsov, G. La Rosa, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, L. Marcelli, A. Marini, G. Martin-Chassard, O. Martinez, G. Masciantonio, K. Mase, R. Matev, A. Maurissen, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, D. Monnier-Ragaigne, J. A. Morales de los Rios, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, J. W. Nam, S. Nam, K. Nam, T. Napolitano, D. Naumov, A. Neronov, K. Nomoto, T. Ogawa, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, N. Pacheco, M. I. Panasyuk, E. Parizot, I. H. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, T. Peter, P. Picozza, A. Pollini, H. Prieto, P. Reardon, M. Reina, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, M. Scuderi, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieb, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, T. Tomida, N. Tone, F. Trillaud, R. Tsenov, K. Tsuno, T. Tymieniecka, Y. Uchihori, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, A. Zamora, A. Zuccaro Marchi

We evaluate the exposure during nadir observations with JEM-EUSO, the Extreme Universe Space Observatory, on-board the Japanese Experiment Module of the International Space Station. Designed as a mission to explore the extreme energy Universe from space, JEM-EUSO will monitor the Earth's nighttime atmosphere to record the ultraviolet light from tracks generated by extensive air showers initiated by ultra-high energy cosmic rays. In the present work, we discuss the particularities of space-based observation and we compute the annual exposure in nadir observation. Read More

2012Aug
Affiliations: 1The LVD Collaboration, 2The LVD Collaboration, 3The LVD Collaboration, 4The LVD Collaboration, 5The LVD Collaboration, 6The LVD Collaboration, 7The LVD Collaboration, 8The LVD Collaboration, 9The LVD Collaboration, 10The LVD Collaboration, 11The LVD Collaboration, 12The LVD Collaboration, 13The LVD Collaboration, 14The LVD Collaboration, 15The LVD Collaboration, 16The LVD Collaboration, 17The LVD Collaboration, 18The LVD Collaboration, 19The LVD Collaboration, 20The LVD Collaboration, 21The LVD Collaboration, 22The LVD Collaboration, 23The LVD Collaboration, 24The LVD Collaboration, 25The LVD Collaboration, 26The LVD Collaboration, 27The LVD Collaboration, 28The LVD Collaboration, 29The LVD Collaboration, 30The LVD Collaboration

We report the measurement of the time-of-flight of ~17 GeV muon neutrinos on the CNGS baseline (732 km) with the Large Volume Detector (LVD) at the Gran Sasso Laboratory. The CERN-SPS accelerator has been operated from May 10th to May 24th 2012, with a tightly bunched-beam structure to allow the velocity of neutrinos to be accurately measured on an event-by-event basis. LVD has detected 48 neutrino events, associated to the beam, with a high absolute time accuracy. Read More

2012Apr
Authors: The JEM-EUSO Collaboration, :, J. H. Adams Jr, S. Ahmad, J. -N. Albert, D. Allard, M. Ambrosio, L. Anchordoqui, A. Anzalone, Y. Arai, C. Aramo, K. Asano, P. Barrillon, T. Batsch, J. Bayer, T. Belenguer, R. Bellotti, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, V. Connaughton, J. F. Cortes, H. J. Crawford, R. Cremonini, S. Csorna, J. C. D'Olivo, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, M. P. De Pascale, L. del Peral, A. Dell'Oro, M. Di Martino, G. Distrati, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, S. Ferrarese, I. Fernandez-Gomez, A. Franceschi, J. Fujimoto, P. Galeotti, G. Garipov, J. Geary, U. G. Giaccari, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, T. Iguchi, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, S. H. Ko, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, E. Kuznetsov, G. La Rosa, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, L. Marcelli, A. Marini, G. Martin-Chassard, O. Martinez, G. Masciantonio, K. Mase, R. Matev, A. Maurissen, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, D. Monnier-Ragaigne, J. A. Morales de los Rıos, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, J. W. Nam, S. Nam, K. Nam, T. Napolitano, D. Naumov, A. Neronov, K. Nomoto, T. Ogawa, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, N. Pacheco, M. I. Panasyuk, E. Parizot, I. H. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, T. Peter, P. Picozza, A. Pollini, H. Prieto, P. Reardon, M. Reina, M. Reyes, M. Ricci, I. Rodrıguez, M. D. Rodrıguez Frıas, F. Ronga, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, M. Scuderi, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, H. Takami, T. Nakamura, M. Takeda, Y. Takahashi, Y. Takizawa, C. Tenzer, L. Tkachev, T. Tomida, N. Tone, F. Trillaud, R. Tsenov, K. Tsuno, T. Tymieniecka, Y. Uchihori, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts Jr, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, A. Zamora, A. Zuccaro Marchi

Contributions of the JEM-EUSO Collaboration to the 32nd International Cosmic Ray Conference, Beijing, August, 2011. Read More

ARGO-YBJ is an air shower detector array with a fully covered layer of resistive plate chambers. It is operated with a high duty cycle and a large field of view. It continuously monitors the northern sky at energies above 0. Read More

2011Jan
Authors: G. Aielli1, C. Bacci2, B. Bartoli3, P. Bernardini4, X. J. Bi5, C. Bleve6, P. Branchini7, A. Budano8, S. Bussino9, A. K. Calabrese Melcarne10, P. Camarri11, Z. Cao12, A. Cappa13, R. Cardarelli14, S. Catalanotti15, C. Cattaneo16, P. Celio17, S. Z. Chen18, T. L. Chen19, Y. Chen20, P. Creti21, S. W. Cui22, B. Z. Dai23, G. D'Alí Staiti24, Danzengluobu25, M. Dattoli26, I. De Mitri27, B. D'Ettorre Piazzoli28, M. De Vincenzi29, T. Di Girolamo30, X. H. Ding31, G. Di Sciascio32, C. F. Feng33, Z. Y. Feng34, Zhenyong Feng35, F. Galeazzi36, P. Galeotti37, R. Gargana38, Q. B. Gou39, Y. Q. Guo40, H. H. He41, Haibing Hu42, Hongbo Hu43, Q. Huang44, M. Iacovacci45, R. Iuppa46, I. James47, H. Y. Jia48, Labaciren49, H. J. Li50, J. Y. Li51, X. X. Li52, B. Liberti53, G. Liguori54, C. Liu55, C. Q. Liu56, M. Y. Liu57, J. Liu58, H. Lu59, X. H. Ma60, G. Mancarella61, S. M. Mari62, G. Marsella63, D. Martello64, S. Mastroianni65, X. R. Meng66, P. Montini67, C. C. Ning68, A. Pagliaro69, M. Panareo70, L. Perrone71, P. Pistilli72, X. B. Qu73, E. Rossi74, F. Ruggieri75, L. Saggese76, P. Salvini77, R. Santonico78, P. R. Shen79, X. D. Sheng80, F. Shi81, C. Stanescu82, A. Surdo83, Y. H. Tan84, P. Vallania85, S. Vernetto86, C. Vigorito87, B. Wang88, H. Wang89, C. Y. Wu90, H. R. Wu91, Z. G. Yao92, B. Xu93, L. Xue94, Y. X. Yan95, Q. Y. Yang96, X. C. Yang97, A. F. Yuan98, M. Zha99, H. M. Zhang100, JiLong Zhang101, JianLi Zhang102, L. Zhang103, P. Zhang104, X. Y. Zhang105, Y. Zhang106, Zhaxisangzhu107, Zhaxiciren108, X. X. Zhou109, F. R. Zhu110, Q. Q. Zhu111, G. Zizzi112
Affiliations: 1The ARGO-YBJ Collaboration, 2The ARGO-YBJ Collaboration, 3The ARGO-YBJ Collaboration, 4The ARGO-YBJ Collaboration, 5The ARGO-YBJ Collaboration, 6The ARGO-YBJ Collaboration, 7The ARGO-YBJ Collaboration, 8The ARGO-YBJ Collaboration, 9The ARGO-YBJ Collaboration, 10The ARGO-YBJ Collaboration, 11The ARGO-YBJ Collaboration, 12The ARGO-YBJ Collaboration, 13The ARGO-YBJ Collaboration, 14The ARGO-YBJ Collaboration, 15The ARGO-YBJ Collaboration, 16The ARGO-YBJ Collaboration, 17The ARGO-YBJ Collaboration, 18The ARGO-YBJ Collaboration, 19The ARGO-YBJ Collaboration, 20The ARGO-YBJ Collaboration, 21The ARGO-YBJ Collaboration, 22The ARGO-YBJ Collaboration, 23The ARGO-YBJ Collaboration, 24The ARGO-YBJ Collaboration, 25The ARGO-YBJ Collaboration, 26The ARGO-YBJ Collaboration, 27The ARGO-YBJ Collaboration, 28The ARGO-YBJ Collaboration, 29The ARGO-YBJ Collaboration, 30The ARGO-YBJ Collaboration, 31The ARGO-YBJ Collaboration, 32The ARGO-YBJ Collaboration, 33The ARGO-YBJ Collaboration, 34The ARGO-YBJ Collaboration, 35The ARGO-YBJ Collaboration, 36The ARGO-YBJ Collaboration, 37The ARGO-YBJ Collaboration, 38The ARGO-YBJ Collaboration, 39The ARGO-YBJ Collaboration, 40The ARGO-YBJ Collaboration, 41The ARGO-YBJ Collaboration, 42The ARGO-YBJ Collaboration, 43The ARGO-YBJ Collaboration, 44The ARGO-YBJ Collaboration, 45The ARGO-YBJ Collaboration, 46The ARGO-YBJ Collaboration, 47The ARGO-YBJ Collaboration, 48The ARGO-YBJ Collaboration, 49The ARGO-YBJ Collaboration, 50The ARGO-YBJ Collaboration, 51The ARGO-YBJ Collaboration, 52The ARGO-YBJ Collaboration, 53The ARGO-YBJ Collaboration, 54The ARGO-YBJ Collaboration, 55The ARGO-YBJ Collaboration, 56The ARGO-YBJ Collaboration, 57The ARGO-YBJ Collaboration, 58The ARGO-YBJ Collaboration, 59The ARGO-YBJ Collaboration, 60The ARGO-YBJ Collaboration, 61The ARGO-YBJ Collaboration, 62The ARGO-YBJ Collaboration, 63The ARGO-YBJ Collaboration, 64The ARGO-YBJ Collaboration, 65The ARGO-YBJ Collaboration, 66The ARGO-YBJ Collaboration, 67The ARGO-YBJ Collaboration, 68The ARGO-YBJ Collaboration, 69The ARGO-YBJ Collaboration, 70The ARGO-YBJ Collaboration, 71The ARGO-YBJ Collaboration, 72The ARGO-YBJ Collaboration, 73The ARGO-YBJ Collaboration, 74The ARGO-YBJ Collaboration, 75The ARGO-YBJ Collaboration, 76The ARGO-YBJ Collaboration, 77The ARGO-YBJ Collaboration, 78The ARGO-YBJ Collaboration, 79The ARGO-YBJ Collaboration, 80The ARGO-YBJ Collaboration, 81The ARGO-YBJ Collaboration, 82The ARGO-YBJ Collaboration, 83The ARGO-YBJ Collaboration, 84The ARGO-YBJ Collaboration, 85The ARGO-YBJ Collaboration, 86The ARGO-YBJ Collaboration, 87The ARGO-YBJ Collaboration, 88The ARGO-YBJ Collaboration, 89The ARGO-YBJ Collaboration, 90The ARGO-YBJ Collaboration, 91The ARGO-YBJ Collaboration, 92The ARGO-YBJ Collaboration, 93The ARGO-YBJ Collaboration, 94The ARGO-YBJ Collaboration, 95The ARGO-YBJ Collaboration, 96The ARGO-YBJ Collaboration, 97The ARGO-YBJ Collaboration, 98The ARGO-YBJ Collaboration, 99The ARGO-YBJ Collaboration, 100The ARGO-YBJ Collaboration, 101The ARGO-YBJ Collaboration, 102The ARGO-YBJ Collaboration, 103The ARGO-YBJ Collaboration, 104The ARGO-YBJ Collaboration, 105The ARGO-YBJ Collaboration, 106The ARGO-YBJ Collaboration, 107The ARGO-YBJ Collaboration, 108The ARGO-YBJ Collaboration, 109The ARGO-YBJ Collaboration, 110The ARGO-YBJ Collaboration, 111The ARGO-YBJ Collaboration, 112The ARGO-YBJ Collaboration

The sun blocks cosmic ray particles from outside the solar system, forming a detectable shadow in the sky map of cosmic rays detected by the ARGO-YBJ experiment in Tibet. Because the cosmic ray particles are positive charged, the magnetic field between the sun and the earth deflects them from straight trajectories and results in a shift of the shadow from the true location of the sun. Here we show that the shift measures the intensity of the field which is transported by the solar wind from the sun to the earth. Read More

The proton-air inelastic cross section value \sigmapairin=338$\pm$21({\it stat})$\pm$19({\it syst})-28({\it syst}) mb at $\sqrt{s} \approx $ 2 TeV has been measured by the EAS-TOP Extensive Air Shower experiment. The absorption length of cosmic ray proton primaries cascades reaching the maximum development at the observation level is obtained from the flux attenuation for different zenith angles (i.e. Read More

2009Jan
Affiliations: 1The EAS-TOP Collaboration, 2The EAS-TOP Collaboration, 3The EAS-TOP Collaboration, 4The EAS-TOP Collaboration, 5The EAS-TOP Collaboration, 6The EAS-TOP Collaboration, 7The EAS-TOP Collaboration, 8The EAS-TOP Collaboration, 9The EAS-TOP Collaboration, 10The EAS-TOP Collaboration, 11The EAS-TOP Collaboration, 12The EAS-TOP Collaboration, 13The EAS-TOP Collaboration, 14The EAS-TOP Collaboration, 15The EAS-TOP Collaboration, 16The EAS-TOP Collaboration, 17The EAS-TOP Collaboration, 18The EAS-TOP Collaboration, 19The EAS-TOP Collaboration, 20The EAS-TOP Collaboration, 21The EAS-TOP Collaboration, 22The EAS-TOP Collaboration, 23The EAS-TOP Collaboration, 24The EAS-TOP Collaboration, 25The EAS-TOP Collaboration, 26The EAS-TOP Collaboration

The amplitude and phase of the cosmic ray anisotropy are well established experimentally between 10^{11} eV and 10^{14} eV. The study of their evolution into the energy region 10^{14}-10^{16} eV can provide a significant tool for the understanding of the steepening ("knee") of the primary spectrum. In this letter we extend the EAS-TOP measurement performed at E_0 around 10^{14} eV, to higher energies by using the full data set (8 years of data taking). Read More

We re-examine the data taken by the neutrino detectors during the supernova SN1987A. It is found that the Kamiokande data, in addition to the well known burst at 7:35 hours UT, show another one at 7:54 hours, with seven pulses in 6.2 seconds. Read More

The CERN Neutrino to Gran Sasso (CNGS) project aims to produce a high energy, wide band $\nu_{\mu}$ beam at CERN and send it toward the INFN Gran Sasso National Laboratory (LNGS), 732 km away. Its main goal is the observation of the $\nu_{\tau}$ appearance, through neutrino flavour oscillation. The beam started its operation in August 2006 for about 12 days: a total amount of $7. Read More

2007Jul
Affiliations: 1IASF-Palermo/INAF, Italy, 2LIP-Lisbon, Portugal, 3IASF-Palermo/INAF, Italy, 4LIP-Lisbon, Portugal, 5IFSI-Torino/INAF & INFN-Torino, Italy, 6IASF-Palermo/INAF & INFN-Catania, Italy, 7LPSC-Grenoble, France, 8IASF-Palermo/INAF & DiFTeR/Univ.Palermo & INFN-Catania, Italy, 9IFSI-Torino/INAF & INFN-Torino & Univ.Torino, Italy, 10LIP-Lisbon, Portugal, 11INFN-Torino & Univ.Torino, Italy, 12INFN-Torino & Univ.Torino, Italy, 13IASF-Palermo/INAF & INFN-Catania, Italy, 14IASF-Palermo/INAF & INFN-Catania, Italy, 15IASF-Palermo/INAF & INFN-Catania, Italy, 16LPSC-Grenoble, France, 17IASF-Palermo/INAF & INFN-Catania, Italy, 18IASF-Palermo/INAF & INFN-Catania, Italy, 19LIP-Lisbon, Portugal, 20LPSC-Grenoble, France, 21LIP-Lisbon, Portugal, 22IASF-Palermo/INAF, Italy, 23INFN-Torino & Univ.Torino, Italy, 24IASF-Palermo/INAF & INFN-Catania, Italy, 25LIP-Lisbon, Portugal, 26LPSC-Grenoble, France, 27LIP-Lisbon, Portugal, 28IFSI-Torino/INAF & INFN-Torino, Italy, 29INFN-Torino & Univ.Torino, Italy
Category: Astrophysics

The study of Ultra High Energy Cosmic Rays represents one of the most challenging topic in the Cosmic Rays and in the Astroparticle Physics fields. The interaction of primary particles with atmospheric nuclei produces a huge Extensive Air Shower together with isotropic emission of UV fluorescence light and highly directional Cherenkov photons, that are reflected/diffused isotropically by the impact on the Earth's surface or on high optical depth clouds. For space-based observations, detecting the reflected Cherenkov signal in a delayed coincidence with the fluorescence light improves the accuracy of the shower reconstruction in space and in particular the measurement of the shower maximum, giving a strong signature for discriminating hadrons and neutrinos, and helping to estimate the primary chemical composition. Read More

The observations of supernova 1987A in underground detectors are revisited. It is shown that, while the LSD detector in the Mont Blanc Laboratory observed only one burst at 2h 52min 36.8sec U. Read More

The LVD detector, located in the INFN Gran Sasso National Laboratory (Italy), studies supernova neutrinos through the interactions with protons and carbon nuclei in the liquid scintillator and interactions with the iron nuclei of the support structure. We investigate the effect of neutrino oscillations in the signal expected in the LVD detector. The MSW effect has been studied in detail for neutrinos travelling through the collapsing star and the Earth. Read More

2006Feb
Affiliations: 1LPSC, 2LPSC, 3LPSC, 4LPSC, 5LPSC, 6LPSC, 7LPSC, 8LPSC, 9LPSC, 10LPSC, 11LPSC, 12LPSC, 13LPSC, 14LPSC, 15LPSC, 16LPSC, 17LPSC, 18LPSC, 19LPSC, 20LPSC, 21LPSC, 22LPSC, 23LPSC, 24LPSC, 25LPSC, 26LPSC
Category: Astrophysics

The detection of Cerenkov light from EAS in a delayed coincidence with fluorescence light gives a strong signature to discriminate protons and neutrinos in cosmic rays. For this purpose, the ULTRA experiment has been designed with 2 detectors: a small EAS array (ETscope) and an UV optical device including wide field (Belenos) and narrow field (UVscope) Cerenkov light detectors. The array measures the shower size and the arrival direction of the incoming EAS, while the UV devices, pointing both to zenith and nadir, are used to determine the amount of direct and diffused coincident Cerenkov light. Read More

GAW, acronym for Gamma Air Watch, is a path-finder experiment to test the feasibility of a new generation of imaging atmospheric Cherenkov telescopes that join high flux sensitivity with large field of view capability. GAW is conceived as an array of three identical imaging telescopes disposed at the vertexes of an equilateral triangle, about 80 m side. Two main features characterize GAW with respect to all the existing and presently planned ground-based Cherenkov telescopes. Read More

We report on a search for low-energy neutrino (antineutrino) bursts in correlation with the 8 time coincident events observed by the gravitational waves detectors EXPLORER and NAUTILUS (GWD) during the year 2001. The search, conducted with the LVD detector (INFN Gran Sasso National Laboratory, Italy), has considered several neutrino reactions, corresponding to different neutrino species, and a wide range of time intervals around the (GWD) observed events. No evidence for statistically significant correlated signals in LVD has been found. Read More

We present an update of our previous study (astro-ph/0112312) on how $\nu$ oscillations affect the signal from a supernova core collapse observed in the LVD detector at LNGS. In this paper we use a recent, more precise determination of the cross section (astro-ph/0302055) to calculate the expected number of inverse beta decay events, we introduce in the simulation also the $\nu$-{\rm Fe} interactions, we include the Earth matter effects and, finally, we study also the inverted mass hierarchy case. Read More

The importance of an adequate CNGS beam monitor at the Gran Sasso Laboratory has been stressed in many papers. Since the number of internal $\nu_\mu$ CC and NC interactions in the various detectors will not allow to collect statistics rapidly, one should also be able to detect the $\nu_\mu$ CC interactions in the upstream rock. In this study we have investigated the performances of the LVD detector as a monitor for the CNGS neutrino beam. Read More

We study the impact of neutrino oscillations on the supernova neutrino signal in the Large Volume Detector (LVD). The number of expected events for a galactic supernova (D=10 kpc) is calculated, assuming neutrino masses and mixing that explain solar and atmospheric neutrino results. The possibility to detect neutrinos in different channels makes LVD sensitive to different scenarios for neutrino properties, such as normal or inverted neutrino mass hierarchy, and/or adiabatic or non adiabatic MSW resonances associated to U(e3). Read More