Cosmic-Ray Anisotropies in Right Ascension Measured by the Pierre Auger Observatory

Autor(es):Mostrar menos -

Aab, A. ^[1] ; Abreu, P. ^{[2, 3]} ; Aglietta, M. ^{[4, 5]} ; Albuquerque, I. F. M. ^[6] ; Albury, J. M. ^[7] ; Allekotte, I. ^{[8, 9]} ; Almela, A. ^{[10, 11]} ; Alvarez Castillo, J. ^[12] ; Alvarez-Muniz, J. ^[13] ; Anastasi, G. A. ^{[4, 14]} ; Anchordoqui, L. ^[15] ; Andrada, B. ^[10] ; Andringa, S. ^{[2, 3]} ; Aramo, C. ^[16] ; Ferreira, P. R. Araujo ^[17] ; Asorey, H. ^[10] ; Assis, P. ^{[2, 3]} ; Avila, G. ^{[18, 19]} ; Badescu, A. M. ^[20] ; Bakalova, A. ^[21] ; Balaceanu, A. ^[22] ; Barbato, F. ^{[16, 23]} ; Barreira Luz, R. J. ^{[2, 3]} ; Becker, K. H. ^[24] ; Bellido, J. A. ^[7] ; Berat, C. ^[25] ; Bertaina, M. E. ^{[4, 14]} ; Bertou, X. ^{[8, 9]} ; Biermann, P. L. ^[26] ; Bister, T. ^[17] ; Biteau, J. ^[27] ; Blanco, A. ^{[2, 3]} ; Blazek, J. ^[21] ; Bleve, C. ^[25] ; Bohacova, M. ^[21] ; Boncioli, D. ^{[28, 29]} ; Bonifazi, C. ^[30] ; Bonneau Arbeletche, L. ^[6] ; Borodai, N. ^[31] ; Botti, A. M. ^{[10, 32]} ; Brack, J. ^{[33, 4]} ; Bretz, T. ^[17] ; Briechle, F. L. ^[17] ; Buchholz, P. ^[34] ; Bueno, A. ^{[35, 36]} ; Buitink, S. ^[37] ; Buscemi, M. ^{[38, 39]} ; Caballero-Mora, K. S. ^[40] ; Caccianiga, L. ^[41] ; Calcagni, L. ^{[42, 43]} ; Cancio, A. ^{[10, 11]} ; Canfora, F. ^{[1, 44]} ; Caracas, I. ^[24] ; Carceller, J. M. ^{[35, 36]} ; Caruso, R. ^{[38, 39]} ; Castellina, A. ^{[4, 5]} ; Catalani, F. ^[45] ; Cataldi, G. ^[46] ; Cazon, L. ^{[2, 3]} ; Cerda, M. ^[18] ; Chinellato, J. A. ^[47] ; Choi, K. ^[48] ; Chudoba, J. ^[21] ; Chytka, L. ^[49] ; Clay, R. W. ^[7] ; Cobos Cerutti, A. C. ^{[50, 51]} ; Colalillo, R. ^{[16, 23]} ; Coleman, A. ^[52] ; Coluccia, M. R. ^{[46, 53]} ; Conceicao, R. ^{[2, 3]} ; Condorelli, A. ^{[28, 54]} ; Consolati, G. ^{[55, 56]} ; Contreras, F. ^{[18, 19]} ; Convenga, F. ^{[46, 53]} ; Covault, C. E. ^[57] ; Dasso, S. ^{[58, 59, 60, 61]} ; Daumiller, K. ^[32] ; Dawson, B. R. ^[7] ; Day, J. A. ^[7] ; de Almeida, R. M. ^[62] ; de Jesus, J. ^{[10, 32]} ; de Jong, S. J. ^{[1, 44]} ; De Mauro, G. ^{[1, 44]} ; de Mello Neto, J. R. T. ^{[30, 63]} ; De Mitri, I. ^{[28, 54]} ; de Oliveira, J. ^[62] ; de Oliveira Franco, D. ^[47] ; de Souza, V. ^[64] ; Debatin, J. ^[65] ; del Rio, M. ^{[18, 19]} ; Deligny, O. ^[27] ; Dhital, N. ^[31] ; Di Matteo, A. ^[4] ; Diaz Castro, M. L. ^[47] ; Dobrigkeit, C. ^[47] ; D'Olivo, J. C. ^[12] ; Dorosti, Q. ^[34] ; dos Anjos, R. C. ^[66] ; Dova, M. T. ^{[42, 43]} ; Ebr, J. ^[21] ; Engel, R. ^{[32, 65]} ; Epicoco, I. ^{[46, 53]} ; Erdmann, M. ^[17] ; Escobar, C. O. ^[67] ; Etchegoyen, A. ^{[10, 11]} ; Falcke, H. ^{[1, 68, 44]} ; Farmer, J. ^[69] ; Farrar, G. ^[70] ; Fauth, A. C. ^[47] ; Fazzini, N. ^[67] ; Feldbusch, F. ^[71] ; Fenu, F. ^{[4, 14]} ; Fick, B. ^[72] ; Figueira, J. M. ^[10] ; Filipcic, A. ^{[73, 74]} ; Freire, M. M. ^{[75, 76]} ; Fujii, T. ^[69] ; Fuster, A. ^{[10, 11]} ; Galea, C. ^[1] ; Galelli, C. ^{[41, 55]} ; Garcia, B. ^{[50, 51]} ; Vegas, A. L. Garcia ^[17] ; Gemmeke, H. ^[71] ; Gesualdi, F. ^{[10, 32]} ; Gherghel-Lascu, A. ^[22] ; Ghia, P. L. ^[27] ; Giaccari, U. ^[1] ; Giammarchi, M. ^[55] ; Giller, M. ^[77] ; Glombitza, J. ^[17] ; Gobbi, F. ^[18] ; Golup, G. ^{[8, 9]} ; Gomez Berisso, M. ^{[8, 9]} ; Gomez Vitale, P. F. ^{[18, 19]} ; Gongora, J. P. ^[18] ; Gonzalez, N. ^[10] ; Goos, I. ^{[8, 32, 9]} ; Gora, D. ^[31] ; Gorgi, A. ^{[4, 5]} ; Gottowik, M. ^[24] ; Grubb, T. D. ^[7] ; Guarino, F. ^{[16, 23]} ; Guedes, G. P. ^[78] ; Guido, E. ^{[4, 14]} ; Hahn, S. ^{[10, 32]} ; Halliday, R. ^[57] ; Hampel, M. R. ^[10] ; Hansen, P. ^{[42, 43]} ; Harari, D. ^{[8, 9]} ; Harvey, V. M. ^[7] ; Haungs, A. ^[32] ; Hebbeker, T. ^[17] ; Heck, D. ^[32] ; Hill, G. C. ^[7] ; Hojvat, C. ^[67] ; Horandel, J. R. ^{[1, 44]} ; Horvath, P. ^[49] ; Hrabovsky, M. ^[49] ; Huege, T. ^{[32, 37]} ; Hulsman, J. ^{[10, 32]} ; Insolia, A. ^{[38, 39]} ; Isar, P. G. ^[79] ; Johnsen, J. A. ^[80] ; Jurysek, J. ^[21] ; Kaeaepae, A. ^[24] ; Kampert, K. H. ^[24] ; Keilhauer, B. ^[32] ; Kemp, J. ^[17] ; Klages, H. O. ^[32] ; Kleifges, M. ^[71] ; Kleinfeller, J. ^[18] ; Koepke, M. ^[65] ; Mezek, G. Kukec ^[74] ; Awad, A. Kuotb ^[65] ; Lago, B. L. ^[81] ; LaHurd, D. ^[57] ; Lang, R. G. ^[64] ; Leigui de Oliveira, M. A. ^[82] ; Lenok, V. ^[32] ; Letessier-Selvon, A. ^{[83, 84]} ; Lhenry-Yvon, I. ^[27] ; Lo Presti, D. ^{[38, 39]} ; Lopes, L. ^{[2, 3]} ; Lopez, R. ^[85] ; Lopez Casado, A. ^[13] ; Lorek, R. ^[57] ; Luce, Q. ^[65] ; Lucero, A. ^[10] ; Payeras, A. Machado ^[47] ; Malacari, M. ^[69] ; Mancarella, G. ^{[46, 53]} ; Mandat, D. ^[21] ; Manning, B. C. ^[7] ; Manshanden, J. ^[86] ; Mantsch, P. ^[67] ; Mariazzi, A. G. ^{[42, 43]} ; Maris, I. C. ^[48] ; Marsella, G. ^{[46, 53]} ; Martello, D. ^{[46, 53]} ; Martinez, H. ^[64] ; Martinez Bravo, O. ^[85] ; Mastrodicasa, M. ^{[28, 29]} ; Mathes, H. J. ^[32] ; Matthews, J. ^[87] ; Matthiae, G. ^{[88, 89]} ; Mayotte, E. ^[24] ; Mazur, P. O. ^[67] ; Medina-Tanco, G. ^[12] ; Melo, D. ^[10] ; Menshikov, A. ^[71] ; Merenda, K. -D. ^[80] ; Michal, S. ^[49] ; Micheletti, M. I. ^{[75, 76]} ; Miramonti, L. ^{[41, 55]} ; Mockler, D. ^[48] ; Mollerach, S. ^{[8, 9]} ; Montanet, F. ^[25] ; Morello, C. ^{[4, 5]} ; Morlino, G. ^{[28, 54]} ; Mostafa, M. ^[90] ; Mueller, A. L. ^{[10, 32]} ; Muller, M. A. ^{[47, 30]} ; Mueller, S. ^[65] ; Mussa, R. ^[4] ; Muzio, M. ^[70] ; Namasaka, W. M. ^[24] ; Nellen, L. ^[12] ; Niculescu-Oglinzanu, M. ^[22] ; Niechciol, M. ^[34] ; Nitz, D. ^[72] ; Nosek, D. ^[91] ; Novotny, V. ^[91] ; Nozka, L. ^[49] ; Nucita, A. ^{[46, 25, 53]} ; Nunez, L. A. ^[92] ; Palatka, M. ^[21] ; Pallotta, J. ^{[93, 94]} ; Panetta, M. P. ^{[46, 53]} ; Papenbreer, P. ^[24] ; Parente, G. ^[13] ; Parra, A. ^[85] ; Pech, M. ^[21] ; Pedreira, F. ^[13] ; Kala, J. P. ^[31] ; Pelayo, R. ^[95] ; Pena-Rodriguez, J. ^[92] ; Pereira, L. A. S. ^[47] ; Perez Armand, J. ^[6] ; Perlin, M. ^{[10, 32]} ; Perrone, L. ^{[46, 53]} ; Peters, C. ^[17] ; Petrera, S. ^{[28, 54]} ; Pierog, T. ^[32] ; Pimenta, M. ^{[2, 3]} ; Pirronello, V. ^{[38, 39]} ; Platino, M. ^[10] ; Pont, B. ^[1] ; Pothast, M. ^{[1, 44]} ; Privitera, P. ^[69] ; Prouza, M. ^[21] ; Puyleart, A. ^[72] ; Querchfeld, S. ^[24] ; Rautenberg, J. ^[24] ; Ravignani, D. ^[10] ; Reininghaus, M. ^{[10, 32]} ; Ridky, J. ^[21] ; Riehn, F. ^{[2, 3]} ; Risse, M. ^[34] ; Ristori, P. ^{[93, 94]} ; Rizi, V. ^{[28, 29]} ; Rodrigues de Carvalho, W. ^[6] ; Rodriguez Rojo, J. ^[18] ; Roncoroni, M. J. ^[10] ; Roth, M. ^[32] ; Roulet, E. ^{[8, 9]} ; Rovero, A. C. ^[59] ; Ruehl, P. ^[34] ; Saffi, S. J. ^[7] ; Saftoiu, A. ^[22] ; Salamida, F. ^{[28, 29]} ; Salazar, H. ^[85] ; Salina, G. ^[89] ; Sanabria Gomez, J. D. ^[92] ; Sanchez, F. ^[10] ; Santos, E. M. ^[6] ; Santos, E. ^[21] ; Sarazin, F. ^[80] ; Sarmento, R. ^{[2, 3]} ; Sarmiento-Cano, C. ^[10] ; Sato, R. ^[18] ; Savina, P. ^{[46, 27, 53]} ; Schaefer, C. ^[32] ; Scherini, V. ^[46] ; Schieler, H. ^[32] ; Schimassek, M. ^{[10, 65]} ; Schimp, M. ^[24] ; Schlueter, F. ^{[10, 32]} ; Schmidt, D. ^[65] ; Scholten, O. ^{[96, 37]} ; Schovanek, P. ^[21] ; Schroeder, F. G. ^{[32, 52]} ; Schroeder, S. ^[24] ; Sciutto, S. J. ^{[42, 43]} ; Scornavacche, M. ^{[10, 32]} ; Shellard, R. C. ^[97] ; Sigl, G. ^[86] ; Silli, G. ^{[10, 32]} ; Sima, O. ^[22] ; Smida, R. ^[69] ; Sommers, P. ^[90] ; Soriano, J. F. ^[15] ; Souchard, J. ^[25] ; Squartini, R. ^[18] ; Stadelmaier, M. ^{[10, 32]} ; Stanca, D. ^[22] ; Stanic, S. ^[74] ; Stasielak, J. ^[31] ; Stassi, P. ^[25] ; Streich, A. ^{[10, 65]} ; Suarez-Duran, M. ^[92] ; Sudholz, T. ^[7] ; Suomijarvi, T. ^[27] ; Supanitsky, A. D. ^[10] ; Supik, J. ^[49] ; Szadkowski, Z. ^[98] ; Taboada, A. ^{[10, 65]} ; Taborda, O. A. ^{[8, 9]} ; Tapia, A. ^[99] ; Timmermans, C. ^{[1, 44]} ; Tobiska, P. ^[21] ; Todero Peixoto, C. J. ^[45] ; Tome, B. ^{[2, 3]} ; Torralba Elipe, G. ^[13] ; Travaini, A. ^[18] ; Travnicek, P. ^[21] ; Trimarelli, C. ^{[28, 29]} ; Trini, M. ^[74] ; Tueros, M. ^{[42, 43]} ; Ulrich, R. ^[32] ; Unger, M. ^[32] ; Urban, M. ^[17] ; Vaclavek, L. ^[49] ; Valdes Galicia, J. F. ^[12] ; Valino, I. ^{[28, 54]} ; Valore, L. ^{[16, 23]} ; van Vliet, A. ^[1] ; Varela, E. ^[85] ; Vargas Cardenas, B. ^[12] ; Vasquez-Ramirez, A. ^[92] ; Veberic, D. ^[32] ; Ventura, C. ^[63] ; Vergara Quispe, I. D. ^{[42, 43]} ; Verzi, V. ^[89] ; Vicha, J. ^[21] ; Villasenor, L. ^[85] ; Vink, J. ^[100] ; Vorobiov, S. ^[74] ; Wahlberg, H. ^{[42, 43]} ; Watson, A. A. ^[101] ; Weber, M. ^[71] ; Weindl, A. ^[32] ; Wiencke, L. ^[80] ; Wilczynski, H. ^[31] ; Winchen, T. ^[37] ; Wirtz, M. ^[17] ; Wittkowski, D. ^[24] ; Wundheiler, B. ^[10] ; Yushkov, A. ^[21] ; Zas, E. ^[13] ; Zavrtanik, D. ^{[73, 74]} ; Zavrtanik, M. ^{[73, 74]} ; Zehrer, L. ^[74] ; Zepeda, A. ^[102] ; Ziolkowski, M. ^[34] ; Zuccarello, F. ^{[38, 39]} ; Collaboration, Pierre Auger

Afiliação do(s) autor(es):Mostrar menos -

^[1] Radboud Univ Nijmegen, IMAPP, Nijmegen - Netherlands

^[2] Univ Lisboa UL, Lab Instrumentacao & Fis Expt Particulas LIP, Lisbon - Portugal

^[3] Univ Lisboa UL, Inst Super Tecn IST, Lisbon - Portugal

^[4] INFN, Sez Torino, Turin - Italy

^[5] Osservatorio Astron Torino INAF, Turin - Italy

^[6] Univ Sao Paulo, Inst Fis, Sao Paulo, SP - Brazil

^[7] Univ Adelaide, Adelaide, SA - Australia

^[8] CNEA UNCuyo CONICET, Inst Balseiro, San Carlos De Bariloche, Rio Negro - Argentina

^[9] Ctr Atom Bariloche, San Carlos De Bariloche, Rio Negro - Argentina

^[10] UNSAM, CONICET, CNEA, Inst Tecnol Detecc & Astroparticulas, Buenos Aires, DF - Argentina

^[11] Univ Tecnol Nacl, Fac Reg Buenos Aires, Buenos Aires, DF - Argentina

^[12] Univ Nacl Autonoma Mexico, Mexico City, DF - Mexico

^[13] Univ Santiago de Compostela, Inst Galego Fis Altas Enerxias, Santiago De Compostela - Spain

^[14] Univ Torino, Dipartimento Fis, Turin - Italy

^[15] CUNY, Lehman Coll, Dept Phys & Astron, New York, NY - USA

^[16] INFN, Sez Napoli, Naples - Italy

^[17] Rhein Westfal TH Aachen, Inst Phys 3 A, Aachen - Germany

^[18] Observ Pierre Auger, Malargue - Argentina

^[19] Comis Nacl Energia Atom, Malargue - Argentina

^[20] Univ Politehn Bucuresti, Bucharest - Romania

^[21] Czech Acad Sci, Inst Phys, Prague - Czech Republic

^[22] Horia Hulubei Natl Inst Phys & Nucl Engn, Bucharest - Romania

^[23] Univ Napoli Federico II, Dipartimento Fis Ettore Pancini, Naples - Italy

^[24] Berg Univ Wuppertal, Dept Phys, Wuppertal - Germany

^[25] Univ Grenoble Alpes, Grenoble Inst Engn, CNRS, LPSC IN2P3, F-38000 Grenoble - France

^[26] Max Planck Inst Radioastron, Bonn - Germany

^[27] Univ Paris Sud, Inst Phys Nucl Orsay IPNO, Univ Paris Saclay, CNRS IN2P3, Orsay - France

^[28] INFN, Lab Nazl Gran Sasso, Assergi LAquila - Italy

^[29] Univ Aquila, Dipartimento Sci Fis & Chim, Laquila - Italy

^[30] Univ Fed Rio de Janeiro, Inst Fis, Rio De Janeiro, RJ - Brazil

^[31] Inst Nucl Phys PAN, Krakow - Poland

^[32] Karlsruhe Inst Technol, Inst Kernphys, Karlsruhe - Germany

^[33] Colorado State Univ, Ft Collins, CO 80523 - USA

^[34] Univ Siegen, Fachbereich Phys Expt Teilchenphys 7, Siegen - Germany

^[35] Univ Granada, Granada - Spain

^[36] CAFPE, Granada - Spain

^[37] Vrije Univ Brussels, Brussels - Belgium

^[38] Univ Catania, Dipartimento Fis & Astron, Catania - Italy

^[39] INFN, Sez Catania, Catania - Italy

^[40] Univ Autonoma Chiapas, Tuxtla Gutierrez, Chiapas - Mexico

^[41] Univ Milan, Dipartimento Fis, Milan - Italy

^[42] Consejo Nacl Invest Cient & Tecn, La Plata - Argentina

^[43] Univ Nacl La Plata, IFLP, La Plata - Argentina

^[44] Natl Inst Kernfys & Hoge Energie Fys NIKHEF, Sci Pk, Amsterdam - Netherlands

^[45] Univ Sao Paulo, Escola Engn Lorena, Lorena, SP - Brazil

^[46] INFN, Sez Lecce, Lecce - Italy

^[47] Univ Estadual Campinas, IFGW, Campinas, SP - Brazil

^[48] Univ Libre Bruxelles ULB, Brussels - Belgium

^[49] Palacky Univ, RCPTM, Olomouc - Czech Republic

^[50] UNSAM, CONICET, CNEA, Inst Tecnol Detecc & Astroparticulas, Mendoza - Argentina

^[51] Univ Tecnol Nacl, CNEA, CONICET, Fac Reg Mendoza, Mendoza - Argentina

^[52] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 - USA

^[53] Univ Salento, Dipartimento Matemat & Fis E Giorgi, Lecce - Italy

^[54] Gran Sasso Sci Inst, Laquila - Italy

^[55] INFN, Sez Milano, Milan - Italy

^[56] Politecn Milan, Dipartimento Sci & Tecnol Aerosp, Milan - Italy

^[57] Case Western Reserve Univ, Cleveland, OH 44106 - USA

^[58] Univ Buenos Aires, Dept Fis, Buenos Aires, DF - Argentina

^[59] CONICET UBA, IAFE, Inst Astron & Fis Espacio, Buenos Aires, DF - Argentina

^[60] Univ Buenos Aires, FCEyN, Dept Ciencias Atmosfera & Oceanos, Buenos Aires, DF - Argentina

^[61] Univ Buenos Aires, CONICET, Buenos Aires, DF - Argentina

^[62] Univ Fed Fluminense, EEIMVR, Volta Redonda, RJ - Brazil

^[63] Univ Fed Rio de Janeiro UFRJ, Observ Valongo, Rio De Janeiro, RJ - Brazil

^[64] Univ Sao Paulo, Inst Fis Sao Carlos, Sao Carlos, SP - Brazil

^[65] Karlsruhe Inst Technol, Inst Expt Particle Phys ETP, Karlsruhe - Germany

^[66] Univ Fed Parana, Setor Palotina, Palotina - Brazil

^[67] Fermilab Natl Accelerator Lab, Batavia, IL 60510 - USA

^[68] Stichting Astron Onderzoek Nederland ASTRON, Dwingeloo - Netherlands

^[69] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 - USA

^[70] NYU, New York, NY - USA

^[71] Karlsruhe Inst Technol, Inst Prozessdatenverarbeitung & Elekt, Karlsruhe - Germany

^[72] Michigan Technol Univ, Houghton, MI 49931 - USA

^[73] J Stefan Inst, Expt Particle Phys Dept, Ljubljana - Slovenia

^[74] Univ Nova Gorica, Ctr Astrophys & Cosmol CAC, Nova Gorica - Slovenia

^[75] UNR, CONICET, Inst Fis Rosario IFIR, Rosario - Argentina

^[76] UNR, Fac Ciencias Bioquim & Farmaceut, Rosario - Argentina

^[77] Univ Lodz, Fac Astrophys, Lodz - Poland

^[78] Univ Estadual Feira de Santana, Feira De Santana - Brazil

^[79] Inst Space Sci, Bucharest - Romania

^[80] Colorado Sch Mines, Golden, CO 80401 - USA

^[81] Ctr Fed Educ Tecnol Celso Suckow Fonseca, Nova Friburgo - Brazil

^[82] Univ Fed ABC, Santo Andre, SP - Brazil

^[83] Univ Paris 06, Lab Phys Nucl & Hautes Energies LPNHE, CNRS IN2P3, Paris - France

^[84] Univ Paris 07, Lab Phys Nucl & Hautes Energies LPNHE, CNRS IN2P3, Paris - France

^[85] Benemerita Univ Autonoma Puebla, Puebla - Mexico

^[86] Univ Hamburg, Inst Theoret Phys 2, Hamburg - Germany

^[87] Louisiana State Univ, Baton Rouge, LA 70803 - USA

^[88] Univ Roma Tor Vergata, Dipartimento Fis, Rome - Italy

^[89] INFN, Sez Roma Tor Vergata, Rome - Italy

^[90] Penn State Univ, University Pk, PA 16802 - USA

^[91] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, Prague - Czech Republic

^[92] Univ Ind Santander, Bucaramanga - Colombia

^[93] Consejo Nacl Invest Cient & Tecn, Villa Martelli - Argentina

^[94] CITEDEF, Ctr Invest Laseres & Aplicac, Villa Martelli - Argentina

^[95] Inst Politecn Nacl UPIITA IPN, Unidad Profes Interdisciplinaria Ingn & Tecnol Av, Mexico City, DF - Mexico

^[96] Univ Groningen, KVI Ctr Adv Radiat Technol, Groningen - Netherlands

^[97] Ctr Brasileiro Pesquisas Fis, Rio De Janeiro, RJ - Brazil

^[98] Univ Lodz, Fac High Energy Astrophys, Lodz - Poland

^[99] Univ Medellin, Medellin - Colombia

^[100] Univ Amsterdam, Fac Sci, Amsterdam - Netherlands

^[101] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire - England

^[102] Ctr Invest & Estudios Avanzados IPN CINVESTAV, Mexico City, DF - Mexico

• Tipo de documento: Artigo Científico
• Fonte: ASTROPHYSICAL JOURNAL; v. 891, n. 2 MAR 10 2020.
• Citações Web of Science: 1

Resumo

We present measurements of the large-scale cosmic-ray (CR) anisotropies in R.A., using data collected by the surface detector array of the Pierre Auger Observatory over more than 14 yr. We determine the equatorial dipole component, d(perpendicular to), through a Fourier analysis in R.A. that includes weights for each event so as to account for the main detector-induced systematic effects. For the energies at which the trigger efficiency of the array is small, the ``east-west{''} method is employed. Besides using the data from the array with detectors separated by 1500.m, we also include data from the smaller but denser subarray of detectors with 750 m separation, which allows us to extend the analysis down to similar to 0.03.EeV. The most significant equatorial dipole amplitude obtained is that in the cumulative bin above 8.EeV, = d(perpendicular to) = 6.0(-0.9)(+1.0)%, which is inconsistent with isotropy at the 6 sigma level. In the bins below 8.EeV, we obtain 99% CL upper bounds on d(perpendicular to) at the level of 1%-3%. At energies below 1.EeV, even though the amplitudes are not significant, the phases determined in most of the bins are not far from the R.A. of the Galactic center, at (GC)=-94 degrees, suggesting a predominantly Galactic origin for anisotropies at these energies. The reconstructed dipole phases in the energy bins above 4.EeV point instead to R.A. that are almost opposite to the Galactic center one, indicative of an extragalactic CR origin.alpha (AU)

• Processo FAPESP: 99/05404-3 - Observatório Pierre Auger
• Beneficiário: Carlos Ourivio Escobar
• Modalidade de apoio: Auxílio à Pesquisa - Temático
• Processo FAPESP: 10/07359-6 - Estudo dos raios cósmicos de mais altas energias com o Observatório Pierre Auger
• Beneficiário: Carola Dobrigkeit Chinellato
• Modalidade de apoio: Auxílio à Pesquisa - Temático