Observation of the suppression of the flux of cosmic rays above 4x10(19) eV

Abraham, J; Abreu, P; Aglietta, M; Aguirre, C; Allard, D; Allekotte, I; Allen, J; Allison, P; Alvarez Muniz, J; Ambrosio, M; Anchordoqui, L; Andringa, S; Anzalone, A; Aramo, C; Argiro, S; Arisaka, K; Armengaud, E; Arneodo, F; Arqueros, F; Asch, T; Asorey, H; Assis, P; Atulugama, Bs; Aublin, J; Ave, M; Avila, G; Backer, T; Badagnani, D; Barbosa, Af; Barnhill, D; Barroso, Slc; Baughman, B; Bauleo, P; Beatty, Jj; Beau, T; Becker, Br; Becker, Kh; Bellido, Ja; Benzvi, S; Berat, C; Bergmann, T; Bernardini, P; Bertou, X; Biermann, Pl; Billoir, P; Blanch Bigas, O; Blanco, F; Blasi, P; Bleve, C; Mer, Hb; Bohacova, M; Bonifazi, C; Bonino, R; Brack, J; Brogueira, P; Brown, Wc; Buchholz, P; Bueno, A; Burton, Re; Busca, Ng; Caballero Mora KS,; Cai, B; Camin, Dv; Caramete, L; Caruso, R; Carvalho, W; Castellina, A; Catalano, O; Cataldi, G; Cazon, L; Cester, R; Chauvin, J; Chiavassa, A; Chinellato, Ja; Chou, A; Chudoba, J; Chye, J; Clark, Pdj; Clay, Rw; Colombo, E; Conceicao, R; Connolly, B; Contreras, F; Coppens, J; Cordier, A; Cotti, U; Coutu, S; Covault, Ce; Creusot, A; Criss, A; Cronin, J; Curutiu, A; Dagoret Campagne, S; Daumiller, K; Dawson, Br; de Almeida RM,; de Donato, C; de Jong SJ,; De La Vega, G; Junior, Wjmd; Neto, Jrtd; De Mitri, I; de Souza, V; del Peral, L; Deligny, O; Della Selva, A; Delle Fratte, C; Dembinski, H; Di Giulio, C; Diaz, Jc; Diep, Pn; Dobrigkeit, C; D'Olivo, Jc; Dong, Pn; Dornic, D; Dorofeev, A; dos Anjos JC,; Dova, Mt; D'Urso, D; Dutan, I; Duvernois, Ma; Engel, R; Epele, L; Erdmann, M; Escobar, Co; Etchegoyen, A; Luis, Pfs; Falcke, H; Farrar, G; Fauth, Ac; Fazzini, N; Ferrer, F; Ferrero, A; Fick, B; Filevich, A; Filipcic, A; Fleck, I; Fracchiolla, Ce; Fulgione, W; Garcia, B; Gamez, Dg; Garcia Pinto, D; Garrido, X; Geenen, H; Gelmini, G; Gemmeke, H; Ghia, Pl; Giller, M; Glass, H; Gold, Ms; Golup, G; Albarracin, Fg; Berisso, Mg; Goncalves, P; do Amaral MG,; Gonzalez, D; Gonzalez, Jg; Gonzalez, M; Gora, D; Gorgi, A; Gouffon, P; Grassi, V; Grillo, Af; Grunfeld, C; Guardincerri, Y; Guarino, F; Guedes, Gp; Gutierrez, J; Hague, Jd; Halenka, V; Hamilton, Jc; Hansen, P; Harari, D; Harmsma, S; Harton, Jl; Haungs, A; Hauschildt, T; Healy, Md; Hebbeker, T; Hebrero, G; Heck, D; Hojvat, C; Holmes, Vc; Homola, P; Horandel, Jr; Horneffer, A; Hrabovsky, M; Huege, T; Hussain, M; Iarlori, M; Insolia, A; Ionita, F; Italiano, A; Kaducak, M; Kampert, Kh; Karova, T; Kasper, P; Kegl, B; Keilhauer, B; Kemp, E; Kieckhafer, Rm; Klages, Ho; Kleifges, M; Kleinfeller, J; Knapik, R; Knapp, J; Koang, Dh; Krieger, A; Kromer, O; Kuempel, D; Kunka, N; Kusenko, A; La Rosa, G; Lachaud, C; Lago, Bl; Lebrun, D; Lebrun, P; Lee, J; de Oliveira MAL,; Letessier Selvon, A; Leuthold, M; Lhenry Yvon, I; Lopez, R; Aguera, Al; Bahilo, Jl; Lucero, A; Garcia, Rl; Maccarone, Mc; Macolino, C; Maldera, S; Mancarella, G; Mancenido, Me; Mandat, D; Mantsch, P; Mariazzi, Ag; Maris, Ic; Falcon, Hrm; Martello, D; Martinez, J; Bravo, Om; Mathes, Hj; Matthews, J; Matthews, Jaj; Matthiae, G; Maurizio, D; Mazur, Po; Mccauley, T; Mcewen, M; Mcneil, Rr; Medina, Mc; Medina Tanco, G; Melo, D; Menichetti, E; Menschikov, A; Meurer, C; Meyhandan, R; Micheletti, Mi; Miele, G; Miller, W; Mollerach, S; Monasor, M; Ragaigne, Dm; Montanet, F; Morales, B; Morello, C; Moreno, Jc; Morris, C; Mostafa, M; Muller, Ma; Mussa, R; Navarra, G; Navarro, Jl; Navas, S; Necesal, P; Nellen, L; Newman Holmes, C; Newton, D; Nhung, Pt; Nierstenhoefer, N; Nitz, D; Nosek, D; Nozka, L; Oehlschlager, J; Ohnuki, T; Olinto, A; Olmos Gilbaja VM,; Ortiz, M; Ortolani, F; Ostapchenko, S; Otero, L; Pacheco, N; Selmi Dei DP,; Palatka, M; Pallotta, J; Parente, G; Parizot, E; Parlati, S; Pastor, S; Patel, M; Paul, T; Pavlidou, V; Payet, K; Pech, M; Pekala, J; Pelayo, R; Pepe, Im; Perrone, L; Pesce, R; Petrera, Sergio; Petrinca, P; Petrov, Y; Pichel, A; Piegaia, R; Pierog, T; Pimenta, M; Pinto, T; Pirronello, V; Pisanti, O; Platino, M; Pochon, J; Privitera, P; Prouza, M; Quel, Ej; Rautenberg, J; Redondo, A; Reucroft, S; Revenu, B; Rezende, Fas; Ridky, J; Riggi, S; Risse, M; Riviere, C; Rizi, Vincenzo; Roberts, M; Robledo, C; Rodriguez, G; Martino, Jr; Rojo, Jr; Rodriguez Cabo, I; Rodriguez Frias MD,; Ros, G; Rosado, J; Roth, M; Rouille d'Orfeuil, B; Roulet, E; Rovero, Ac; Salamida, Francesco; Salazar, H; Salina, G; Sanchez, F; Santander, M; Santo, Ce; Santos, Em; Sarazin, F; Sarkar, S; Sato, R; Scherini, V; Schieler, H; Schmidt, A; Schmidt, F; Schmidt, T; Scholten, O; Schovanek, P; Schroeder, F; Schulte, S; Schussler, F; Sciutto, Sj; Scuderi, M; Segreto, A; Semikoz, D; Settimo, M; Shellard, Rc; Sidelnik, I; Siffert, Bb; Sigl, G; De Grande NS,; Smialkowski, A; Smida, R; Smith, Agk; Smith, Be; Snow, Gr; Sokolsky, P; Sommers, P; Sorokin, J; Spinka, H; Squartini, R; Strazzeri, E; Stutz, A; Suarez, F; Suomijarvi, T; Supanitsky, Ad; Sutherland, Ms; Swain, J; Szadkowski, Z; Takahashi, J; Tamashiro, A; Tamburro, A; Tarutina, T; Tascau, O; Tcaciuc, R; Thao, Nt; Thomas, D; Ticona, R; Tiffenberg, J; Timmermans, C; Tkaczyk, W; Peixoto, Cjt; Tome, B; Tonachini, A; Torres, I; Travnicek, P; Tripathi, A; Tristram, G; Tscherniakhovski, D; Tuci, V; Tueros, M; Tunnicliffe, V; Ulrich, R; Unger, M; Urban, M; Galicia, Jfv; Valino, I; Valore, L; van den Berg AM,; van Elewyck, V; Vazquez, Ra; Veberic, D; Veiga, A; Velarde, A; Venters, T; Verzi, V; Videla, M; Villasenor, L; Vorobiov, S; Voyvodic, L; Wahlberg, H; Wahrlich, P; Wainberg, O; Walker, P; Warner, D; Watson, Aa; Westerhoff, S; Wieczorek, G; Wiencke, L; Wilczynska, B; Wilczynski, H; Wileman, C; Winnick, Mg; Wu, H; Wundheiler, B; Yamamoto, T; Younk, P; Zas, E; Zavrtanik, D; Zavrtanik, M; Zaw, I; Zepeda, A; Ziolkowski, M.

doi:10.1103/PhysRevLett.101.061101

CINECA IRIS Institutional Research Information System

IRIS è la soluzione IT che facilita la raccolta e la gestione dei dati relativi alle attività e ai prodotti della ricerca. Fornisce a ricercatori, amministratori e valutatori gli strumenti per monitorare i risultati della ricerca, aumentarne la visibilità e allocare in modo efficace le risorse disponibili.

The energy spectrum of cosmic rays above 2.5 x 10(18) eV, derived from 20 000 events recorded at the Pierre Auger Observatory, is described. The spectral index gamma of the particle flux, J proportional to E(-gamma), at energies between 4 x 10(18) eV and 4 x 10(19) eV is 2.69 +/- 0.02(stat) +/- 0.06(syst), steepening to 4.2 +/- 0.4(stat) +/- 0: 06 (syst) at higher energies. The hypothesis of a single power law is rejected with a significance greater than 6 standard deviations. The data are consistent with the prediction by Greisen and by Zatsepin and Kuz'min.

Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11697/11386

Titolo:	Observation of the suppression of the flux of cosmic rays above 4x10(19) eV
Autori:	Abraham J Abreu P Aglietta M Aguirre C Allard D Allekotte I Allen J Allison P Alvarez Muniz J Ambrosio M Anchordoqui L Andringa S Anzalone A Aramo C Argiro S Arisaka K Armengaud E Arneodo F Arqueros F Asch T Asorey H Assis P Atulugama BS Aublin J Ave M Avila G Backer T Badagnani D Barbosa AF Barnhill D Barroso SLC Baughman B Bauleo P Beatty JJ Beau T Becker BR Becker KH Bellido JA BenZvi S Berat C Bergmann T Bernardini P Bertou X Biermann PL Billoir P Blanch Bigas O Blanco F Blasi P Bleve C Mer HB Bohacova M Bonifazi C Bonino R Brack J Brogueira P Brown WC Buchholz P Bueno A Burton RE Busca NG Caballero Mora KS Cai B Camin DV Caramete L Caruso R Carvalho W Castellina A Catalano O Cataldi G Cazon L Cester R Chauvin J Chiavassa A Chinellato JA Chou A Chudoba J Chye J Clark PDJ Clay RW Colombo E Conceicao R Connolly B Contreras F Coppens J Cordier A Cotti U Coutu S Covault CE Creusot A Criss A Cronin J Curutiu A Dagoret Campagne S Daumiller K Dawson BR de Almeida RM de Donato C de Jong SJ De La Vega G Junior WJMD Neto JRTD De Mitri I de Souza V del Peral L Deligny O Della Selva A Delle Fratte C Dembinski H Di Giulio C Diaz JC Diep PN Dobrigkeit C D'Olivo JC Dong PN Dornic D Dorofeev A dos Anjos JC Dova MT D'Urso D Dutan I DuVernois MA Engel R Epele L Erdmann M Escobar CO Etchegoyen A Luis PFS Falcke H Farrar G Fauth AC Fazzini N Ferrer F Ferrero A Fick B Filevich A Filipcic A Fleck I Fracchiolla CE Fulgione W Garcia B Gamez DG Garcia Pinto D Garrido X Geenen H Gelmini G Gemmeke H Ghia PL Giller M Glass H Gold MS Golup G Albarracin FG Berisso MG Goncalves P do Amaral MG Gonzalez D Gonzalez JG Gonzalez M Gora D Gorgi A Gouffon P Grassi V Grillo AF Grunfeld C Guardincerri Y Guarino F Guedes GP Gutierrez J Hague JD Halenka V Hamilton JC Hansen P Harari D Harmsma S Harton JL Haungs A Hauschildt T Healy MD Hebbeker T Hebrero G Heck D Hojvat C Holmes VC Homola P Horandel JR Horneffer A Hrabovsky M Huege T Hussain M Iarlori M Insolia A Ionita F Italiano A Kaducak M Kampert KH Karova T Kasper P Kegl B Keilhauer B Kemp E Kieckhafer RM Klages HO Kleifges M Kleinfeller J Knapik R Knapp J Koang DH Krieger A Kromer O Kuempel D Kunka N Kusenko A La Rosa G Lachaud C Lago BL Lebrun D Lebrun P Lee J de Oliveira MAL Letessier Selvon A Leuthold M Lhenry Yvon I Lopez R Aguera AL Bahilo JL Lucero A Garcia RL Maccarone MC Macolino C Maldera S Mancarella G Mancenido ME Mandat D Mantsch P Mariazzi AG Maris IC Falcon HRM Martello D Martinez J Bravo OM Mathes HJ Matthews J Matthews JAJ Matthiae G Maurizio D Mazur PO McCauley T McEwen M McNeil RR Medina MC Medina Tanco G Melo D Menichetti E Menschikov A Meurer C Meyhandan R Micheletti MI Miele G Miller W Mollerach S Monasor M Ragaigne DM Montanet F Morales B Morello C Moreno JC Morris C Mostafa M Muller MA Mussa R Navarra G Navarro JL Navas S Necesal P Nellen L Newman Holmes C Newton D Nhung PT Nierstenhoefer N Nitz D Nosek D Nozka L Oehlschlager J Ohnuki T Olinto A Olmos Gilbaja VM Ortiz M Ortolani F Ostapchenko S Otero L Pacheco N Selmi Dei DP Palatka M Pallotta J Parente G Parizot E Parlati S Pastor S Patel M Paul T Pavlidou V Payet K Pech M Pekala J Pelayo R Pepe IM Perrone L Pesce R PETRERA, SERGIO Petrinca P Petrov Y Pichel A Piegaia R Pierog T Pimenta M Pinto T Pirronello V Pisanti O Platino M Pochon J Privitera P Prouza M Quel EJ Rautenberg J Redondo A Reucroft S Revenu B Rezende FAS Ridky J Riggi S Risse M Riviere C RIZI, VINCENZO Roberts M Robledo C Rodriguez G Martino JR Rojo JR Rodriguez Cabo I Rodriguez Frias MD Ros G Rosado J Roth M Rouille d'Orfeuil B Roulet E Rovero AC SALAMIDA, Francesco Salazar H Salina G Sanchez F Santander M Santo CE Santos EM Sarazin F Sarkar S Sato R Scherini V Schieler H Schmidt A Schmidt F Schmidt T Scholten O Schovanek P Schroeder F Schulte S Schussler F Sciutto SJ Scuderi M Segreto A Semikoz D Settimo M Shellard RC Sidelnik I Siffert BB Sigl G De Grande NS Smialkowski A Smida R Smith AGK Smith BE Snow GR Sokolsky P Sommers P Sorokin J Spinka H Squartini R Strazzeri E Stutz A Suarez F Suomijarvi T Supanitsky AD Sutherland MS Swain J Szadkowski Z Takahashi J Tamashiro A Tamburro A Tarutina T Tascau O Tcaciuc R Thao NT Thomas D Ticona R Tiffenberg J Timmermans C Tkaczyk W Peixoto CJT Tome B Tonachini A Torres I Travnicek P Tripathi A Tristram G Tscherniakhovski D Tuci V Tueros M Tunnicliffe V Ulrich R Unger M Urban M Galicia JFV Valino I Valore L van den Berg AM van Elewyck V Vazquez RA Veberic D Veiga A Velarde A Venters T Verzi V Videla M Villasenor L Vorobiov S Voyvodic L Wahlberg H Wahrlich P Wainberg O Walker P Warner D Watson AA Westerhoff S Wieczorek G Wiencke L Wilczynska B Wilczynski H Wileman C Winnick MG Wu H Wundheiler B Yamamoto T Younk P Zas E Zavrtanik D Zavrtanik M Zaw I Zepeda A Ziolkowski M. mostra contributor esterni nascondi contributor esterni
Data di pubblicazione:	2008
Rivista:	PHYSICAL REVIEW LETTERS
Abstract:	The energy spectrum of cosmic rays above 2.5 x 10(18) eV, derived from 20 000 events recorded at the Pierre Auger Observatory, is described. The spectral index gamma of the particle flux, J proportional to E(-gamma), at energies between 4 x 10(18) eV and 4 x 10(19) eV is 2.69 +/- 0.02(stat) +/- 0.06(syst), steepening to 4.2 +/- 0.4(stat) +/- 0: 06 (syst) at higher energies. The hypothesis of a single power law is rejected with a significance greater than 6 standard deviations. The data are consistent with the prediction by Greisen and by Zatsepin and Kuz'min.
Handle:	http://hdl.handle.net/11697/11386
Appare nelle tipologie:	1.1 Articolo in rivista

File in questo prodotto:

Non ci sono file associati a questo prodotto.

Citazioni

I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.