Improved Limit To The Diffuse Flux Of Ultrahigh Energy Neutrinos From The Pierre Auger Observatory

A Aab,P Abreu,M Aglietta,E J Ahn,I Al Samarai,Ivone F M Albuquerque,I Allekotte,P Allison,A Almela,J Alvarez Castillo,J Alvarezmuniz,R Alves Batista,M Ambrosio,A Aminaei,Luis A Anchordoqui,S Andringa,C Aramo, V M Aranda,F Arqueros,N Arsene,H Asorey,P Assis,J Aublin,M Ave,M Avenier,G Avila, Nafiun Awal,A M Badescu, K B Barber,J Baeuml, Colin Baus,J J Beatty,K H Becker,J A Bellido,C Berat, M Bertaina,X Bertou,Peter L Biermann,P Billoir, Simon G Blaess,A Blanco,M Blanco,C Bleve, H Bluemer, M Bohacova,D Boncioli,C Bonifazi, N Borodi,J Brack,I M Brancus,A Bridgeman,P Brogueira,W C Brown, P Buchholz,A Bueno,S Buitink,M Buscemi,K S Caballeromora, B Caccianiga,L Caccianiga, M Candusso,L Caramete,R Caruso,A Castellina,G Cataldi,L Cazon,R Cester,A G Chavez, A Chiavassa,Jose Chinellato,J Chudoba, M Cilmo,R W Clay,G Cocciolo,Roberta Colalillo,A Coleman,Laura Collica, M R Coluccia,R Conceicao,F Contreras,M J Cooper,A Cordier,S Coutu,C E Covault, John Edward Cronin,R Dallier,Bruno Daniel,S Dasso,K Daumiller,Bruce R Dawson,R M De Almeida,S J De Jong,G De Mauro,J R T De Mello Neto,I De Mitri,J De Oliveira,V De Souza,L Del Peral,O Deligny,H Dembinski,N Dhital,C Di Giulio,A Di Matteo,J C Diaz,M L Diaz Castro, F Diogo,C Dobrigkeit, W Docters, J C Dolivo,A Dorofeev, Q Dorosti Hasankiadeh,M T Dova,J Ebr, R Enge,M Erdmann, M Erfani,C Escobar,J Espadanal,A Etchegoyen,H Falcke,Ke Fang,Glennys R Farrar,A C Fauth,N Fazzini,A P Ferguson,M V Fernandes,B E Fick,J M Figueira,A Filevich,A Filipcic,B D Fox,Octavian Fratu, Martin Miguel Freire,Beate Fuchs, Toshitaka Fujii,Bruce Rafael Mellado Garcia,D Garciapinto, F Gate,H Gemmeke,A Gherghellascu,P L Ghia,U Giaccari,M Giammarchi,M Giller, D Glas,C Glaser, H L Glass,G Golup,M Gomez Berisso,P F Gomez Vitale, Narciso Barrero Gonzalez,B Gookin,John C Gordon,A Gorgi,Peter W Gorham,P Gouffon,N Griffith,A F Grillo,Trent D Grubb,Y Guardincerri,F Guarino,G P Guedes, M R Hampe, P H Hansen,D Harari,T A Harrison, Stephan Hartmann,J L Harton, A Haungs, T Hebbeker,D Heck, P Heimann,A Herve,G C Hi,C Hojvat,N Hollon,Ewa Holt,P Homola,J R Horande,Pavel Horvath,Miroslav Hrabovsky,Daniel Huber,T Huege,A Insolia, P G Isar, I Jandt,S Jansen,C Jarne, Jeffrey A Johnsen,M Josebachuili, A Kaeaepae, Olga Kambeitz, K H Kampert, P A Kasper,I Katkov,B Kegl,B Keilhauer,A Keivani,E Kemp, R M Kieckhafer,H O Klages,M Kleifges,J Kleinfeller,R Krause,N Krohm,O Kroemer,D Kuempel,N Kunka,Danielle Lahurd,L Latronico,R Lauer,Markus Lauscher,P Lautridou,S Le Coz,D Lebrun, P Lebrun,M A Leigui De Oliveira,A Letessierselvon,I Lhenryyvon,K Link, Leticia Dos S Lopes, Ricardo Alarcon Lopez,A Lopez Casado,K Louedec,Lixin Lu, Alfredo Marquez Lucero,M Malacari,S Maldera,M Mallamaci, Jennifer Maller,D Mandat,R Mantsch,A G Mariazzi, V Mann,I C Maris,G Marsella,D Martello,Lisa J Martin,H Martinez,O Martinez Bravo,Diane Martraire,J J Masias Meza,H J Mathes, S Mathys,J A J Matthews,G Matthiae, D Maurel,D Maurizio,Eric Mayotte,P O Mazur, Claudia S Medina,G Medinatanco,R Meissner, Victor Mello, Daniele Santana De Melo,A Menshikov,S Messina,R Meyhandan,M I Micheletti, Lukas Middendorf,I A Minaya,L Miramonti,B Mitrica,L Molinabueno,Silvia Mollerach,F Montanet,C Morello,M Mostafa,C A Moura,M Muller, Gerhard J Mueller,Steffen Mueller,R Mussa,G Navarra,J L Navarro,S Navas, R Necesal,L Nellen,A Nelles, J Neuser,Phong H Nguyen, M Niculescuoglinzanu,M Niechciol, L Niemietz,Tim Niggemann,Dave F Nitz,D Nosek,Vojtech Novotny,L Nozka,L Ochilo,Foteini Oikonomou,Angela V Olinto,Nazaret Pacheco,D Pakk Selmidei,M Palatka,J Pallotta, P Papenbreer,G Parente,A Parra,T Paul,M Pech,J Pekala,R Pelayo,I M Pepe,L Perrone,E Petermann, Carsten Peters,S Petrera,Y Petrov, J Phuntsok, R Piegaia,T Pierog,P Pieroni,M Pimenta,V Pirronello,M Platino, M Plum, A Porcelli, C Porowski,Raul Ribeiro Prado,P Privitera,M Prouza,V Purrello,E J Quel,S Querchfeld,Samuel N Quinn,J Rautenberg,O Ravel,D Ravignani,B Revenu,J Ridky,S Riggi,M Risse,P Ristori,V Rizi,W Rodrigues De Carvalho,G Rodriguez Fernandez,J Rodriguez Rojo, D Rodriguezfrias, Dmytro Rogozin,Jander Fagundes Rosado,M Roth,Esteban Roulet,A C Rovero, Steven J Saffi,A Saftoiu,F Salamida,H Salazar, Anthony D Saleh,F Salesa Greus,G Salina, Francisca Javiela Munoz Sanchez,P Sanchezlucas, E M Santos,F Sarazin,Bishnu Charan Sarkar,Renato Almeida Sarmento,R Sato,C Scarso, Maggie Schauer,V Scherini,H Schieler,P Schiffer,David M Schmidt,O Scholten,H Schoorlemmer,P Schovanek,Friedhelm Schroeder, Andreas Schulz,J T Schulz, J W Schumacher,S J Sciutto,A Segreto,M Settimo,A Shadkam,R C Shellard,I Sidelnik,Gunter Sigl,O Sima,A Smialkowski,R Smida, G R Snow,Paul Sommers, J Sorokin, R Sotuartini, Y N Srivastava, D Stanca,S Stanic,Jack T Stapleton,J Stasielak,M Stephan,Anne Stutz,F Suarez, T Suomijaervi,A D Supanitsky,M S Sutherland,J E Swain,Z Szadkowski, O A Taborda,A Tapia,A Tepe, V M Theodoro,J Tiffenberg,C Timmermans,C J Todero Peixoto,G Toma, Lenka Tomankova,B Tome,A Tonachini,G Torralba Elipe,D Torres Machado,Petr Travnicek,R Ulrich,Michael Unger,Marcel Urban,J F Valdes Galicia,I Valino,L Valore,G Van Aar,P Van Bodegom,A M Van Den Berg,S Van Velzen,A Van Vliet,E Varela,B Vargas Cardenas,G Varner, R Vasquez, R A Vazquez,D Veberic,V Verzi,J Vicha,M Videla,L Villasenor, Brian Vlcek,S Vorobiov,Hernan Wahlberg,O Wainberg,D Walz,Alan Watson, M Weber, K Weidenhaupt,A Weindl,Frederick W Werner,A Widom,L Wiencke,H Wilczynski,T Winchen, D Wittkowski,B Wundheiler,S Wykes,L Yang,T Yapici,A N Yushkov,E Zas, D Zawtanik,M Zavrtanik,A Zepeda,Yingchun Zhu, Bernhard G Zimmermann,M Ziolkowski,Francesca Zuccarello

PHYSICAL REVIEW D（2015）

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摘要

Neutrinos in the cosmic ray flux with energies near 1 EeV and above are detectable with the Surface Detector array (SD) of the Pierre Auger Observatory. We report here on searches through Auger data from 1 January 2004 until 20 June 2013. No neutrino candidates were found, yielding a limit to the diffuse flux of ultrahigh energy neutrinos that challenges the Waxman-Bahcall bound predictions. Neutrino identification is attempted using the broad time structure of the signals expected in the SD stations, and is efficiently done for neutrinos of all flavors interacting in the atmosphere at large zenith angles, as well as for "Earth-skimming" neutrino interactions in the case of tau neutrinos. In this paper the searches for downward-going neutrinos in the zenith angle bins 60 degrees-75 degrees and 75 degrees-90 degrees as well as for upward-going neutrinos, are combined to give a single limit. The 90% C.L. single-flavor limit to the diffuse flux of ultrahigh energy neutrinos with an E-2 spectrum in the energy range 1.0 x 10(17) eV-2.5 x 10(19) eV is E(nu)(2)dN(nu)/dE(nu) < 6.4 x 10(-9) GeV cm(-2) s(-1) sr(-1).

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