The Advanced LIGO and Advanced Virgo observatories recently discovered gravitational waves from a binary neutron star inspiral. A short gammaray burst GRB that followed the merger of this binary was also recorded by the Fermi Gammaray Burst Monitor FermiGBM and the AntiCoincidence Shield for the Spectrometer for the International GammaRay Astrophysics Laboratory INTEGRAL indicating particle acceleration by the source. The precise location of the event was determined by optical detections of emission following the merger. We searched for highenergy neutrinos from the merger in the GeVEeV energy range using the ANTARES IceCube and Pierre Auger Observatories. No neutrinos directionally coincident with the source were detected within 500 s around the merger time. Additionally no MeV neutrino burst signal was detected coincident with the merger. We further carried out an extended search in the direction of the source for highenergy neutrinos within the 14 day period following the merger but found no evidence of emission. We used these results to probe dissipation mechanisms in relativistic outflows driven by the binary neutron star merger. The nondetection is consistent with model predictions of short GRBs observed at a large offaxis angle.
['gamma-ray burst: general', 'gravitational waves', 'neutrinos', 'Astrophysics - High Energy Astrophysical Phenomena']
Search for Highenergy Neutrinos from Binary Neutron Star Merger GW170817 with ANTARES IceCube and the Pierre Auger Observatory
{'SEARCH FOR HIGH-ENERGY NEUTRINOS FROM BINARY NEUTRON STAR MERGER GW170817 WITH ANTARES, ICECUBE, AND THE PIERRE AUGER OBSERVATORY': "A. ALBERT, 1 M. ANDR'E, 2 M. ANGHINOLFI, 3 M. ARDID, 4 J.-J. AUBERT, 5 J. AUBLIN, 6 T. AVGITAS, 6 B. BARET, 6 J. BARRIOS-MART'I, 7 S. BASA, 8 B. BELHORMA, 9 V. BERTIN, 5 S. BIAGI, 10 R. BORMUTH, 11, 12 S. BOURRET, 6 M.C. BOUWHUIS, 11 H. BR ˆANZAS¸, 13 R. BRUIJN, 11, 14 J. BRUNNER, 5 J. BUSTO, 5 A. CAPONE, 15, 16 L. CARAMETE, 13 J. CARR, 5 S. CELLI, 15, 16, 17 R. CHERKAOUI EL MOURSLI, 18 T. CHIARUSI, 19 M. CIRCELLA, 20 J.A.B. COELHO, 6 A. COLEIRO, 6, 7 R. CONIGLIONE, 10 H. COSTANTINI, 5 P. COYLE, 5 A. CREUSOT, 6 A. F. D'IAZ, 21 A. DESCHAMPS, 22 G. DE BONIS, 15 C. DISTEFANO, 10 I. DI PALMA, 15, 16 A. DOMI, 3, 23 C. DONZAUD, 6, 24 D. DORNIC, 5 D. DROUHIN, 1 T. EBERL, 25 I. EL BOJADDAINI, 26 N. EL KHAYATI, 18 D. ELS ASSER, 27 A. ENZENHOFER, 5 A. ETTAHIRI, 18 F. FASSI, 18 I. FELIS, 4 L.A. FUSCO, 19, 28 P. GAY, 29, 6 V. GIORDANO, 30 H. GLOTIN, 31, 32 T. GR'EGOIRE, 6 R. GRACIA RUIZ, 6, 33 K. GRAF, 25 S. HALLMANN, 25 H. VAN HAREN, 34 A.J. HEIJBOER, 11 Y. HELLO, 22 J.J. HERN'ANDEZ-REY, 7 J. H OSSL, 25 J. HOFEST ADT, 25 G. ILLUMINATI, 7 C.W. JAMES, 25 M. DE JONG, 11, 12 M. JONGEN, 11 M. KADLER, 27 O. KALEKIN, 25 U. KATZ, 25 D. KIESSLING, 25 A. KOUCHNER, 6, 32 M. KRETER, 27 I. KREYKENBOHM, 35 V. KULIKOVSKIY, 5, 36 C. LACHAUD, 6 R. LAHMANN, 25 D. LEF'EVRE, 37 E. LEONORA, 30, 38 M. LOTZE, 7 S. LOUCATOS, 39, 6 M. MARCELIN, 8 A. MARGIOTTA, 19, 28 A. MARINELLI, 40, 41 J.A. MART'INEZ-MORA, 4 R. MELE, 42, 43 K. MELIS, 11, 14 T. MICHAEL, 11 P. MIGLIOZZI, 42 A. MOUSSA, 26 S. NAVAS, 44 E. NEZRI, 8 M. ORGANOKOV, 33 G.E. P ˘AV ˘ALAS¸, 13 C. PELLEGRINO, 19, 28 C. PERRINA, 15, 16 P. PIATTELLI, 10 V. POPA, 13 T. PRADIER, 33 L. QUINN, 5 C. RACCA, 1 G. RICCOBENE, 10 A. S 'ANCHEZ-LOSA, 20 M. SALDA˜NA, 4 I. SALVADORI, 5 D. F. E. SAMTLEBEN, 11, 12 M. SANGUINETI, 3, 23 P. SAPIENZA, 10 F. SCH USSLER, 39 C. SIEGER, 25 M. SPURIO, 19, 28 TH. STOLARCZYK, 39 M. TAIUTI, 3, 23 Y. TAYALATI, 18 A. TROVATO, 10 D. TURPIN, 5 C. T ONNIS, 7 B. VALLAGE, 39, 6 V. VAN ELEWYCK, 6, 32 F. VERSARI, 19, 28 D. VIVOLO, 42, 43 A. VIZZOCA, 15, 16 J. WILMS, 45 J.D. ZORNOZA, 7 AND J. Z 'U ˜NIGA 7", '(ANTARES COLLABORATION)': "M. G. AARTSEN, 46 M. ACKERMANN, 47 J. ADAMS, 48 J. A. AGUILAR, 49 M. AHLERS, 50 M. AHRENS, 51 I. AL SAMARAI, 52 D. ALTMANN, 53 K. ANDEEN, 54 T. ANDERSON, 55 I. ANSSEAU, 49 G. ANTON, 53 C. ARGUELLES, 56 J. AUFFENBERG, 57 S. AXANI, 56 H. BAGHERPOUR, 48 X. BAI, 58 J. P. BARRON, 59 S. W. BARWICK, 60 V. BAUM, 61 R. BAY, 62 J. J. BEATTY, 63, 64 J. BECKER TJUS, 65 K.-H. BECKER, 66 S. BENZVI, 67 D. BERLEY, 68 E. BERNARDINI, 47 D. Z. BESSON, 69 G. BINDER, 70, 62 D. BINDIG, 66 E. BLAUFUSS, 68 S. BLOT, 47 C. BOHM, 51 M. BORNER, 71 F. BOS, 65 D. BOSE, 72 S. B OSER, 61 O. BOTNER, 73 E. BOURBEAU, 50 J. BOURBEAU, 74 F. BRADASCIO, 47 J. BRAUN, 74 L. BRAYEUR, 75 M. BRENZKE, 57 H.-P. BRETZ, 47 S. BRON, 52 J. BROSTEAN-KAISER, 47 A. BURGMAN, 73 T. CARVER, 52 J. CASEY, 74 M. CASIER, 75 E. CHEUNG, 68 D. CHIRKIN, 74 A. CHRISTOV, 52 K. CLARK, 76 L. CLASSEN, 77 S. COENDERS, 78 G. H. COLLIN, 56 J. M. CONRAD, 56 D. F. COWEN, 55, 79 R. CROSS, 67 M. DAY, 74 J. P. A. M. DE ANDR'E, 80 C. DE CLERCQ, 75 J. J. DELAUNAY, 55 H. DEMBINSKI, 81 S. DE RIDDER, 82 P. DESIATI, 74 K. D. DE VRIES, 75 G. DE WASSEIGE, 75 M. DE WITH, 83 T. DEYOUNG, 80 J. C. D'IAZ-V'ELEZ, 74 V. DI LORENZO, 61 H. DUJMOVIC, 72 J. P. DUMM, 51 M. DUNKMAN, 55 E. DVORAK, 58 B. EBERHARDT, 61 T. EHRHARDT, 61 B. EICHMANN, 65 P. ELLER, 55 P. A. EVENSON, 81 S. FAHEY, 74 A. R. FAZELY, 84 J. FELDE, 68 K. FILIMONOV, 62 C. FINLEY, 51 S. FLIS, 51 A. FRANCKOWIAK, 47 E. FRIEDMAN, 68 T. FUCHS, 71 T. K. GAISSER, 81 J. GALLAGHER, 85 L. GERHARDT, 70 K. GHORBANI, 74 W. GIANG, 59 T. GLAUCH, 57 T. GL USENKAMP, 53 A. GOLDSCHMIDT, 70 J. G. GONZALEZ, 81 D. GRANT, 59 Z. GRIFFITH, 74 C. HAACK, 57 A. HALLGREN, 73 F. HALZEN, 74 K. HANSON, 74 D. HEBECKER, 83 D. HEEREMAN, 49 K. HELBING, 66 R. HELLAUER, 68 S. HICKFORD, 66 J. HIGNIGHT, 80 G. C. HILL, 46 K. D. HOFFMAN, 68 R. HOFFMANN, 66 B. HOKANSON-FASIG, 74 K. HOSHINA, 74, 86 F. HUANG, 55 M. HUBER, 78 K. HULTQVIST, 51 M. HUNNEFELD, 71 S. IN, 72 A. ISHIHARA, 87 E. JACOBI, 47 G. S. JAPARIDZE, 88 M. JEONG, 72 K. JERO, 74 B. J. P. JONES, 89 P. KALACZYNSKI, 57 W. KANG, 72 A. KAPPES, 77 T. KARG, 47 A. KARLE, 74 U. KATZ, 53 M. KAUER, 74 A. KEIVANI, 55 J. L. KELLEY, 74 A. KHEIRANDISH, 74 J. KIM, 72 M. KIM, 87 T. KINTSCHER, 47 J. KIRYLUK, 90 T. KITTLER, 53 S. R. KLEIN, 70, 62 G. KOHNEN, 91 R. KOIRALA, 81 H. KOLANOSKI, 83 L. K OPKE, 61 C. KOPPER, 59 S. KOPPER, 92 J. P. KOSCHINSKY, 57 D. J. KOSKINEN, 50 M. KOWALSKI, 83, 47 K. KRINGS, 78 M. KROLL, 65 G. KRUCKL, 61 J. KUNNEN, 75 S. KUNWAR, 47 N. KURAHASHI, 93 T. KUWABARA, 87 A. KYRIACOU, 46 M. LABARE, 82 J. L. LANFRANCHI, 55 M. J. LARSON, 50 F. LAUBER, 66 M. LESIAK-BZDAK, 90 M. LEUERMANN, 57 Q. R. LIU, 74 L. LU, 87 J. L UNEMANN, 75 W. LUSZCZAK, 74 J. MADSEN, 94 G. MAGGI, 75 K. B. M. MAHN, 80 S. MANCINA, 74 R. MARUYAMA, 95 K. MASE, 87 R. MAUNU, 68 F. MCNALLY, 74 K. MEAGHER, 49 M. MEDICI, 50 M. MEIER, 71 T. MENNE, 71 G. MERINO, 74 T. MEURES, 49 S. MIARECKI, 70, 62 J. MICALLEF, 80 G. MOMENT'E, 61 T. MONTARULI, 52 R. W. MOORE, 59 M. MOULAI, 56 R. NAHNHAUER, 47 P. NAKARMI, 92 U. NAUMANN, 66 G. NEER, 80 H. NIEDERHAUSEN, 90 S. C. NOWICKI, 59 D. R. NYGREN, 70 A. OBERTACKE POLLMANN, 66 A. OLIVAS, 68 A. O'MURCHADHA, 49 T. PALCZEWSKI, 70, 62 H. PANDYA, 81 D. V. PANKOVA, 55 P. PEIFFER, 61 J. A. PEPPER, 92 C. P'EREZ DE LOS HEROS, 73 D. PIELOTH, 71 E. PINAT, 49 M. PLUM, 54 D. PRANAV, 96 P. B. PRICE, 62 G. T. PRZYBYLSKI, 70 C. RAAB, 49 L. R ADEL, 57 M. RAMEEZ, 50 K. RAWLINS, 97 I. C. REA, 78 R. REIMANN, 57 B. RELETHFORD, 93 M. RELICH, 87 E. RESCONI, 78 W. RHODE, 71 M. RICHMAN, 93 S. ROBERTSON, 46 M. RONGEN, 57 C. ROTT, 72 T. RUHE, 71 D. RYCKBOSCH, 82 D. RYSEWYK, 80 T. S ALZER, 57 S. E. SANCHEZ HERRERA, 59 A. SANDROCK, 71 J. SANDROOS, 61 M. SANTANDER, 92 S. SARKAR, 50, 98 S. SARKAR, 59 K. SATALECKA, 47 P. SCHLUNDER, 71 T. SCHMIDT, 68 A. SCHNEIDER, 74 S. SCHOENEN, 57 S. SCH ONEBERG, 65 L. SCHUMACHER, 57 D. SECKEL, 81 S. SEUNARINE, 94 J. SOEDINGREKSO, 71 D. SOLDIN, 66 M. SONG, 68 G. M. SPICZAK, 94 C. SPIERING, 47 J. STACHURSKA, 47 M. STAMATIKOS, 63  \nT. STANEV, 81 A. STASIK, 47 J. STETTNER, 57 A. STEUER, 61 T. STEZELBERGER, 70 R. G. STOKSTAD, 70 A. ST OSSL, 87 N. L. STROTJOHANN, 47 T. STUTTARD, 50 G. W. SULLIVAN, 68 M. SUTHERLAND, 63 I. TABOADA, 96 J. TATAR, 70, 62 F. TENHOLT, 65 S. TER-ANTONYAN, 84 A. TERLIUK, 47 G. TEˇSI 'C, 55 S. TILAV, 81 P. A. TOALE, 92 M. N. TOBIN, 74 S. TOSCANO, 75 D. TOSI, 74 M. TSELENGIDOU, 53 C. F. TUNG, 96 A. TURCATI, 78 C. F. TURLEY, 55 B. TY, 74 E. UNGER, 73 M. USNER, 47 J. VANDENBROUCKE, 74 W. VAN DRIESSCHE, 82 N. VAN EIJNDHOVEN, 75 S. VANHEULE, 82 J. VAN SANTEN, 47 M. VEHRING, 57 E. VOGEL, 57 M. VRAEGHE, 82 C. WALCK, 51 A. WALLACE, 46 M. WALLRAFF, 57 F. D. WANDLER, 59 N. WANDKOWSKY, 74 A. WAZA, 57 C. WEAVER, 59 M. J. WEISS, 55 C. WENDT, 74 J. WERTHEBACH, 71 S. WESTERHOFF, 74 B. J. WHELAN, 46 K. WIEBE, 61 C. H. WIEBUSCH, 57 L. WILLE, 74 D. R. WILLIAMS, 92 L. WILLS, 93 M. WOLF, 74 J. WOOD, 74 T. R. WOOD, 59 E. WOOLSEY, 59 K. WOSCHNAGG, 62 D. L. XU, 74 X. W. XU, 84 Y. XU, 90 J. P. YANEZ, 59 G. YODH, 60 S. YOSHIDA, 87 T. YUAN, 74 AND M. ZOLL 51", '(ICECUBE COLLABORATION)': "A. AAB, 99 P. ABREU, 100 M. AGLIETTA, 101, 102 I.F.M. ALBUQUERQUE, 103 J.M. ALBURY, 104 I. ALLEKOTTE, 105 A. ALMELA, 106, 107 J. ALVAREZ CASTILLO, 108 J. ALVAREZ-MU˜NIZ, 109 G.A. ANASTASI, 110, 111 L. ANCHORDOQUI, 112 B. ANDRADA, 106 S. ANDRINGA, 100 C. ARAMO, 113 N. ARSENE, 114 H. ASOREY, 105, 115 P. ASSIS, 100 G. AVILA, 116, 117 A.M. BADESCU, 118 A. BALACEANU, 119 F. BARBATO, 120 R.J. BARREIRA LUZ, 100 J.J. BEATTY, 121 K.H. BECKER, 122 J.A. BELLIDO, 104 C. BERAT, 123 M.E. BERTAINA, 124, 102 X. BERTOU, 105 P.L. BIERMANN, 125 J. BITEAU, 126 S.G. BLAESS, 104 A. BLANCO, 100 J. BLAZEK, 127 C. BLEVE, 128, 129 M. BOH'AˇCOV 'A, 127 C. BONIFAZI, 130 N. BORODAI, 131 A.M. BOTTI, 106, 132 J. BRACK, 133 I. BRANCUS, 119 T. BRETZ, 134 A. BRIDGEMAN, 135 F.L. BRIECHLE, 134 P. BUCHHOLZ, 136 A. BUENO, 137 S. BUITINK, 99 M. BUSCEMI, 138, 139 K.S. CABALLERO-MORA, 140 L. CACCIANIGA, 141 A. CANCIO, 107, 106 F. CANFORA, 99 R. CARUSO, 138, 139 A. CASTELLINA, 101, 102 F. CATALANI, 142 G. CATALDI, 129 L. CAZON, 100 A.G. CHAVEZ, 143 J.A. CHINELLATO, 144 J. CHUDOBA, 127 R.W. CLAY, 104 A.C. COBOS CERUTTI, 145 R. COLALILLO, 120, 113 A. COLEMAN, 146 L. COLLICA, 102 M.R. COLUCCIA, 128, 129 R. CONCEIC¸ ˜AO, 100 G. CONSOLATI, 147, 148 F. CONTRERAS, 116, 117 M.J. COOPER, 104 S. COUTU, 146 C.E. COVAULT, 149 J. CRONIN, 150, ∗ S. D'AMICO, 151, 129 B. DANIEL, 144 S. DASSO, 152, 153 K. DAUMILLER, 132 B.R. DAWSON, 104 J.A. DAY, 104 R.M. DE ALMEIDA, 154 S.J. DE JONG, 99, 155 G. DE MAURO, 99 J.R.T. DE MELLO NETO, 130, 156 I. DE MITRI, 128, 129 J. DE OLIVEIRA, 154 V. DE SOUZA, 157 J. DEBATIN, 135 O. DELIGNY, 126 M.L. D'IAZ CASTRO, 144 F. DIOGO, 100 C. DOBRIGKEIT, 144 J.C. D'OLIVO, 108 Q. DOROSTI, 136 R.C. DOS ANJOS, 158 M.T. DOVA, 159 A. DUNDOVIC, 160 J. EBR, 127 R. ENGEL, 132 M. ERDMANN, 134 M. ERFANI, 136 C.O. ESCOBAR, 161 J. ESPADANAL, 100 A. ETCHEGOYEN, 106, 107 H. FALCKE, 99, 162, 155 J. FARMER, 150 G. FARRAR, 163 A.C. FAUTH, 144 N. FAZZINI, 161 F. FELDBUSCH, 164 F. FENU, 124, 102 B. FICK, 165 J.M. FIGUEIRA, 106 A. FILIP ˇCI ˇC, 166, 167 M.M. FREIRE, 168 T. FUJII, 150 A. FUSTER, 106, 107 R. GAIOR, 169 B. GARC'IA, 145 F. GAT'E, 170 H. GEMMEKE, 164 A. GHERGHEL-LASCU, 119 P.L. GHIA, 126 U. GIACCARI, 130, 171 M. GIAMMARCHI, 147 M. GILLER, 172 D. GŁAS, 173 C. GLASER, 134 G. GOLUP, 105 M. G'OMEZ BERISSO, 105 P.F. G 'OMEZ VITALE, 116, 117 N. GONZ'ALEZ, 106, 132 A. GORGI, 101, 102 M. GOTTOWIK, 122 A.F. GRILLO, 111, † T.D. GRUBB, 104 F. GUARINO, 120, 113 G.P. GUEDES, 174 R. HALLIDAY, 149 M.R. HAMPEL, 106 P. HANSEN, 159 D. HARARI, 105 T.A. HARRISON, 104 V.M. HARVEY, 104 A. HAUNGS, 132 T. HEBBEKER, 134 D. HECK, 132 P. HEIMANN, 136 A.E. HERVE, 135 G.C. HILL, 104 C. HOJVAT, 161 E. HOLT, 132, 106 P. HOMOLA, 131 J.R. H ORANDEL, 99, 155 P. HORVATH, 175 M. HRABOVSK'Y, 175 T. HUEGE, 132 J. HULSMAN, 106, 132 A. INSOLIA, 138, 139 P.G. ISAR, 114 I. JANDT, 122 J.A. JOHNSEN, 176 M. JOSEBACHUILI, 106 J. JURYSEK, 127 A. K A AP A, 122 K.H. KAMPERT, 122 B. KEILHAUER, 132 N. KEMMERICH, 103 J. KEMP, 134 R.M. KIECKHAFER, 165 H.O. KLAGES, 132 M. KLEIFGES, 164 J. KLEINFELLER, 116 R. KRAUSE, 134 N. KROHM, 122 D. KUEMPEL, 122 G. KUKEC MEZEK, 167 N. KUNKA, 164 A. KUOTB AWAD, 135 B.L. LAGO, 177 D. LAHURD, 149 R.G. LANG, 157 M. LAUSCHER, 134 R. LEGUMINA, 172 M.A. LEIGUI DE OLIVEIRA, 178 A. LETESSIER-SELVON, 169 I. LHENRY-YVON, 126 K. LINK, 135 D. LO PRESTI, 138, 139 L. LOPES, 100 R. L 'OPEZ, 179 A. L 'OPEZ CASADO, 109 R. LOREK, 149 Q. LUCE, 126 A. LUCERO, 106 M. MALACARI, 150 M. MALLAMACI, 141, 147 D. MANDAT, 127 P. MANTSCH, 161 A.G. MARIAZZI, 159 I.C. MARIS¸, 180 G. MARSELLA, 128, 129 D. MARTELLO, 128, 129 H. MARTINEZ, 181 O. MART'INEZ BRAVO, 179 J.J. MAS'IAS MEZA, 153 H.J. MATHES, 132 S. MATHYS, 122 J. MATTHEWS, 182 G. MATTHIAE, 183, 184 E. MAYOTTE, 122 P.O. MAZUR, 161 C. MEDINA, 176 G. MEDINA-TANCO, 108 D. MELO, 106 A. MENSHIKOV, 164 K.-D. MERENDA, 176 S. MICHAL, 175 M.I. MICHELETTI, 168 L. MIDDENDORF, 134 L. MIRAMONTI, 141, 147 B. MITRICA, 119 D. MOCKLER, 135 S. MOLLERACH, 105 F. MONTANET, 123 C. MORELLO, 101, 102 G. MORLINO, 110, 111 M. MOSTAF'A, 146 A.L. MULLER, 106, 132 G. MULLER, 134 M.A. MULLER, 144, 185 S. M ULLER, 135, 106 R. MUSSA, 102 I. NARANJO, 105 L. NELLEN, 108 P.H. NGUYEN, 104 M. NICULESCU-OGLINZANU, 119 M. NIECHCIOL, 136 L. NIEMIETZ, 122 T. NIGGEMANN, 134 D. NITZ, 165 D. NOSEK, 186 V. NOVOTNY, 186 L. NOˇZKA, 175 L.A. N 'U ˜NEZ, 115 F. OIKONOMOU, 146 A. OLINTO, 150 M. PALATKA, 127 J. PALLOTTA, 187 P. PAPENBREER, 122 G. PARENTE, 109 A. PARRA, 179 T. PAUL, 112 M. PECH, 127 F. PEDREIRA, 109 J. PE¸ KALA, 131 R. PELAYO, 188 J. PE ˜NA-RODRIGUEZ, 115 L.A.S. PEREIRA, 144 M. PERLIN, 106 L. PERRONE, 128, 129 C. PETERS, 134 S. PETRERA, 110, 111 J. PHUNTSOK, 146 T. PIEROG, 132 M. PIMENTA, 100 V. PIRRONELLO, 138, 139 M. PLATINO, 106 M. PLUM, 134 J. POH, 150 C. POROWSKI, 131 R.R. PRADO, 157 P. PRIVITERA, 150 M. PROUZA, 127 E.J. QUEL, 187 S. QUERCHFELD, 122 S. QUINN, 149 R. RAMOS-POLLAN, 115 J. RAUTENBERG, 122 D. RAVIGNANI, 106 J. RIDKY, 127 F. RIEHN, 100 M. RISSE, 136 P. RISTORI, 187 V. RIZI, 189, 111 W. RODRIGUES DE CARVALHO, 103 G. RODRIGUEZ FERNANDEZ, 183, 184 J. RODRIGUEZ ROJO, 116 M.J. RONCORONI, 106 M. ROTH, 132 E. ROULET, 105 A.C. ROVERO, 152 P. RUEHL, 136 S.J. SAFFI, 104 A. SAFTOIU, 119 F. SALAMIDA, 189, 111 H. SALAZAR, 179 A. SALEH, 167 G. SALINA, 184 F. S 'ANCHEZ, 106 P. SANCHEZ-LUCAS, 137 E.M. SANTOS, 103 E. SANTOS, 127 F. SARAZIN, 176 R. SARMENTO, 100 C. SARMIENTO-CANO, 106 R. SATO, 116 M. SCHAUER, 122 V. SCHERINI, 129 H. SCHIELER, 132 M. SCHIMP, 122 D. SCHMIDT, 132, 106 O. SCHOLTEN, 190, 191 P. SCHOV 'ANEK, 127 F.G. SCHR ODER, 132 S. SCHR ODER, 122 A. SCHULZ, 135 J. SCHUMACHER, 134 S.J. SCIUTTO, 159 A. SEGRETO, 192, 139 A. SHADKAM, 182 R.C. SHELLARD, 171 G. SIGL, 160 G. SILLI, 106, 132 R. ˇ SM'IDA, 132 G.R. SNOW, 193 P. SOMMERS, 146 S. SONNTAG, 136 J.F. SORIANO, 112 R. SQUARTINI, 116 D. STANCA, 119 S. STANIˇC, 167 J. STASIELAK, 131 P. STASSI, 123 M. STOLPOVSKIY, 123 F. STRAFELLA, 128, 129  \nA. STREICH, 135 F. SUAREZ, 106, 107 M. SUAREZ DUR'AN, 115 T. SUDHOLZ, 104 T. SUOMIJ ARVI, 126 A.D. SUPANITSKY, 152 J. ˇ SUP'IK, 175 J. SWAIN, 194 Z. SZADKOWSKI, 173 A. TABOADA, 132 O.A. TABORDA, 105 C. TIMMERMANS, 155, 99 C.J. TODERO PEIXOTO, 142 L. TOMANKOVA, 132 B. TOM'E, 100 G. TORRALBA ELIPE, 109 P. TRAVNICEK, 127 M. TRINI, 167 M. TUEROS, 159 R. ULRICH, 132 M. UNGER, 132 M. URBAN, 134 J.F. VALD'ES GALICIA, 108 I. VALI ˜NO, 109 L. VALORE, 120, 113 G. VAN AAR, 99 P. VAN BODEGOM, 104 A.M. VAN DEN BERG, 190 A. VAN VLIET, 99 E. VARELA, 179 B. VARGAS C'ARDENAS, 108 R.A. V 'AZQUEZ, 109 D. VEBERIˇC, 132 C. VENTURA, 156 I.D. VERGARA QUISPE, 159 V. VERZI, 184 J. VICHA, 127 L. VILLASE ˜NOR, 143 S. VOROBIOV, 167 H. WAHLBERG, 159 O. WAINBERG, 106, 107 D. WALZ, 134 A.A. WATSON, 195 M. WEBER, 164 A. WEINDL, 132 M. WIEDE'NSKI, 173 L. WIENCKE, 176 H. WILCZY'NSKI, 131 M. WIRTZ, 134 D. WITTKOWSKI, 122 B. WUNDHEILER, 106 L. YANG, 167 A. YUSHKOV, 127 E. ZAS, 109 D. ZAVRTANIK, 167, 166 M. ZAVRTANIK, 166, 167 A. ZEPEDA, 181 B. ZIMMERMANN, 164 M. ZIOLKOWSKI, 136 Z. ZONG, 126 AND 138, 139", '(THE PIERRE AUGER COLLABORATION)': "B. P. ABBOTT, 196 R. ABBOTT, 196 T. D. ABBOTT, 197 F. ACERNESE, 198, 199 K. ACKLEY, 200, 201 C. ADAMS, 202 T. ADAMS, 203 P. ADDESSO, 204 R. X. ADHIKARI, 196 V. B. ADYA, 205 C. AFFELDT, 205 M. AFROUGH, 206 B. AGARWAL, 207 M. AGATHOS, 208 K. AGATSUMA, 209 N. AGGARWAL, 210 O. D. AGUIAR, 211 L. AIELLO, 212, 213 A. AIN, 214 P. AJITH, 215 B. ALLEN, 205, 216, 217 G. ALLEN, 207 A. ALLOCCA, 218, 219 P. A. ALTIN, 220 A. AMATO, 221 A. ANANYEVA, 196 S. B. ANDERSON, 196 W. G. ANDERSON, 216 S. V. ANGELOVA, 222 S. ANTIER, 223 S. APPERT, 196 K. ARAI, 196 M. C. ARAYA, 196 J. S. AREEDA, 224 N. ARNAUD, 223, 225 K. G. ARUN, 226 S. ASCENZI, 227, 228 G. ASHTON, 205 M. AST, 229 S. M. ASTON, 202 P. ASTONE, 230 D. V. ATALLAH, 231 P. AUFMUTH, 217 C. AULBERT, 205 K. AULTONEAL, 232 C. AUSTIN, 197 A. AVILA-ALVAREZ, 224 S. BABAK, 233 P. BACON, 234 M. K. M. BADER, 209 S. BAE, 235 P. T. BAKER, 236 F. BALDACCINI, 237, 238 G. BALLARDIN, 225 S. W. BALLMER, 239 S. BANAGIRI, 240 J. C. BARAYOGA, 196 S. E. BARCLAY, 241 B. C. BARISH, 196 D. BARKER, 242 K. BARKETT, 243 F. BARONE, 198, 199 B. BARR, 241 L. BARSOTTI, 210 M. BARSUGLIA, 234 D. BARTA, 244 J. BARTLETT, 242 I. BARTOS, 245, 200 R. BASSIRI, 246 A. BASTI, 218, 219 J. C. BATCH, 242 M. BAWAJ, 247, 238 J. C. BAYLEY, 241 M. BAZZAN, 248, 249 B. B'ECSY, 250 C. BEER, 205 M. BEJGER, 251 I. BELAHCENE, 223 A. S. BELL, 241 B. K. BERGER, 196 G. BERGMANN, 205 J. J. BERO, 252 C. P. L. BERRY, 253 D. BERSANETTI, 254 A. BERTOLINI, 209 J. BETZWIESER, 202 S. BHAGWAT, 239 R. BHANDARE, 255 I. A. BILENKO, 256 G. BILLINGSLEY, 196 C. R. BILLMAN, 200 J. BIRCH, 202 R. BIRNEY, 257 O. BIRNHOLTZ, 205 S. BISCANS, 196, 210 S. BISCOVEANU, 258, 201 A. BISHT, 217 M. BITOSSI, 225, 219 C. BIWER, 239 M. A. BIZOUARD, 223 J. K. BLACKBURN, 196 J. BLACKMAN, 243 C. D. BLAIR, 196, 259 D. G. BLAIR, 259 R. M. BLAIR, 242 S. BLOEMEN, 260 O. BOCK, 205 N. BODE, 205 M. BOER, 261 G. BOGAERT, 261 A. BOHE, 233 F. BONDU, 262 E. BONILLA, 246 R. BONNAND, 203 B. A. BOOM, 209 R. BORK, 196 V. BOSCHI, 225, 219 S. BOSE, 263, 214 K. BOSSIE, 202 Y. BOUFFANAIS, 234 A. BOZZI, 225 C. BRADASCHIA, 219 P. R. BRADY, 216 M. BRANCHESI, 212, 213 J. E. BRAU, 264 T. BRIANT, 265 A. BRILLET, 261 M. BRINKMANN, 205 V. BRISSON, 223 P. BROCKILL, 216 J. E. BROIDA, 266 A. F. BROOKS, 196 D. A. BROWN, 239 D. D. BROWN, 267 S. BRUNETT, 196 C. C. BUCHANAN, 197 A. BUIKEMA, 210 T. BULIK, 268 H. J. BULTEN, 269, 209 A. BUONANNO, 233, 270 D. BUSKULIC, 203 C. BUY, 234 R. L. BYER, 246 M. CABERO, 205 L. CADONATI, 271 G. CAGNOLI, 221, 272 C. CAHILLANE, 196 J. CALDER 'ON BUSTILLO, 271 T. A. CALLISTER, 196 E. CALLONI, 273, 199 J. B. CAMP, 274 M. CANEPA, 275, 254 P. CANIZARES, 260 K. C. CANNON, 276 H. CAO, 267 J. CAO, 277 C. D. CAPANO, 205 E. CAPOCASA, 234 F. CARBOGNANI, 225 S. CARIDE, 278 M. F. CARNEY, 279 J. CASANUEVA DIAZ, 223 C. CASENTINI, 227, 228 S. CAUDILL, 216, 209 M. CAVAGLI'A, 206 F. CAVALIER, 223 R. CAVALIERI, 225 G. CELLA, 219 C. B. CEPEDA, 196 P. CERD 'A-DUR 'AN, 280 G. CERRETANI, 218, 219 E. CESARINI, 281, 228 S. J. CHAMBERLIN, 258 M. CHAN, 241 S. CHAO, 282 P. CHARLTON, 283 E. CHASE, 284 E. CHASSANDE-MOTTIN, 234 D. CHATTERJEE, 216 B. D. CHEESEBORO, 236 H. Y. CHEN, 285 X. CHEN, 259 Y. CHEN, 243 H.-P. CHENG, 200 H. CHIA, 200 A. CHINCARINI, 254 A. CHIUMMO, 225 T. CHMIEL, 279 H. S. CHO, 286 M. CHO, 270 J. H. CHOW, 220 N. CHRISTENSEN, 266, 261 Q. CHU, 259 A. J. K. CHUA, 208 S. CHUA, 265 A. K. W. CHUNG, 287 S. CHUNG, 259 G. CIANI, 200, 248, 249 R. CIOLFI, 288, 289 C. E. CIRELLI, 246 A. CIRONE, 275, 254 F. CLARA, 242 J. A. CLARK, 271 P. CLEARWATER, 290 F. CLEVA, 261 C. COCCHIERI, 206 E. COCCIA, 212, 213 P.-F. COHADON, 265 D. COHEN, 223 A. COLLA, 291, 230 C. G. COLLETTE, 292 L. R. COMINSKY, 293 M. CONSTANCIO JR., 211 L. CONTI, 249 S. J. COOPER, 253 P. CORBAN, 202 T. R. CORBITT, 197 I. CORDERO-CARRI'ON, 294 K. R. CORLEY, 245 N. CORNISH, 295 A. CORSI, 278 S. CORTESE, 225 C. A. COSTA, 211 M. W. COUGHLIN, 266, 196 S. B. COUGHLIN, 284 J.-P. COULON, 261 S. T. COUNTRYMAN, 245 P. COUVARES, 196 P. B. COVAS, 296 E. E. COWAN, 271 D. M. COWARD, 259 M. J. COWART, 202 D. C. COYNE, 196 R. COYNE, 278 J. D. E. CREIGHTON, 216 T. D. CREIGHTON, 297 J. CRIPE, 197 S. G. CROWDER, 298 T. J. CULLEN, 224, 197 A. CUMMING, 241 L. CUNNINGHAM, 241 E. CUOCO, 225 T. DAL CANTON, 274 G. D 'ALYA, 250 S. L. DANILISHIN, 217, 205 S. D'ANTONIO, 228 K. DANZMANN, 217, 205 A. DASGUPTA, 299 C. F. DA SILVA COSTA, 200 V. DATTILO, 225 I. DAVE, 255 M. DAVIER, 223 D. DAVIS, 239 E. J. DAW, 300 B. DAY, 271 S. DE, 239 D. DEBRA, 246 J. DEGALLAIX, 221 M. DE LAURENTIS, 212, 199 S. DEL'EGLISE, 265 W. DEL POZZO, 253, 218, 219 N. DEMOS, 210 T. DENKER, 205 T. DENT, 205 R. DE PIETRI, 301, 302 V. DERGACHEV, 233 R. DE ROSA, 273, 199 R. T. DEROSA, 202 C. DE ROSSI, 221, 225 R. DESALVO, 303 O. DE VARONA, 205 J. DEVENSON, 222 S. DHURANDHAR, 214 M. C. D'IAZ, 297 L. DI FIORE, 199 M. DI GIOVANNI, 304, 289 T. DI GIROLAMO, 245, 273, 199 A. DI LIETO, 218, 219 S. DI PACE, 291, 230 I. DI PALMA, 291, 230 F. DI RENZO, 218, 219 Z. DOCTOR, 285 V. DOLIQUE, 221 F. DONOVAN, 210 K. L. DOOLEY, 206 S. DORAVARI, 205 I. DORRINGTON, 231 R. DOUGLAS, 241 M. DOVALE ' ALVAREZ, 253 T. P. DOWNES, 216 M. DRAGO, 205 C. DREISSIGACKER, 205 J. C. DRIGGERS, 242 Z. DU, 277 M. DUCROT, 203 P. DUPEJ, 241 S. E. DWYER, 242 T. B. EDO, 300 M. C. EDWARDS, 266 A. EFFLER, 202 H.-B. EGGENSTEIN, 233, 205 P. EHRENS, 196 J. EICHHOLZ, 196 S. S. EIKENBERRY, 200 R. A. EISENSTEIN, 210 R. C. ESSICK, 210 D. ESTEVEZ, 203 Z. B. ETIENNE, 236 T. ETZEL, 196 M. EVANS, 210 T. M. EVANS, 202 M. FACTOUROVICH, 245 V. FAFONE, 227, 228, 212 H. FAIR, 239 S. FAIRHURST, 231 X. FAN, 277 S. FARINON, 254 B. FARR, 285 W. M. FARR, 253 E. J. FAUCHON-JONES, 231 M. FAVATA, 305 M. FAYS, 231 C. FEE, 279 H. FEHRMANN, 205 J. FEICHT, 196 M. M. FEJER, 246  \nA. FERNANDEZ-GALIANA,  \n210  \nI. FERRANTE,  \n218, 219  \nE. C. FERREIRA,  \n211  \nF. FERRINI,  \n225  \nF. FIDECARO,  \n218, 219  \nD. FINSTAD,  \n239  \nI. FIORI,  \n225  \nD. FIORUCCI, 234 M. FISHBACH, 285 R. P. FISHER, 239 M. FITZ-AXEN, 240 R. FLAMINIO, 221, 306 M. FLETCHER, 241 H. FONG, 307 J. A. FONT, 280, 308 P. W. F. FORSYTH, 220 S. S. FORSYTH, 271 J.-D. FOURNIER, 261 S. FRASCA, 291, 230 F. FRASCONI, 219 Z. FREI, 250 A. FREISE, 253 R. FREY, 264 V. FREY, 223 E. M. FRIES, 196 P. FRITSCHEL, 210 V. V. FROLOV, 202 P. FULDA, 200 M. FYFFE, 202 H. GABBARD, 241 B. U. GADRE, 214 S. M. GAEBEL, 253 J. R. GAIR, 309 L. GAMMAITONI, 237 M. R. GANIJA, 267 S. G. GAONKAR, 214 C. GARCIA-QUIROS, 296 F. GARUFI, 273, 199 B. GATELEY, 242 S. GAUDIO, 232 G. GAUR, 310 V. GAYATHRI, 311 N. GEHRELS, 274, † G. GEMME, 254 E. GENIN, 225 A. GENNAI, 219 D. GEORGE, 207 J. GEORGE, 255 L. GERGELY, 312 V. GERMAIN, 203 S. GHONGE, 271 ABHIRUP GHOSH, 215 ARCHISMAN GHOSH, 215, 209 S. GHOSH, 260, 209, 216 J. A. GIAIME, 197, 202 K. D. GIARDINA, 202 A. GIAZOTTO, 219 K. GILL, 232 L. GLOVER, 303 E. GOETZ, 313 R. GOETZ, 200 S. GOMES, 231 B. GONCHAROV, 201 G. GONZ'ALEZ, 197 J. M. GONZALEZ CASTRO, 218, 219 A. GOPAKUMAR, 314 M. L. GORODETSKY, 256 S. E. GOSSAN, 196 M. GOSSELIN, 225 R. GOUATY, 203 A. GRADO, 315, 199 C. GRAEF, 241 M. GRANATA, 221 A. GRANT, 241 S. GRAS, 210 C. GRAY, 242 G. GRECO, 316, 317 A. C. GREEN, 253 E. M. GRETARSSON, 232 P. GROOT, 260 H. GROTE, 205 S. GRUNEWALD, 233 P. GRUNING, 223 G. M. GUIDI, 316, 317 X. GUO, 277 A. GUPTA, 258 M. K. GUPTA, 299 K. E. GUSHWA, 196 E. K. GUSTAFSON, 196 R. GUSTAFSON, 313 O. HALIM, 213, 212 B. R. HALL, 263 E. D. HALL, 210 E. Z. HAMILTON, 231 G. HAMMOND, 241 M. HANEY, 318 M. M. HANKE, 205 J. HANKS, 242 C. HANNA, 258 M. D. HANNAM, 231 O. A. HANNUKSELA, 287 J. HANSON, 202 T. HARDWICK, 197 J. HARMS, 212, 213 G. M. HARRY, 319 I. W. HARRY, 233 M. J. HART, 241 C.-J. HASTER, 307 K. HAUGHIAN, 241 J. HEALY, 252 A. HEIDMANN, 265 M. C. HEINTZE, 202 H. HEITMANN, 261 P. HELLO, 223 G. HEMMING, 225 M. HENDRY, 241 I. S. HENG, 241 J. HENNIG, 241 A. W. HEPTONSTALL, 196 M. HEURS, 205, 217 S. HILD, 241 T. HINDERER, 260 D. HOAK, 225 D. HOFMAN, 221 K. HOLT, 202 D. E. HOLZ, 285 P. HOPKINS, 231 C. HORST, 216 J. HOUGH, 241 E. A. HOUSTON, 241 E. J. HOWELL, 259 A. HREIBI, 261 Y. M. HU, 205 E. A. HUERTA, 207 D. HUET, 223 B. HUGHEY, 232 S. HUSA, 296 S. H. HUTTNER, 241 T. HUYNH-DINH, 202 N. INDIK, 205 R. INTA, 278 G. INTINI, 291, 230 H. N. ISA, 241 J.-M. ISAC, 265 M. ISI, 196 B. R. IYER, 215 K. IZUMI, 242 T. JACQMIN, 265 K. JANI, 271 P. JARANOWSKI, 320 S. JAWAHAR, 257 F. JIM'ENEZ-FORTEZA, 296 W. W. JOHNSON, 197 D. I. JONES, 321 R. JONES, 241 R. J. G. JONKER, 209 L. JU, 259 J. JUNKER, 205 C. V. KALAGHATGI, 231 V. KALOGERA, 284 B. KAMAI, 196 S. KANDHASAMY, 202 G. KANG, 235 J. B. KANNER, 196 S. J. KAPADIA, 216 S. KARKI, 264 K. S. KARVINEN, 205 M. KASPRZACK, 197 M. KATOLIK, 207 E. KATSAVOUNIDIS, 210 W. KATZMAN, 202 S. KAUFER, 217 K. KAWABE, 242 F. K'EF'ELIAN, 261 D. KEITEL, 241 A. J. KEMBALL, 207 R. KENNEDY, 300 C. KENT, 231 J. S. KEY, 322 F. Y. KHALILI, 256 I. KHAN, 212, 228 S. KHAN, 205 Z. KHAN, 299 E. A. KHAZANOV, 323 N. KIJBUNCHOO, 220 CHUNGLEE KIM, 324 J. C. KIM, 325 K. KIM, 287 W. KIM, 267 W. S. KIM, 326 Y.-M. KIM, 286 S. J. KIMBRELL, 271 E. J. KING, 267 P. J. KING, 242 M. KINLEY-HANLON, 319 R. KIRCHHOFF, 205 J. S. KISSEL, 242 L. KLEYBOLTE, 229 S. KLIMENKO, 200 T. D. KNOWLES, 236 P. KOCH, 205 S. M. KOEHLENBECK, 205 S. KOLEY, 209 V. KONDRASHOV, 196 A. KONTOS, 210 M. KOROBKO, 229 W. Z. KORTH, 196 I. KOWALSKA, 268 D. B. KOZAK, 196 C. KR AMER, 205 V. KRINGEL, 205 B. KRISHNAN, 205 A. KR'OLAK, 327, 328 G. KUEHN, 205 P. KUMAR, 307 R. KUMAR, 299 S. KUMAR, 215 L. KUO, 282 A. KUTYNIA, 327 S. KWANG, 216 B. D. LACKEY, 233 K. H. LAI, 287 M. LANDRY, 242 R. N. LANG, 329 J. LANGE, 252 B. LANTZ, 246 R. K. LANZA, 210 A. LARTAUX-VOLLARD, 223 P. D. LASKY, 201 M. LAXEN, 202 A. LAZZARINI, 196 C. LAZZARO, 249 P. LEACI, 291, 230 S. LEAVEY, 241 C. H. LEE, 286 H. K. LEE, 330 H. M. LEE, 331 H. W. LEE, 325 K. LEE, 241 J. LEHMANN, 205 A. LENON, 236 M. LEONARDI, 304, 289 N. LEROY, 223 N. LETENDRE, 203 Y. LEVIN, 201 T. G. F. LI, 287 S. D. LINKER, 303 T. B. LITTENBERG, 332 J. LIU, 259 R. K. L. LO, 287 N. A. LOCKERBIE, 257 L. T. LONDON, 231 J. E. LORD, 239 M. LORENZINI, 212, 213 V. LORIETTE, 333 M. LORMAND, 202 G. LOSURDO, 219 J. D. LOUGH, 205 C. O. LOUSTO, 252 G. LOVELACE, 224 H. L UCK, 217, 205 D. LUMACA, 227, 228 A. P. LUNDGREN, 205 R. LYNCH, 210 Y. MA, 243 R. MACAS, 231 S. MACFOY, 222 B. MACHENSCHALK, 205 M. MACINNIS, 210 D. M. MACLEOD, 231 I. MAGA˜NA HERNANDEZ, 216 F. MAGA˜NA-SANDOVAL, 239 L. MAGA˜NA ZERTUCHE, 239 R. M. MAGEE, 258 E. MAJORANA, 230 I. MAKSIMOVIC, 333 N. MAN, 261 V. MANDIC, 240 V. MANGANO, 241 G. L. MANSELL, 220 M. MANSKE, 216, 220 M. MANTOVANI, 225 F. MARCHESONI, 247, 238 F. MARION, 203 S. M 'ARKA, 245 Z. M'ARKA, 245 C. MARKAKIS, 207 A. S. MARKOSYAN, 246 A. MARKOWITZ, 196 E. MAROS, 196 A. MARQUINA, 294 F. MARTELLI, 316, 317 L. MARTELLINI, 261 I. W. MARTIN, 241 R. M. MARTIN, 305 D. V. MARTYNOV, 210 K. MASON, 210 E. MASSERA, 300 A. MASSEROT, 203 T. J. MASSINGER, 196 M. MASSO-REID, 241 S. MASTROGIOVANNI, 291, 230 A. MATAS, 240 F. MATICHARD, 196, 210 L. MATONE, 245 N. MAVALVALA, 210 N. MAZUMDER, 263 R. MCCARTHY, 242 D. E. MCCLELLAND, 220 S. MCCORMICK, 202 L. MCCULLER, 210 S. C. MCGUIRE, 334 G. MCINTYRE, 196 J. MCIVER, 196 D. J. MCMANUS, 220 L. MCNEILL, 201 T. MCRAE, 220 S. T. MCWILLIAMS, 236 D. MEACHER, 258 G. D. MEADORS, 233, 205 M. MEHMET, 205 J. MEIDAM, 209 E. MEJUTO-VILLA, 204 A. MELATOS, 290 G. MENDELL, 242 R. A. MERCER, 216 E. L. MERILH, 242 M. MERZOUGUI, 261 S. MESHKOV, 196 C. MESSENGER, 241 C. MESSICK, 258 R. METZDORFF, 265 P. M. MEYERS, 240 H. MIAO, 253 C. MICHEL, 221 H. MIDDLETON, 253 E. E. MIKHAILOV, 335 L. MILANO, 273, 199 A. L. MILLER, 200, 291, 230 B. B. MILLER, 284 J. MILLER, 210 M. MILLHOUSE, 295 M. C. MILOVICH-GOFF, 303 O. MINAZZOLI, 261, 336 Y. MINENKOV, 228 J. MING, 233 C. MISHRA, 337 S. MITRA, 214 V. P. MITROFANOV, 256 G. MITSELMAKHER, 200 R. MITTLEMAN, 210 D. MOFFA, 279 A. MOGGI, 219 K. MOGUSHI, 206 M. MOHAN, 225 S. R. P. MOHAPATRA, 210 M. MONTANI, 316, 317 C. J. MOORE, 208 D. MORARU, 242 G. MORENO, 242 S. R. MORRISS, 297 B. MOURS, 203 C. M. MOW-LOWRY, 253 G. MUELLER, 200 A. W. MUIR, 231 ARUNAVA MUKHERJEE, 205 D. MUKHERJEE, 216 S. MUKHERJEE, 297 N. MUKUND, 214 A. MULLAVEY, 202 J. MUNCH, 267 E. A. MU ˜NIZ, 239 M. MURATORE, 232 P. G. MURRAY, 241 K. NAPIER, 271 I. NARDECCHIA, 227, 228 L. NATICCHIONI, 291, 230 R. K. NAYAK, 338 J. NEILSON, 303 G. NELEMANS, 260, 209 T. J. N. NELSON, 202 M. NERY, 205 A. NEUNZERT, 313 L. NEVIN, 196 J. M. NEWPORT, 319 G. NEWTON, 241, ‡ K. K. Y. NG, 287 T. T. NGUYEN, 220 D. NICHOLS, 260 A. B. NIELSEN, 205 S. NISSANKE, 260, 209 A. NITZ, 205 A. NOACK, 205 F. NOCERA, 225 D. NOLTING, 202 C. NORTH, 231 L. K. NUTTALL, 231 J. OBERLING, 242 G. D. O'DEA, 303 G. H. OGIN, 339 J. J. OH, 326 S. H. OH, 326 F. OHME, 205 M. A. OKADA, 211 M. OLIVER, 296 P. OPPERMANN, 205 RICHARD J. ORAM, 202 B. O'REILLY, 202 R. ORMISTON, 240 L. F. ORTEGA, 200 R. O'SHAUGHNESSY, 252 S. OSSOKINE, 233 D. J. OTTAWAY, 267 H. OVERMIER, 202 B. J. OWEN, 278 A. E. PACE, 258 J. PAGE, 332 M. A. PAGE, 259 A. PAI, 311, 340 S. A. PAI, 255 J. R. PALAMOS, 264 O. PALASHOV, 323 C. PALOMBA, 230 A. PAL-SINGH, 229 HOWARD PAN, 282 HUANG-WEI PAN, 282  \nB. PANG, 243 P. T. H. PANG, 287 C. PANKOW, 284 F. PANNARALE, 231 B. C. PANT, 255 F. PAOLETTI, 219 A. PAOLI, 225 M. A. PAPA, 233, 216, 205 A. PARIDA, 214 W. PARKER, 202 D. PASCUCCI, 241 A. PASQUALETTI, 225 R. PASSAQUIETI, 218, 219 D. PASSUELLO, 219 M. PATIL, 328 B. PATRICELLI, 341, 219 B. L. PEARLSTONE, 241 M. PEDRAZA, 196 R. PEDURAND, 221, 342 L. PEKOWSKY, 239 A. PELE, 202 S. PENN, 343 C. J. PEREZ, 242 A. PERRECA, 196, 304, 289 L. M. PERRI, 284 H. P. PFEIFFER, 307, 233 M. PHELPS, 241 O. J. PICCINNI, 291, 230 M. PICHOT, 261 F. PIERGIOVANNI, 316, 317 V. PIERRO, 204 G. PILLANT, 225 L. PINARD, 221 I. M. PINTO, 204 M. PIRELLO, 242 M. PITKIN, 241 M. POE, 216 R. POGGIANI, 218, 219 P. POPOLIZIO, 225 E. K. PORTER, 234 A. POST, 205 J. POWELL, 241, 344 J. PRASAD, 214 J. W. W. PRATT, 232 G. PRATTEN, 296 V. PREDOI, 231 T. PRESTEGARD, 216 M. PRIJATELJ, 205 M. PRINCIPE, 204 S. PRIVITERA, 233 G. A. PRODI, 304, 289 L. G. PROKHOROV, 256 O. PUNCKEN, 205 M. PUNTURO, 238 P. PUPPO, 230 M. P URRER, 233 H. QI, 216 V. QUETSCHKE, 297 E. A. QUINTERO, 196 R. QUITZOW-JAMES, 264 F. J. RAAB, 242 D. S. RABELING, 220 H. RADKINS, 242 P. RAFFAI, 250 S. RAJA, 255 C. RAJAN, 255 B. RAJBHANDARI, 278 M. RAKHMANOV, 297 K. E. RAMIREZ, 297 A. RAMOS-BUADES, 296 P. RAPAGNANI, 291, 230 V. RAYMOND, 233 M. RAZZANO, 218, 219 J. READ, 224 T. REGIMBAU, 261 L. REI, 254 S. REID, 257 D. H. REITZE, 196, 200 W. REN, 207 S. D. REYES, 239 F. RICCI, 291, 230 P. M. RICKER, 207 S. RIEGER, 205 K. RILES, 313 M. RIZZO, 252 N. A. ROBERTSON, 196, 241 R. ROBIE, 241 F. ROBINET, 223 A. ROCCHI, 228 L. ROLLAND, 203 J. G. ROLLINS, 196 V. J. ROMA, 264 R. ROMANO, 198, 199 C. L. ROMEL, 242 J. H. ROMIE, 202 D. ROSI 'NSKA, 345, 251 M. P. ROSS, 346 S. ROWAN, 241 A. R UDIGER, 205 P. RUGGI, 225 G. RUTINS, 222 K. RYAN, 242 S. SACHDEV, 196 T. SADECKI, 242 L. SADEGHIAN, 216 M. SAKELLARIADOU, 347 L. SALCONI, 225 M. SALEEM, 311 F. SALEMI, 205 A. SAMAJDAR, 338 L. SAMMUT, 201 L. M. SAMPSON, 284 E. J. SANCHEZ, 196 L. E. SANCHEZ, 196 N. SANCHIS-GUAL, 280 V. SANDBERG, 242 J. R. SANDERS, 239 B. SASSOLAS, 221 P. R. SAULSON, 239 O. SAUTER, 313 R. L. SAVAGE, 242 A. SAWADSKY, 229 P. SCHALE, 264 M. SCHEEL, 243 J. SCHEUER, 284 J. SCHMIDT, 205 P. SCHMIDT, 196, 260 R. SCHNABEL, 229 R. M. S. SCHOFIELD, 264 A. SCH ONBECK, 229 E. SCHREIBER, 205 D. SCHUETTE, 205, 217 B. W. SCHULTE, 205 B. F. SCHUTZ, 231, 205 S. G. SCHWALBE, 232 J. SCOTT, 241 S. M. SCOTT, 220 E. SEIDEL, 207 D. SELLERS, 202 A. S. SENGUPTA, 348 D. SENTENAC, 225 V. SEQUINO, 227, 228, 212 A. SERGEEV, 323 D. A. SHADDOCK, 220 T. J. SHAFFER, 242 A. A. SHAH, 332 M. S. SHAHRIAR, 284 M. B. SHANER, 303 L. SHAO, 233 B. SHAPIRO, 246 P. SHAWHAN, 270 A. SHEPERD, 216 D. H. SHOEMAKER, 210 D. M. SHOEMAKER, 271 K. SIELLEZ, 271 X. SIEMENS, 216 M. SIENIAWSKA, 251 D. SIGG, 242 A. D. SILVA, 211 L. P. SINGER, 274 A. SINGH, 233, 205, 217 A. SINGHAL, 212, 230 A. M. SINTES, 296 B. J. J. SLAGMOLEN, 220 B. SMITH, 202 J. R. SMITH, 224 R. J. E. SMITH, 196, 201 S. SOMALA, 349 E. J. SON, 326 J. A. SONNENBERG, 216 B. SORAZU, 241 F. SORRENTINO, 254 T. SOURADEEP, 214 A. P. SPENCER, 241 A. K. SRIVASTAVA, 299 K. STAATS, 232 A. STALEY, 245 M. STEINKE, 205 J. STEINLECHNER, 229, 241 S. STEINLECHNER, 229 D. STEINMEYER, 205 S. P. STEVENSON, 253, 344 R. STONE, 297 D. J. STOPS, 253 K. A. STRAIN, 241 G. STRATTA, 316, 317 S. E. STRIGIN, 256 A. STRUNK, 242 R. STURANI, 350 A. L. STUVER, 202 T. Z. SUMMERSCALES, 351 L. SUN, 290 S. SUNIL, 299 J. SURESH, 214 P. J. SUTTON, 231 B. L. SWINKELS, 225 M. J. SZCZEPA 'NCZYK, 232 M. TACCA, 209 S. C. TAIT, 241 C. TALBOT, 201 D. TALUKDER, 264 D. B. TANNER, 200 M. T'APAI, 312 A. TARACCHINI, 233 J. D. TASSON, 266 J. A. TAYLOR, 332 R. TAYLOR, 196 S. V. TEWARI, 343 T. THEEG, 205 F. THIES, 205 E. G. THOMAS, 253 M. THOMAS, 202 P. THOMAS, 242 K. A. THORNE, 202 E. THRANE, 201 S. TIWARI, 212, 289 V. TIWARI, 231 K. V. TOKMAKOV, 257 K. TOLAND, 241 M. TONELLI, 218, 219 Z. TORNASI, 241 A. TORRES-FORN'E, 280 C. I. TORRIE, 196 D. T OYR A, 253 F. TRAVASSO, 225, 238 G. TRAYLOR, 202 J. TRINASTIC, 200 M. C. TRINGALI, 304, 289 L. TROZZO, 352, 219 K. W. TSANG, 209 M. TSE, 210 R. TSO, 196 L. TSUKADA, 276 D. TSUNA, 276 D. TUYENBAYEV, 297 K. UENO, 216 D. UGOLINI, 353 C. S. UNNIKRISHNAN, 314 A. L. URBAN, 196 S. A. USMAN, 231 H. VAHLBRUCH, 217 G. VAJENTE, 196 G. VALDES, 197 N. VAN BAKEL, 209 M. VAN BEUZEKOM, 209 J. F. J. VAN DEN BRAND, 269, 209 C. VAN DEN BROECK, 209, 354 D. C. VANDER-HYDE, 239 L. VAN DER SCHAAF, 209 J. V. VAN HEIJNINGEN, 209 A. A. VAN VEGGEL, 241 M. VARDARO, 248, 249 V. VARMA, 243 S. VASS, 196 M. VAS'UTH, 244 A. VECCHIO, 253 G. VEDOVATO, 249 J. VEITCH, 241 P. J. VEITCH, 267 K. VENKATESWARA, 346 G. VENUGOPALAN, 196 D. VERKINDT, 203 F. VETRANO, 316, 317 A. VICER'E, 316, 317 A. D. VIETS, 216 S. VINCIGUERRA, 253 D. J. VINE, 222 J.-Y. VINET, 261 S. VITALE, 210 T. VO, 239 H. VOCCA, 237, 238 C. VORVICK, 242 S. P. VYATCHANIN, 256 A. R. WADE, 196 L. E. WADE, 279 M. WADE, 279 R. WALET, 209 M. WALKER, 224 L. WALLACE, 196 S. WALSH, 233, 205, 216 G. WANG, 212, 317 H. WANG, 253 J. Z. WANG, 258 W. H. WANG, 297 Y. F. WANG, 287 R. L. WARD, 220 J. WARNER, 242 M. WAS, 203 J. WATCHI, 292 B. WEAVER, 242 L.-W. WEI, 205, 217 M. WEINERT, 205 A. J. WEINSTEIN, 196 R. WEISS, 210 L. WEN, 259 E. K. WESSEL, 207 P. WESSELS, 205 J. WESTERWECK, 205 T. WESTPHAL, 205 K. WETTE, 220 J. T. WHELAN, 252 B. F. WHITING, 200 C. WHITTLE, 201 D. WILKEN, 205 D. WILLIAMS, 241 R. D. WILLIAMS, 196 A. R. WILLIAMSON, 260 J. L. WILLIS, 196, 355 B. WILLKE, 217, 205 M. H. WIMMER, 205 W. WINKLER, 205 C. C. WIPF, 196 H. WITTEL, 205, 217 G. WOAN, 241 J. WOEHLER, 205 J. WOFFORD, 252 K. W. K. WONG, 287 J. WORDEN, 242 J. L. WRIGHT, 241 D. S. WU, 205 D. M. WYSOCKI, 252 S. XIAO, 196 H. YAMAMOTO, 196 C. C. YANCEY, 270 L. YANG, 356 M. J. YAP, 220 M. YAZBACK, 200 HANG YU, 210 HAOCUN YU, 210 M. YVERT, 203 A. ZADRO˙ZNY, 327 M. ZANOLIN, 232 T. ZELENOVA, 225 J.-P. ZENDRI, 249 M. ZEVIN, 284 L. ZHANG, 196 M. ZHANG, 335 T. ZHANG, 241 Y.-H. ZHANG, 252 C. ZHAO, 259 M. ZHOU, 284 Z. ZHOU, 284 S. J. ZHU, 233, 205 X. J. ZHU, 201 M. E. ZUCKER, 196, 210 AND J. ZWEIZIG 196  \n(LIGO SCIENTIFIC COLLABORATION AND VIRGO COLLABORATION)  \n- 7 IFIC - Instituto de F'ısica Corpuscular (CSIC - Universitat de Val'encia) c/ Catedr'atico Jos'e Beltr'an, 2 E-46980 Paterna, Valencia, Spain\n- 8 LAM - Laboratoire d'Astrophysique de Marseille, Pˆole de l' ' Etoile Site de Chˆateau-Gombert, rue Fr'ed'eric Joliot-Curie 38, 13388 Marseille Cedex 13, France\n- 9 National Center for Energy Sciences and Nuclear Techniques, B.P.1382, R. P.10001 Rabat, Morocco\n- 10 INFN - Laboratori Nazionali del Sud (LNS), Via S. Sofia 62, 95123 Catania, Italy\n- 11 Nikhef, Science Park, Amsterdam, The Netherlands\n- 12 Huygens-Kamerlingh Onnes Laboratorium, Universiteit Leiden, The Netherlands\n- 13 Institute of Space Science, RO-077125 Bucharest, M˘agurele, Romania\n- 14 Universiteit van Amsterdam, Instituut voor Hoge-Energie Fysica, Science Park 105, 1098 XG Amsterdam, The Netherlands\n- 15 INFN - Sezione di Roma, P.le Aldo Moro 2, 00185 Roma, Italy\n- 16 Dipartimento di Fisica dell'Universit'a La Sapienza, P.le Aldo Moro 2, 00185 Roma, Italy\n- 17 Gran Sasso Science Institute, Viale Francesco Crispi 7, 00167 L'Aquila, Italy\n- 18 University Mohammed V in Rabat, Faculty of Sciences, 4 av. Ibn Battouta, B.P. 1014, R.P. 10000 Rabat, Morocco\n- 19 INFN - Sezione di Bologna, Viale Berti-Pichat 6/2, 40127 Bologna, Italy\n- 20 INFN - Sezione di Bari, Via E. Orabona 4, 70126 Bari, Italy\n- 21 Department of Computer Architecture and Technology/CITIC, University of Granada, 18071 Granada, Spain\n- 22 G'eoazur, UCA, CNRS, IRD, Observatoire de la Cˆote d'Azur, Sophia Antipolis, France\n- 23 Dipartimento di Fisica dell'Universit'a, Via Dodecaneso 33, 16146 Genova, Italy\n- 24 Universit'e Paris-Sud, 91405 Orsay Cedex, France\n- 25 Friedrich-Alexander-Universitat Erlangen-Nurnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, 91058 Erlangen, Germany\n- 26 University Mohammed I, Laboratory of Physics of Matter and Radiations, B.P.717, Oujda 6000, Morocco\n- 27 Institut fur Theoretische Physik und Astrophysik, Universitat Wurzburg, Emil-Fischer Str. 31, 97074 Wurzburg, Germany\n- 28 Dipartimento di Fisica e Astronomia dell'Universit'a, Viale Berti Pichat 6/2, 40127 Bologna, Italy\n- 29 Laboratoire de Physique Corpusculaire, Clermont Universit'e, Universit'e Blaise Pascal, CNRS/IN2P3, BP 10448, F-63000 Clermont-Ferrand, France\n- 30\n- INFN - Sezione di Catania, Viale Andrea Doria 6, 95125 Catania, Italy\n- 31 31, Aix Marseille Universit'e CNRS ENSAM LSIS UMR 7296 13397 Marseille, France; Universit'e de Toulon CNRS LSIS UMR 7296, 83957 La Garde, France\n- 32 Institut Universitaire de France, 75005 Paris, France\n- 33 Universit'e de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France\n- 34 Royal Netherlands Institute of Sea Research (NIOZ) and Utrecht University, Landsdiep 4, 1797 SZ 't Horntje (Texel), the Netherlands\n- 35 Dr. Remeis-Sternwarte and ECAP, Friedrich-Alexander-Universitat Erlangen-Nurnberg, Sternwartstr. 7, 96049 , Germany\n- 36 Moscow State University, Skobeltsyn Institute of Nuclear Physics, Leninskie gory, 119991 Moscow, Russia\n- 37 Mediterranean Institute of Oceanography (MIO), Aix-Marseille University, 13288, Marseille, Cedex 9, France; Universit'e du Sud Toulon-Var, CNRS-INSU/IRD UM110, 83957, La Garde Cedex, France\n- 38 Dipartimento di Fisica ed Astronomia dell'Universit'a, Viale Andrea Doria 6, 95125 Catania, Italy\n- 39 Direction des Sciences de la Mati'ere - Institut de recherche sur les lois fondamentales de l'Univers - Service de Physique des Particules, CEA Saclay, 91191\n- Gif-sur-Yvette Cedex, France\n- 40 INFN - Sezione di Pisa, Largo B. Pontecorvo 3, 56127 Pisa, Italy\n- 41 Dipartimento di Fisica dell'Universit'a, Largo B. Pontecorvo 3, 56127 Pisa, Italy\n- 42 INFN - Sezione di Napoli, Via Cintia 80126 Napoli, Italy\n- 43 Dipartimento di Fisica dell'Universit'a Federico II di Napoli, Via Cintia 80126, Napoli, Italy\n- 44 Dpto. de F'ısica Te'orica y del Cosmos & C.A.F.P.E., University of Granada, 18071 Granada, Spain\n- 45 Dr. Remeis-Sternwarte and ECAP, Friedrich-Alexander-Universitat Erlangen-Nurnberg, Sternwartstr. 7, 96049 Bamberg, Germany\n- 46 Department of Physics, University of Adelaide, Adelaide, 5005, Australia\n- 47 DESY, D-15738 Zeuthen, Germany\n- 48 Dept. of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand\n- 49 Universit'e Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium\n- 50 Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark\n- 51 Oskar Klein Centre and Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden\n- 52 D'epartement de physique nucl'eaire et corpusculaire, Universit'e de Gen'eve, CH-1211 Gen'eve, Switzerland  \n- 55 Dept. of Physics, Pennsylvania State University, University Park, PA 16802, USA\n- 56 Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA\n- 57 III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany\n- 58 Physics Department, South Dakota School of Mines and Technology, Rapid City, SD 57701, USA\n- 59 Dept. of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2E1\n- 60 Dept. of Physics and Astronomy, University of California, Irvine, CA 92697, USA\n- 61 Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany\n- 62 Dept. of Physics, University of California, Berkeley, CA 94720, USA\n- 63 Dept. of Physics and Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA\n- 64 Dept. of Astronomy, Ohio State University, Columbus, OH 43210, USA\n- 65 Fakultat fur Physik & Astronomie, Ruhr-Universitat Bochum, D-44780 Bochum, Germany\n- 66 Dept. of Physics, University of Wuppertal, D-42119 Wuppertal, Germany\n- 67 Dept. of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA\n- 68 Dept. of Physics, University of Maryland, College Park, MD 20742, USA\n- 69 Dept. of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA\n- 70 Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA\n- 71 Dept. of Physics, TU Dortmund University, D-44221 Dortmund, Germany\n- 72 Dept. of Physics, Sungkyunkwan University, Suwon 440-746, Korea\n- 73 Dept. of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden\n- 74 Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin, Madison, WI 53706, USA\n- 75 Vrije Universiteit Brussel (VUB), Dienst ELEM, B-1050 Brussels, Belgium\n- 76 SNOLAB, 1039 Regional Road 24, Creighton Mine 9, Lively, ON, Canada P3Y 1N2\n- 77 Institut fur Kernphysik, Westfalische Wilhelms-Universitat Munster, D-48149 Munster, Germany\n- 78 Physik-department, Technische Universitat Munchen, D-85748 Garching, Germany\n- 79 Dept. of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, USA\n- 80 Dept. of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA\n- 81 Bartol Research Institute and Dept. of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA\n- 82 Dept. of Physics and Astronomy, University of Gent, B-9000 Gent, Belgium\n- 83 Institut fur Physik, Humboldt-Universitat zu Berlin, D-12489 Berlin, Germany\n- 84 Dept. of Physics, Southern University, Baton Rouge, LA 70813, USA\n- 85 Dept. of Astronomy, University of Wisconsin, Madison, WI 53706, USA\n- 86 Earthquake Research Institute, University of Tokyo, Bunkyo, Tokyo 113-0032, Japan\n- 87 Dept. of Physics and Institute for Global Prominent Research, Chiba University, Chiba 263-8522, Japan\n- 88 CTSPS, Clark-Atlanta University, Atlanta, GA 30314, USA\n- 89 Dept. of Physics, University of Texas at Arlington, 502 Yates St., Science Hall Rm 108, Box 19059, Arlington, TX 76019, USA\n- 90 Dept. of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA\n- 91 Universit'e de Mons, 7000 Mons, Belgium\n- 92 Dept. of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA\n- 93 Dept. of Physics, Drexel University, 3141 Chestnut Street, Philadelphia, PA 19104, USA\n- 94 Dept. of Physics, University of Wisconsin, River Falls, WI 54022, USA\n- 95 Dept. of Physics, Yale University, New Haven, CT 06520, USA\n- 96 School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA 30332, USA\n- 97 Dept. of Physics and Astronomy, University of Alaska Anchorage, 3211 Providence Dr., Anchorage, AK 99508, USA\n- 98 Dept. of Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP, UK\n- 99 IMAPP, Radboud University Nijmegen, Nijmegen, The Netherlands\n- 100 Laborat'orio de Instrumentac¸ ˜ao e F'ısica Experimental de Part'ıculas - LIP and Instituto Superior T'ecnico - IST, Universidade de Lisboa - UL, Lisboa, Portugal\n- 101 Osservatorio Astrofisico di Torino (INAF), Torino, Italy\n- 102 INFN, Sezione di Torino, Torino, Italy\n- 103 Universidade de S˜ao Paulo, Instituto de F'ısica, S˜ao Paulo, SP, Brazil\n- 104 University of Adelaide, Adelaide, S.A., Australia\n- 105 Centro At'omico Bariloche and Instituto Balseiro (CNEA-UNCuyo-CONICET), San Carlos de Bariloche, Argentina\n- 106 Instituto de Tecnolog'ıas en Detecci'on y Astropart'ıculas (CNEA, CONICET, UNSAM), Buenos Aires, Argentina\n- 107 Universidad Tecnol'ogica Nacional - Facultad Regional Buenos Aires, Buenos Aires, Argentina\n- 108 Universidad Nacional Aut'onoma de M'exico, M'exico, D.F., M'exico\n- 109 Universidad de Santiago de Compostela, Santiago de Compostela, Spain\n- 110 Gran Sasso Science Institute (INFN), L'Aquila, Italy\n- 111 INFN Laboratori Nazionali del Gran Sasso, Assergi (L'Aquila), Italy\n- 112 Department of Physics and Astronomy, Lehman College, City University of New York, Bronx, NY, USA  \n- 113 INFN, Sezione di Napoli, Napoli, Italy\n- 114 Institute of Space Science, Bucharest-Magurele, Romania\n- 115 Universidad Industrial de Santander, Bucaramanga, Colombia\n- 116 Observatorio Pierre Auger, Malargue, Argentina\n- 117 Observatorio Pierre Auger and Comisi'on Nacional de Energ'ıa At'omica, Malargue, Argentina\n- 118 University Politehnica of Bucharest, Bucharest, Romania\n- 119 'Horia Hulubei' National Institute for Physics and Nuclear Engineering, Bucharest-Magurele, Romania\n- 120 Universit'a di Napoli 'Federico II', Dipartimento di Fisica 'Ettore Pancini', Napoli, Italy\n- 121 Ohio State University, Columbus, OH, USA\n- 122 Bergische Universitat Wuppertal, Department of Physics, Wuppertal, Germany\n- 123 Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Universit'e Grenoble-Alpes, CNRS/IN2P3, Grenoble, France\n- 124 Universit'a Torino, Dipartimento di Fisica, Torino, Italy\n- 125\n- Max-Planck-Institut fur Radioastronomie, Bonn, Germany\n- 126 Institut de Physique Nucl'eaire d'Orsay (IPNO), Universit'e Paris-Sud, Univ. Paris/Saclay, CNRS-IN2P3, Orsay, France\n- 127 Institute of Physics of the Czech Academy of Sciences, Prague, Czech Republic\n- 128 Universit'a del Salento, Dipartimento di Matematica e Fisica 'E. De Giorgi', Lecce, Italy\n- 129 INFN, Sezione di Lecce, Lecce, Italy\n- 130 Universidade Federal do Rio de Janeiro, Instituto de F'ısica, Rio de Janeiro, RJ, Brazil\n- 131 Institute of Nuclear Physics PAN, Krakow, Poland\n- 132 Karlsruhe Institute of Technology, Institut fur Kernphysik, Karlsruhe, Germany\n- 133 Colorado State University, Fort Collins, CO\n- 134 RWTH Aachen University, III. Physikalisches Institut A, Aachen, Germany\n- 135 Karlsruhe Institute of Technology, Institut fur Experimentelle Kernphysik (IEKP), Karlsruhe, Germany\n- 136 Universitat Siegen, Fachbereich 7 Physik - Experimentelle Teilchenphysik, Siegen, Germany\n- 137 Universidad de Granada and C.A.F.P.E., Granada, Spain\n- 138 Universit'a di Catania, Dipartimento di Fisica e Astronomia, Catania, Italy\n- 139 INFN, Sezione di Catania, Catania, Italy\n- 140 Universidad Aut'onoma de Chiapas, Tuxtla Guti'errez, Chiapas, M'exico\n- 141 Universit'a di Milano, Dipartimento di Fisica, Milano, Italy\n- 142 Universidade de S˜ao Paulo, Escola de Engenharia de Lorena, Lorena, SP, Brazil\n- 143 Universidad Michoacana de San Nicol'as de Hidalgo, Morelia, Michoac'an, M'exico\n- 144 Universidade Estadual de Campinas, IFGW, Campinas, SP, Brazil\n- 145 Instituto de Tecnolog'ıas en Detecci'on y Astropart'ıculas (CNEA, CONICET, UNSAM), and Universidad Tecnol'ogica Nacional - Facultad Regional Mendoza (CONICET/CNEA), Mendoza, Argentina\n- 146 Pennsylvania State University, University Park, PA, USA\n- 147 INFN, Sezione di Milano, Milano, Italy\n- 148 Politecnico di Milano, Dipartimento di Scienze e Tecnologie Aerospaziali , Milano, Italy\n- 149 Case Western Reserve University, Cleveland, OH, USA\n- 150 University of Chicago, Enrico Fermi Institute, Chicago, IL, USA\n- 151 Universit'a del Salento, Dipartimento di Ingegneria, Lecce, Italy\n- 152 Instituto de Astronom'ıa y F'ısica del Espacio (IAFE, CONICET-UBA), Buenos Aires, Argentina\n- 153 Departamento de F'ısica and Departamento de Ciencias de la Atm'osfera y los Oc'eanos, FCEyN, Universidad de Buenos Aires and CONICET, Buenos Aires, Argentina\n- 154 Universidade Federal Fluminense, EEIMVR, Volta Redonda, RJ, Brazil\n- 155 Nationaal Instituut voor Kernfysica en Hoge Energie Fysica (NIKHEF), Science Park, Amsterdam, The Netherlands\n- 156 Universidade Federal do Rio de Janeiro (UFRJ), Observat'orio do Valongo, Rio de Janeiro, RJ, Brazil\n- 157 Universidade de S˜ao Paulo, Instituto de F'ısica de S˜ao Carlos, S˜ao Carlos, SP, Brazil\n- 158 Universidade Federal do Paran'a, Setor Palotina, Palotina, Brazil\n- 159 IFLP, Universidad Nacional de La Plata and CONICET, La Plata, Argentina\n- 160 Universitat Hamburg, II. Institut fur Theoretische Physik, Hamburg, Germany\n- 161 Fermi National Accelerator Laboratory, USA\n- 162 Stichting Astronomisch Onderzoek in Nederland (ASTRON), Dwingeloo, The Netherlands\n- 163 New York University, New York, NY, USA  \n- 165 Michigan Technological University, Houghton, MI, USA\n- 166 Experimental Particle Physics Department, J. Stefan Institute, Ljubljana, Slovenia\n- 167 Center for Astrophysics and Cosmology (CAC), University of Nova Gorica, Nova Gorica, Slovenia\n- 168 Instituto de F'ısica de Rosario (IFIR) - CONICET/U.N.R. and Facultad de Ciencias Bioqu'ımicas y Farmac'euticas U.N.R., Rosario, Argentina\n- 169 Laboratoire de Physique Nucl'eaire et de Hautes Energies (LPNHE), Universit'es Paris 6 et Paris 7, CNRS-IN2P3, Paris, France\n- 170 SUBATECH, ' Ecole des Mines de Nantes, CNRS-IN2P3, Universit'e de Nantes, France\n- 171 Centro Brasileiro de Pesquisas Fisicas, Rio de Janeiro, RJ, Brazil\n- 172 University of Ł'od'z, Faculty of Astrophysics, Ł'od'z, Poland\n- 173 University of Ł'od'z, Faculty of High-Energy Astrophysics,Ł'od'z, Poland\n- 174 Universidade Estadual de Feira de Santana, Feira de Santana, Brazil\n- 175 Palacky University, RCPTM, Olomouc, Czech Republic\n- 176 Colorado School of Mines, Golden, CO, USA\n- 177 Centro Federal de Educac¸˜ao Tecnol'ogica Celso Suckow da Fonseca, Nova Friburgo, Brazil\n- 178 Universidade Federal do ABC, Santo Andr'e, SP, Brazil\n- 179 Benem'erita Universidad Aut'onoma de Puebla, Puebla, M'exico\n- 180 Universit'e Libre de Bruxelles (ULB), Brussels, Belgium\n- 181 Centro de Investigaci'on y de Estudios Avanzados del IPN (CINVESTAV), M'exico, D.F., M'exico\n- 182 Louisiana State University, Baton Rouge, LA, USA\n- 183 Universit'a di Roma 'Tor Vergata', Dipartimento di Fisica, Roma, Italy\n- 184 INFN, Sezione di Roma 'Tor Vergata', Roma, Italy\n- 185 also at Universidade Federal de Alfenas, Bras'ılia, Brazil\n- 186 Charles University, Faculty of Mathematics and Physics, Institute of Particle and Nuclear Physics, Prague, Czech Republic\n- 187 Centro de Investigaciones en L'aseres y Aplicaciones, CITEDEF and CONICET, Villa Martelli, Argentina\n- 188 189\n- Unidad Profesional Interdisciplinaria en Ingenier'ıa y Tecnolog'ıas Avanzadas del Instituto Polit'ecnico Nacional (UPIITA-IPN), M'exico, D.F., M'exico\n- Universit'a dell'Aquila, Dipartimento di Scienze Fisiche e Chimiche, L'Aquila, Italy\n- 190 KVI - Center for Advanced Radiation Technology, University of Groningen, Groningen, The Netherlands\n- 191 also at Vrije Universiteit Brussels, Brussels, Belgium\n- 192 INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Palermo, Italy\n- 193 University of Nebraska, Lincoln, NE, USA\n- 194 Northeastern University, Boston, MA, USA\n- 195 School of Physics and Astronomy, University of Leeds, Leeds, United Kingdom\n- 196 LIGO, California Institute of Technology, Pasadena, CA 91125, USA\n- 197 Louisiana State University, Baton Rouge, LA 70803, USA\n- 198 Universit'a di Salerno, Fisciano, I-84084 Salerno, Italy\n- 199 INFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy\n- 200 University of Florida, Gainesville, FL 32611, USA\n- 201 OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia\n- 202 LIGO Livingston Observatory, Livingston, LA 70754, USA\n- 203 Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Universit'e Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy, France\n- 204 University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy\n- 205 Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany\n- 206 The University of Mississippi, University, MS 38677, USA\n- 207 NCSA, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA\n- 208 University of Cambridge, Cambridge CB2 1TN, United Kingdom\n- 209 Nikhef, Science Park, 1098 XG Amsterdam, The Netherlands\n- 210 LIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USA\n- 211 Instituto Nacional de Pesquisas Espaciais, 12227-010 S˜ao Jos'e dos Campos, S˜ao Paulo, Brazil\n- 212 Gran Sasso Science Institute (GSSI), I-67100 L'Aquila, Italy\n- 213 INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy\n- 214 Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India\n- 215 International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India\n- 216 University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA\n- 217 Leibniz Universitat Hannover, D-30167 Hannover, Germany\n- 218 Universit'a di Pisa, I-56127 Pisa, Italy  \n- 219 INFN, Sezione di Pisa, I-56127 Pisa, Italy\n- 220 OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia\n- 221 Laboratoire des Mat'eriaux Avanc'es (LMA), CNRS/IN2P3, F-69622 Villeurbanne, France\n- 222 SUPA, University of the West of Scotland, Paisley PA1 2BE, United Kingdom\n- 223 LAL, Univ. Paris-Sud, CNRS/IN2P3, Universit'e Paris-Saclay, F-91898 Orsay, France\n- 224 California State University Fullerton, Fullerton, CA 92831, USA\n- 225 European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy\n- 226 Chennai Mathematical Institute, Chennai 603103, India\n- 227 Universit'a di Roma Tor Vergata, I-00133 Roma, Italy\n- 228 INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy\n- 229 Universitat Hamburg, D-22761 Hamburg, Germany\n- 230 INFN, Sezione di Roma, I-00185 Roma, Italy\n- 231 Cardiff University, Cardiff CF24 3AA, United Kingdom\n- 232 Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA\n- 233 Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam-Golm, Germany\n- 234 APC, AstroParticule et Cosmologie, Universit'e Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cit'e, F-75205 Paris Cedex 13, France\n- 235 Korea Institute of Science and Technology Information, Daejeon 34141, Korea\n- 236 West Virginia University, Morgantown, WV 26506, USA\n- 237 Universit'a di Perugia, I-06123 Perugia, Italy\n- 238 INFN, Sezione di Perugia, I-06123 Perugia, Italy\n- 239 Syracuse University, Syracuse, NY 13244, USA\n- 240 University of Minnesota, Minneapolis, MN 55455, USA\n- 241 SUPA, University of Glasgow, Glasgow G12 8QQ, United Kingdom\n- 242 LIGO Hanford Observatory, Richland, WA 99352, USA\n- 243 Caltech CaRT, Pasadena, CA 91125, USA\n- 244 Wigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Mikl'os 'ut 29-33, Hungary\n- 245 Columbia University, New York, NY 10027, USA\n- 246 Stanford University, Stanford, CA 94305, USA\n- 247 Universit'a di Camerino, Dipartimento di Fisica, I-62032 Camerino, Italy\n- 248 Universit'a di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy\n- 249 INFN, Sezione di Padova, I-35131 Padova, Italy\n- 250 Institute of Physics, Eotvos University, P'azm'any P. s. 1/A, Budapest 1117, Hungary\n- 251 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland\n- 252 Rochester Institute of Technology, Rochester, NY 14623, USA\n- 253 University of Birmingham, Birmingham B15 2TT, United Kingdom\n- 254 INFN, Sezione di Genova, I-16146 Genova, Italy\n- 255 RRCAT, Indore MP 452013, India\n- 256 Faculty of Physics, Lomonosov Moscow State University, Moscow 119991, Russia\n- 257 SUPA, University of Strathclyde, Glasgow G1 1XQ, United Kingdom\n- 258 The Pennsylvania State University, University Park, PA 16802, USA\n- 259 OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia\n- 260 Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands\n- 261 Artemis, Universit'e Cˆote d'Azur, Observatoire Cˆote d'Azur, CNRS, CS 34229, F-06304 Nice Cedex 4, France\n- 262 Institut FOTON, CNRS, Universit'e de Rennes 1, F-35042 Rennes, France\n- 263 Washington State University, Pullman, WA 99164, USA\n- 264 University of Oregon, Eugene, OR 97403, USA\n- 265 Laboratoire Kastler Brossel, UPMC-Sorbonne Universit'es, CNRS, ENS-PSL Research University, Coll'ege de France, F-75005 Paris, France\n- 266 Carleton College, Northfield, MN 55057, USA\n- 267 OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia\n- 268 Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland\n- 269 VU University Amsterdam, 1081 HV Amsterdam, The Netherlands\n- 270 University of Maryland, College Park, MD 20742, USA\n- 271 Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA 30332, USA\n- 272 Universit'e Claude Bernard Lyon 1, F-69622 Villeurbanne, France\n- 273 Universit'a di Napoli 'Federico II,' Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy\n- 274 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA\n- 275 Dipartimento di Fisica, Universit'a degli Studi di Genova, I-16146 Genova, Italy\n- 276 RESCEU, University of Tokyo, Tokyo, 113-0033, Japan.\n- 277 Tsinghua University, Beijing 100084, China\n- 278 Texas Tech University, Lubbock, TX 79409, USA\n- 279 Kenyon College, Gambier, OH 43022, USA\n- 280 Departamento de Astronom'ıa y Astrof'ısica, Universitat de Val'encia, E-46100 Burjassot, Val'encia, Spain\n- 281 Museo Storico della Fisica e Centro Studi e Ricerche Enrico Fermi, I-00184 Roma, Italy\n- 282 National Tsing Hua University, Hsinchu City, 30013 Taiwan, Republic of China\n- 283 Charles Sturt University, Wagga Wagga, New South Wales 2678, Australia\n- 284 Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL 60208, USA\n- 285 University of Chicago, Chicago, IL 60637, USA\n- 286 Pusan National University, Busan 46241, Korea\n- 287 The Chinese University of Hong Kong, Shatin, NT, Hong Kong\n- 288 INAF, Osservatorio Astronomico di Padova, I-35122 Padova, Italy\n- 289 INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy\n- 290 OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia\n- 291 Universit'a di Roma 'La Sapienza,' I-00185 Roma, Italy\n- 292 Universit'e Libre de Bruxelles, Brussels 1050, Belgium\n- 293 Sonoma State University, Rohnert Park, CA 94928, USA\n- 294 Departamento de Matem'aticas, Universitat de Val'encia, E-46100 Burjassot, Val'encia, Spain\n- 295 Montana State University, Bozeman, MT 59717, USA\n- 296 Universitat de les Illes Balears, IAC3-IEEC, E-07122 Palma de Mallorca, Spain\n- 297 The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA\n- 298 Bellevue College, Bellevue, WA 98007, USA\n- 299 Institute for Plasma Research, Bhat, Gandhinagar 382428, India\n- 300 The University of Sheffield, Sheffield S10 2TN, United Kingdom\n- 301 Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Universit'a di Parma, I-43124 Parma, Italy\n- 302 INFN, Sezione di Milano Bicocca, Gruppo Collegato di Parma, I-43124 Parma, Italy\n- 303 California State University, Los Angeles, 5151 State University Dr, Los Angeles, CA 90032, USA\n- 304 Universit'a di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy\n- 305 Montclair State University, Montclair, NJ 07043, USA\n- 306 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan\n- 307 Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario M5S 3H8, Canada\n- 308 Observatori Astron'omic, Universitat de Val'encia, E-46980 Paterna, Val'encia, Spain\n- 309 School of Mathematics, University of Edinburgh, Edinburgh EH9 3FD, United Kingdom\n- 310 University and Institute of Advanced Research, Koba Institutional Area, Gandhinagar Gujarat 382007, India\n- 311 IISER-TVM, CET Campus, Trivandrum Kerala 695016, India\n- 312 University of Szeged, D'om t'er 9, Szeged 6720, Hungary\n- 313 University of Michigan, Ann Arbor, MI 48109, USA\n- 314 Tata Institute of Fundamental Research, Mumbai 400005, India\n- 315 INAF, Osservatorio Astronomico di Capodimonte, I-80131, Napoli, Italy\n- 316 Universit'a degli Studi di Urbino 'Carlo Bo,' I-61029 Urbino, Italy\n- 317 INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy\n- 318 Physik-Institut, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland\n- 319 American University, Washington, D.C. 20016, USA\n- 320 University of Białystok, 15-424 Białystok, Poland\n- 321 University of Southampton, Southampton SO17 1BJ, United Kingdom\n- 322 University of Washington Bothell, 18115 Campus Way NE, Bothell, WA 98011, USA\n- 323 Institute of Applied Physics, Nizhny Novgorod, 603950, Russia\n- 324 Korea Astronomy and Space Science Institute, Daejeon 34055, Korea\n- 325 Inje University Gimhae, South Gyeongsang 50834, Korea  \n- 326 National Institute for Mathematical Sciences, Daejeon 34047, Korea\n- 327 NCBJ, 05-400 ' Swierk-Otwock, Poland\n- 328 Institute of Mathematics, Polish Academy of Sciences, 00656 Warsaw, Poland\n- 329 Hillsdale College, Hillsdale, MI 49242, USA\n- 330 Hanyang University, Seoul 04763, Korea\n- 331 Seoul National University, Seoul 08826, Korea\n- 332 NASA Marshall Space Flight Center, Huntsville, AL 35811, USA\n- 333 ESPCI, CNRS, F-75005 Paris, France\n- 334 Southern University and A&M College, Baton Rouge, LA 70813, USA\n- 335 College of William and Mary, Williamsburg, VA 23187, USA\n- 336 Centre Scientifique de Monaco, 8 quai Antoine Ier, MC-98000, Monaco\n- 337 Indian Institute of Technology Madras, Chennai 600036, India\n- 338 IISER-Kolkata, Mohanpur, West Bengal 741252, India\n- 339 Whitman College, 345 Boyer Avenue, Walla Walla, WA 99362 USA\n- 340 Indian Institute of Technology Bombay, Powai, Mumbai, Maharashtra 400076, India\n- 341 Scuola Normale Superiore, Piazza dei Cavalieri 7, I-56126 Pisa, Italy\n- 342 Universit'e de Lyon, F-69361 Lyon, France\n- 343 Hobart and William Smith Colleges, Geneva, NY 14456, USA\n- 344 OzGrav, Swinburne University of Technology, Hawthorn VIC 3122, Australia\n- 345 Janusz Gil Institute of Astronomy, University of Zielona G'ora, 65-265 Zielona G'ora, Poland\n- 346 University of Washington, Seattle, WA 98195, USA\n- 347 King's College London, University of London, London WC2R 2LS, United Kingdom\n- 348 Indian Institute of Technology, Gandhinagar Ahmedabad Gujarat 382424, India\n- 349 Indian Institute of Technology Hyderabad, Sangareddy, Khandi, Telangana 502285, India\n- 350 International Institute of Physics, Universidade Federal do Rio Grande do Norte, Natal RN 59078-970, Brazil\n- 351 Andrews University, Berrien Springs, MI 49104, USA\n- 352 Universit'a di Siena, I-53100 Siena, Italy\n- 353 Trinity University, San Antonio, TX 78212, USA", 'ABSTRACT': 'The Advanced LIGO and Advanced Virgo observatories recently discovered gravitational waves from a binary neutron star inspiral. A short gamma-ray burst (GRB) that followed the merger of this binary was also recorded by the Fermi Gamma-ray Burst Monitor (Fermi-GBM), and the Anticoincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory (INTEGRAL), indicating particle acceleration by the source. The precise location of the event was determined by optical detections of emission following the merger. We searched for high-energy neutrinos from the merger in the GeV-EeV energy range using the ANTARES, IceCube, and Pierre Auger Observatories. No neutrinos directionally coincident with the source were detected within ± 500 s around the merger time. Additionally, no MeV neutrino burst signal was detected coincident with the merger. We further carried out an extended search in the direction of the source for high-energy neutrinos within the 14-day period following the merger, but found no evidence of emission. We used these results to probe dissipation mechanisms in relativistic outflows driven by the binary neutron star merger. The non-detection is consistent with model predictions of short GRBs observed at a large off-axis angle.  \nKeywords: neutrinos - gravitational waves - gamma-ray burst: individual  \n- ∗ Deceased, August 2016.', '1. INTRODUCTION': "The observation of binary neutron star mergers with multiple cosmic messengers is a unique opportunity that enables the detailed study of the merger process, and provides insight into astrophysical particle acceleration and high-energy emission (e.g., Faber & Rasio 2012; Berger 2014; Bartos et al. 2013; Abbott et al. 2017a). Binary neutron star mergers are prime sources of gravitational waves (GWs; e.g., Abadie et al. 2010), which provide information on the neutron star masses and spins (e.g., Veitch et al. 2015). Kilonova/macronova observations of the mergers provide further information on the mass ejected by the disruption of the neutron stars (e.g., Metzger 2017; Abbott et al. 2017b).  \nParticle acceleration and high-energy emission by compact objects are currently not well understood (e.g., M'esz'aros 2013; Kumar & Zhang 2015), and could be deciphered by combined information on the neutron star masses, ejecta mass, and gamma-ray burst (GRB) properties, as expected from multimessenger observations. In particular, the observation of high-energy neutrinos would reveal the hadronic content and dissipation mechanism in relativistic outflows (Waxman & Bahcall 1997). A quasi-diffuse flux of highenergy neutrinos of cosmic origin has been identified by the IceCube observatory (Aartsen et al. 2013; Aartsen et al. 2013). The source population producing these neutrinos is currently not known.  \nOn August 17, 2017, the Advanced LIGO (Aasi et al. 2015) and Advanced Virgo (Acernese et al. 2015) observatories recorded a GW signal, GW170817, from a binary neutron star inspiral (Abbott et al. 2017c). Soon afterwards, Fermi-GBM and INTEGRAL detected a short GRB, GRB170817A, from a consistent location (Goldstein et al. 2017; Savchenko et al. 2017; Abbott et al. 2017a). Subsequently, ultra-violet, optical, and infrared emission was observed from the merger, consistent with kilonova/macronova emission. Optical observations allowed the precise localization of the merger in the galaxy NGC 4993, at equatorial coordinates α (J2000 . 0) = 13 h 09 m 48 . s 085 , δ (J2000 . 0) = -23 · 22 ' 53 . '' 343 (Coulter et al. 2017b,a; Abbott et al. 2017d), and at a distance of ∼ 40 Mpc. At later times, X-ray and radio emissions were also observed (Abbott et al. 2017d), consistent with the expected afterglow of a short GRB at high viewing angles (e.g., Abbott et al. 2017a).  \nHigh-energy neutrino observatories continuously monitor the whole sky or a large fraction of it, making them well suited to study emission from GW sources, even for unknown source locations or for emission prior to or after the GW detection (Adri'an-Mart'ınez et al. 2016a; Albert et al. 2017). It is also possible to rapidly analyze the recorded data and inform other observatories in case of a coincident detection, significantly reducing the source localization uncertainty compared to that provided by GW information alone.  \nIn this Letter we present searches for high-energy neutrinos in coincidence with GW170817/GRB170817A by the three most sensitive high-energy neutrino observatories: (1) the ANTARES neutrino telescope (hereafter ANTARES; Ageron et al. 2011), a ten megaton-scale underwater Cherenkov neutrino detector located at a depth of 2500 m in the Mediterranean Sea; (2) the IceCube Neutrino Observatory (hereafter IceCube; Aartsen et al. 2017), a gigaton-scale neutrino detector installed 1500 m deep in the ice at the geographic South Pole, Antarctica; and (3) the Pierre Auger Observatory (hereafter Auger; Aab et al. 2015), a cosmic-ray air-shower detector consisting of 1660 water-Cherenkov stations spread over an area of ∼ 3000 km 2 . All three detectors joined the low-latency multimessenger follow-up effort of LIGO-Virgo starting with LIGO's second observation run, O2.  \nUpon the identification of the GW signal GW170817, preliminary information on this event was rapidly shared with partner observatories (Abbott et al. 2017d). In response, IceCube (Bartos et al. 2017b,a,c), ANTARES (Ageron et al. 2017a,b), and Auger (Alvarez-Muniz et al. 2017) promptly searched for a neutrino counterpart, and shared their initial results with partner observatories. Subsequently, the three facilities carried out a more in-depth search for a neutrino counterpart using the precise localization of the source.  \nThis Letter is organized as follows. In Section 2, we present the neutrino searches carried out by ANTARES, IceCube, and Auger, as well as the results obtained. In Section 3, we present constraints on processes in the merger that can lead to neutrino emission. We summarize our findings and conclude in Section 4.", '2. SEARCHES AND RESULTS': "Neutrino observatories detect secondary charged particles produced in neutrino interaction with matter. Surface detectors, such as Auger, use arrays of widely-spaced water Cherenkov detectors to observe the air-shower particles created by high-energy neutrinos. In detectors such as ANTARES and IceCube, three-dimensional arrays of optical modules deployed in water or ice detect the Cherenkov radiation from secondary charged particles that travel through the instrumented detector region. For these detectors, the secondary particles can create two main event classes: track-like events from charged-current interactions of muon neutrinos and from a minority of tau neutrino interactions; and showerlike events from all other interactions (neutral-current interactions and charged-current interactions of electron and tau neutrinos). While energy deposition in track-like events can happen over distances of O (km), shower-like events are confined to much smaller regions.  \nFor all detectors, neutrino signals must be identified on top of a persistent background of charged particles produced by  \nFigure 1. Localizations and sensitive sky areas at the time of the GW event in equatorial coordinates: GW 90% credible-level localization (red contour; Abbott et al. 2017c), direction of NGC 4993 (black plus symbol; Coulter et al. 2017a), directions of IceCube's and ANTARES's neutrino candidates within 500 s of the merger (green crosses and blue diamonds, respectively), ANTARES's horizon separating down-going (north of horizon) and up-going (south of horizon) neutrino directions (dashed blue line), and Auger's fields of view for Earth-skimming (darker blue) and down-going (lighter blue) directions. IceCube's up-going and down-going directions are on the northern and southern hemispheres, respectively. The zenith angle of the source at the detection time of the merger was 73 . 8 · for ANTARES, 66 . 6 · for IceCube, and 91 . 9 · for Auger.  \n<!-- image -->  \nthe interaction of cosmic ray particles with the atmosphere above the detectors. This discrimination is done by considering the observed direction and energy of the charged particles. Surface detectors focus on high-energy ( glyph[greaterorsimilar] 10 17 eV) showers created close to the detector by neutrinos from nearhorizontal directions. In-ice and in-water detectors can select well-reconstructed track events from the up-going direction where the Earth is used as a natural shield for the dominant background of penetrating muons from cosmic ray showers. By requiring the neutrino interaction vertex to be contained inside the instrumented volume, or requiring its energy to be sufficiently high to be incompatible with the down-going muon background, even neutrino events originating above the horizon are identifiable. Neutrinos originating from cosmic ray interactions in the atmosphere are also observed and constitute the primary background for up-going and vertexcontained event selections.  \nAll three observatories, ANTARES, IceCube, and Auger, performed searches for neutrino signals in coincidence with the binary neutron star merger event GW170817, each using multiple event selections. Two different time windows were used for the searches. First, we used a ± 500 s time window around the merger to search for neutrinos associated with prompt and extended gamma-ray emission (Baret et al. 2011; Kimura et al. 2017). Second, we searched for neutrinos over a longer 14-day time window following the GW detection, to cover predictions of longer-lived emission processes (e.g., Gao et al. 2013; Fang & Metzger 2017).", '2.1. ANTARES': "The ANTARES neutrino telescope has been continuously operating since 2008. Located deep (2500 m) in the Mediterranean Sea, 40 km from Toulon (France), it is a 10 Mtscale array of photosensors, detecting neutrinos with energies above O (100) GeV.  \nBased on the originally communicated locations of the GWsignal and the GRB detection, high-energy neutrino candidates were initially searched for in the ANTARES online data stream, relying on a fast algorithm which selects only up-going neutrino track candidates (Adri'an-Mart'ınez et al. 2016b). No up-going muon neutrino candidate events were found in a ± 500 s time window centered on the GW event time - for an expected number of atmospheric background events of ∼ 10 -2 during the coincident time window. An extended online search during ± 1 h also resulted in no up-going neutrino coincidences.  \nAs it subsequently became clear, the precise direction of origin of GW170817 in NGC 4993 was above the ANTARES horizon at the detection time of the binary merger (see Fig. 1). Thus, a dedicated analysis looking for down-going muon neutrino candidates in the online ANTARES data stream was also performed. No neutrino counterparts were found in this analysis. The results of these low-latency searches were shared with follow-up partners within a few hours for the up-going search and a few days for the down-going search (Ageron et al. 2017a,b).  \nHere, ANTARES used an updated high-energy neutrino follow up of GW170817 that includes the shower channel. It  \nwas performed with the offline-reconstructed dataset, that incorporates dedicated calibration in terms of positioning, timing and efficiency (Adri'an-Mart'ınez et al. 2012; Aguilar et al. 2011; Aguilar et al. 2007). The analysis has been optimized to increase the sensitivity of the detector and extended to the longer time window of 14 days.  \nThe search for down-going neutrino counterparts to GW170817 was made feasible as the large background affecting this dataset can be drastically suppressed by requiring a time and space coincidence with the GW signal. It was optimized, independently for tracks and showers, such that a directional coincidence with NGC 4993 within the search time window of ± 500 s would have 3 σ significance. Muon neutrino candidates were selected by applying cuts on the estimated angular error and the track quality reconstruction parameter. While ANTARES is sensitive to neutrino events with energy as small as O (100 GeV ) , the energy range corresponding to the 5% -95% quantiles of the neutrino flux for a E -2 signal spectrum is equal to [32 TeV; 22 PeV]. For such a flux, the median angular uncertainty, defined as the median value of the distribution of angles between the reconstructed direction of the event and the true neutrino direction, is equal to 0 . 5 · .  \nShower events were selected by applying a set of cuts primarily devoted to reducing the background rate (Albert et al. 2017). The energy range corresponding to the 5%-95% quantiles of the neutrino flux for a E -2 signal spectrum is equal to [23 TeV; 16 PeV], while the median angular error is 6 · with this set of relaxed cuts.  \nNo events temporally coincident with GW170817 were found. Five background track events (likely atmospheric muons), not compatible with the source position, were detected (see Fig. 1). We used this non-detection to constrain the neutrino fluence (see Fig. 2) which was computed as in Adri'an-Mart'ınez et al. (2016a).  \nThe search over 14 days is restricted to up-going events, but includes all neutrino flavors (tracks and showers). We applied quality cuts optimized for point-source searches which give a median pointing accuracy of 0.4 · and 3 · respectively for track and shower events (Albert et al. 2017). No events spatially coincident with GRB170817A were found.  \nCompared to the upper limits obtained for the short time window of ± 500 s, those limits are significantly less stringent above 1 PeV, where the absorption of neutrinos by the Earth becomes important for up-going events. Below 10 TeV, the constraints computed for the 14-day time window are stricter due to the better acceptance in this energy range for upgoing neutrino candidates compared to down-going events (see Fig. 2).  \n2.2. IceCube  \nIceCube is a cubic-kilometer size neutrino detector (Aartsen et al. 2017) installed in the ice at the geographic South Pole in Antarctica between depths of 1450 m and 2450 m. Detector construction was completed in 2010, and the detector has operated with a ∼ 99% duty cycle since. IceCube searched for neutrino signals from GW170817 using two different event selection techniques.  \nThe first search used an online selection of throughgoing muons, which is used in IceCube's online analyses (Kintscher & the IceCube Collaboration 2016; Aartsen et al. 2016) and follows an event selection similar to that of point source searches (Aartsen et al. 2014). This event selection picks out primarily cosmic-ray-induced background events, with an expectation of 4.0 events in the northern sky (predominantly generated by atmospheric neutrinos) and 2.7 events in the southern sky (predominantly muons generated by high energy cosmic rays interactions in the atmosphere above the detector) per 1000 seconds. For source locations in the southern sky, the sensitivity of the down-going event selection for neutrinos below 1 PeV weakens rapidly with energy due to the rapidly increasing atmospheric muon background at lower energies. Events found by this track selection in the ± 500 s time window are shown in Fig. 1. No events were found to be spatially and temporally correlated with GW170817.  \nA second event selection, described in Wandkowski et al. (2017), was employed offline. This uses the outermost optical sensors of the instrumented volume to veto incoming muon tracks from atmospheric background events. Above 60 TeV, this event selection has the same performance as the high-energy starting event selection (Aartsen et al. 2014). Below this energy, additional veto cuts similar to those described in Aartsen et al. (2015) are applied, in order to maintain a low background level at energies down to a few TeV. Both track- and cascade-like events are retained. The event rate for this selection varies over the sky, but is overall much lower than for the online track selection described above. Between declinations -13 · and -33 · , the mean number of events in a two-week period is 0.4 for tracks and 2.5 for cascades. During the ± 500 s time-window, no events passed this event selection from anywhere in the sky.  \nA combined analysis of the IceCube through-going track selection and the starting-event selection allows upper limits to be placed on the neutrino fluence from GW170817 between the energies of 1 TeV and 1 EeV, shown in Fig. 2. In the central range from 10 TeV to 100 PeV, the upper limit for an E -2 power-law spectral fluence is F ( E ) = 0 . 19 ( E/ GeV) -2 GeV -1 cm -2 .  \nBoth the through-going track selection and the starting event selection were applied to data collected in the 14day period following the time of GW170817. Because of IceCube's location at the South Pole and 99.88% on-time  \nduring the 14-day period, the exposure to the source location is continuous and unvaried. No spatially and temporally coincident events were seen in either selection during this follow-up period. The resulting upper limits are presented in Fig. 2. At most energies these are unchanged from the short time-window. At the lowest energies, where most background events occur, the analysis effectively requires stricter criteria for a coincident event than were required in the short time window; the limits are correspondingly higher. In the central range from 10 TeV to 100 PeV, the upper limit on an E -2 power-law spectral fluence is F ( E ) = 0 . 23 × ( E/ GeV) -2 GeV -1 cm -2 .  \nThe IceCube detector is also sensitive to outbursts of MeV neutrinos via a simultaneous increase in all photomultiplier signal rates. A neutrino burst signal from a galactic corecollapse supernova would be detected with high precision (Abbasi et al. 2011). The detector global dark rate is monitored continuously, the influence of cosmic ray muons is removed and low-level triggers are formed when deviations from the nominal rate exceed pre-defined levels. No alert was triggered during the ± 500 second time-window around the GW candidate. This is consistent with our expectations for cosmic events such as core-collapse supernovae or compact binary mergers that are significantly farther away than Galactic distances.", '2.3. Pierre Auger Observatory': "With the surface detector (SD) of the Pierre Auger Observatory in Malargue, Argentina (Aab et al. 2015), air showers induced by ultra-high energy (UHE) neutrinos can be identified for energies above ∼ 10 17 eV in the more numerous background of UHE cosmic rays (Aab et al. 2015). The SD consists of 1660 water-Cherenkov stations spread over an area of ∼ 3000 km 2 following a triangular arrangement of 1.5 km grid spacing (Aab et al. 2015). The signals produced by the passage of shower particles through the SD detectors are recorded as time traces in 25 ns intervals.  \nCosmic rays interact shortly after entering the atmosphere and induce extensive air showers. For highly inclined directions their electromagnetic component gets absorbed due to the large grammage of atmosphere from the first interaction point to the ground. As a consequence, the shower front at ground level is dominated by muons that induce sharp time traces in the water-Cherenkov stations. On the contrary, showers induced by downward-going neutrinos at large zenith angles can start their development deep in the atmosphere producing traces that spread over longer times. These showers have a considerable fraction of electrons and photons which undergo more interactions than muons in the atmosphere, spreading more in time as they pass through the detector. This is also the case for Earth-skimming showers, mainly induced by tau neutrinos ( ν τ ) that traverse horizon-  \nlly below the Earth's crust, and interact near the exit point inducing a tau lepton that escapes the Earth and decays in flight in the atmosphere above the SD.  \nDedicated and efficient selection criteria based on the different time profiles of the signals detected in showers created by hadronic and neutrino primaries, enable the search for Earth-skimming as well as downward-going neutrino-induced showers (Aab et al. 2015). Deeplystarting downward-going showers initiated by neutrinos of any flavor can be efficiently identified for zenith angles of 60 · < θ < 90 · (Aab et al. 2015). For the Earth-skimming channel typically only ν τ -induced showers with zenith angles 90 · < θ < 95 · can trigger the SD. This is the most sensitive channel to UHE neutrinos, mainly due to the larger grammage and higher density of the target (the Earth) where neutrinos are converted and where tau leptons can travel tens of kilometers (Aab et al. 2015). The angular resolution of the Auger SD for inclined showers is better than 2 . 5 · , improving significantly as the number of triggered stations increases (Bonifazi & Pierre Auger Collaboration 2009).  \nAuger performed a search for UHE neutrinos with its SD in a time window of ± 500 s centered at the merger time of GW170817 (Abbott et al. 2017d), as well as in a 14-day period after it (Murase et al. 2009; Gao et al. 2013; Fang & Metzger 2017).  \nThe sensitivity to UHE neutrinos in Auger is limited to large zenith angles, so that at each instant they can be efficiently detected only from a specific fraction of the sky (Abreu et al. 2012; Aab et al. 2016). Remarkably, the position of the optical counterpart in NGC 4993 (Coulter et al. 2017b,a; Abbott et al. 2017d) is visible from Auger in the field of view of the Earth-skimming channel during the whole ± 500 s window as shown in Fig. 1. In this time period the source of GW170817 transits from θ ∼ 93 . 3 · to θ ∼ 90 . 4 · as seen from the center of the array. The performance of the Auger SD array (regularly monitored every minute) is very stable in the ± 500 s window around GW170817, with an average number of active stations amounting to ∼ 95 . 8 ± 0 . 1 % of the 1660 stations of the SD array.  \nNo inclined showers passing the Earth-skimming selection (neutrino candidates) were found in the time window ± 500 s around the trigger time of GW170817. The estimated number of background events from cosmic rays in a 1000 s period is ∼ 6 . 3 × 10 -7 for the cuts applied in the Earth-skimming analysis (Aab et al. 2015).  \nThe absence of candidates in the ± 500 s window allows us to constrain the fluence in UHE neutrinos from GW170817, assuming they are emitted steadily in this interval and with an E -2 spectrum (Aab et al. 2016). Single-flavor differential limits to the spectral fluence are shown in Fig. 2, in bins of one decade in energy. The sensitivity of the observatory is largest in the energy bin around 10 18 eV. The  \nsingle-flavor upper limit to the spectral fluence is F ( E ) = 0 . 77 ( E/ GeV) -2 GeV -1 cm -2 over the energy range from 10 17 eV to 2 . 5 × 10 19 eV.  \nIn the 14-day search period, as the Earth rotates, the position of NGC 4993 transits through the field of view of the Earth-skimming and downward-going channels. As seen from the Pierre Auger Observatory, the zenith angle of the optical counterpart oscillates daily between θ ∼ 11 · and θ ∼ 121 · . The source is visible in the Earth-skimming channel for ∼ 4% of the day, and in the downward-going channel for ∼ 10 . 5 % ( ∼ 11 . 1 % ) in the zenith angle range 60 · < θ < 75 · ( 75 · < θ < 90 · ). No neutrino candidates were identified in the two-week search period. Singleflavor differential limits to the spectral fluence are shown in Fig. 2. The corresponding upper limit to the spectral fluence is F ( E ) = 25 ( E/ GeV) -2 GeV -1 cm -2 over the same energy interval as for the ± 500 s time window, where the difference is due to the relatively long periods of time when the source of GW170817 is not visible in the inclined directions.", '3. DISCUSSION': "The nature of high-energy emission from the binary merger and its aftermath is not yet clear. We compared the expected spectral fluence for different emission scenarios to our observational upper limits to probe the properties of the merger and its aftermath. Here we briefly outline the relevant information from electromagnetic observations, and present our results for the different emission scenarios.  \nThe merger occurred at a distance of ∼ 40 Mpc, which is the distance of its host galaxy NGC 4993, identified through electromagnetic observations (Coulter et al. 2017b,a; Abbott et al. 2017d). The prompt gamma-ray emission from the source, GRB170817A, had an observed isotropic-equivalent energy of E iso ≈ 4 × 10 46 erg, as recorded by Fermi-GBM (Abbott et al. 2017a). This is orders of magnitude below typical observed short-GRB energies (Berger 2014; Abbott et al. 2017a).  \nPrompt gamma-ray emission in at least some short GRBs is followed by a weaker, extended emission that can last for hundreds of seconds (Norris & Bonnell 2006; Kimura et al. 2017). Fermi-GBM did not detect a temporally extended emission following GRB170817A, placing a constraint of ∼ 2 × 10 46 erg s -1 for a 10 s long emission period over 1 keV10 MeV (Abbott et al. 2017a), significantly below typical luminosities observed for extended emission.  \nThe very faint gamma-ray emission, along with its observed, delayed afterglow, are consistent with a typical short GRB viewed off-axis (Granot et al. 2017; Ioka & Nakamura 2017; Fraija et al. 2017; Troja et al. 2017; Hallinan et al. 2017; Murguia-Berthier et al. 2017; Fong et al. 2017; Margutti et al. 2017; Haggard et al. 2017; Kim et al. 2017; Murguia-Berthier et al. 2017). A GRB is viewed off-axis  \nif its viewing angle θ obs , defined as the angle between the jet axis and the line of sight, is greater than the jet opening half-angle θ j (Granot et al. 2002). The viewing angle inferred from the data is θ obs glyph[greaterorsimilar] 20 · , while typical opening half-angles for short GRBs are within θ j ≈ 3 · -10 · (Berger 2014).  \nGWdata combined with the measured redshift of the host galaxy further provide constraints on θ obs . Here we assume that the jet axis is aligned with the binary's total angular momentum vector. Adopting the Hubble constant from cosmic microwave background measurements by the Planck satellite (Ade et al. 2016), these data are consistent with θ obs = 0 , but also allow for a misalignment of θ obs ≤ 28 · at 90% credible level. Adopting the Hubble constant from Type Ia supernova measurements (Riess et al. 2016) gives a similar result with maximum misalignment of θ obs ≤ 36 · at 90% credible level (LIGO Scientific and Virgo Collaborations et al. 2017).  \nConsidering this off-axis scenario, we examined the expected high-energy neutrino emission from a typical GRB observed at different viewing angles. The most promising neutrino production mechanism from GRBs is related to the extended gamma emission, due to its relatively low Lorentz factor resulting in high meson production efficiency (Kimura et al. 2017). In Fig. 2 we compared our observational constraints with the expected neutrino fluence from the GRB's extended emission. For the on-axis (i.e. θ obs glyph[lessorsimilar] θ j ) spectral fluence F on , we assumed the results of Kimura et al. (2017), rescaled to 40 Mpc. We approximated the observed off-axis spectral fluence, F off ( E ) for these models using F off ( E ) = ηF on ( E/η ) , where the scaling factor η = δ ( θ obs ) /δ (0) accounts for different Doppler factors δ ( θ obs ) = [Γ(1 -β cos( θ obs -θ j ))] -1 (Granot et al. 2002).  \nFor comparison, we also examined the expected neutrino flux associated with the prompt GRB emission (e.g., ]Moharana et al. 2016; Kimura et al. 2017). This emission phase is less favorable for neutrino production than the extended emission. We see in Fig. 2 that prompt emission from a single merger event is unlikely to produce a detected neutrino for the considered observatories, even if viewed on-axis.  \nAnother proposed explanation for the faintness of gammaray emission is the interaction of the GRB jet with ejecta material from the merger (Kasliwal et al. 2017; Gottlieb et al. 2017; Piro & Kollmeier 2017). Energy deposition by the jet into the neutron star ejecta can form a cocoon that expands outwards at mildly relativistic speeds over a wide opening angle. Faint gamma-ray emission is then expected during the breakout of this cocoon from the outer tail of the ejecta (Gottlieb et al. 2017).  \nHigh-energy neutrino production in this scenario may significantly exceed the observed gamma-ray emission as neutrinos can escape through the ejecta even before it becomes transparent to gamma-rays. This scenario resembles that of a  \njet burrowing through the stellar envelope in a core-collapse event (M'esz'aros & Waxman 2001; Razzaque et al. 2003; Bartos et al. 2012; Murase & Ioka 2013). Nevertheless, if the observed gamma-rays come from the outbreak of a wide cocoon, it is less likely that the relativistic jet, which is more narrowly beamed than the cocoon outbreak, also pointed towards Earth.  \nWe further considered an additional neutrino-production mechanism related to ejecta material from the merger. If a rapidly rotating neutron star forms in the merger and does not immediately collapse into a black hole, it can power a relativistic wind with its rotational energy, which may be responsible for the sometimes observed extended emission (Metzger et al. 2008). Optically thick ejecta from the merger can attenuate the gamma-ray flux, while allowing the escape of high-energy neutrinos. Additionally, it may trap some of the wind energy until it expands and becomes transparent. This process can convert some of the wind energy to high-energy particles, producing a long-term neutrino radiation that can last for days (Murase et al. 2009; Gao et al. 2013; Fang & Metzger 2017). The properties of ejecta material around the merger can be characterized from its kilonova/macronova emission.  \nConsidering the possibility that the relative weakness of gamma-ray emission from GRB170817A may be partly due to attenuation by the ejecta, we compared our neutrino constraints to neutrino emission expected for typical GRB parameters. For the prompt and extended emissions, we used the results of Kimura et al. (2017) and compared these to our constraints for the relevant ± 500 s time window. For extended emission we considered source parameters corresponding to both optimistic and moderate scenarios in Table 1 of Kimura et al. (2017). For emission on even longer timescales, we compared our constraints for the 14-day time window with the relevant results of Fang & Metzger (2017), namely emission from approximately 0.3 to 3 days and from 3 to 30 days following the merger. Predictions based on fiducial emission models and neutrino constraints are shown in Fig. 2. We found that our limits would constrain the optimistic extended-emission scenario for a typical GRB at ∼ 40 Mpc, viewed at zero viewing angle.", '4. CONCLUSION': 'We searched for high-energy neutrinos from the first binary neutron star merger detected through GWs, GW170817, in the energy band of [ ∼ 10 11 eV, ∼ 10 20 eV] using the ANTARES, IceCube, and Pierre Auger Observatories, as well as for MeV neutrinos with IceCube. This marks an unprecedented joint effort of experiments sensitive to high-energy neutrinos. We have observed no significant neutrino counterpart within a ± 500 s window, nor in the subsequent 14 days.', 'GW170817 Neutrino limits (fluence per flavor: x + x )': 'E/GeV  \nFigure 2. Upper limits (at 90 % confidence level) on the neutrino spectral fluence from GW170817 during a ± 500 s window centered on the GW trigger time (top panel), and a 14-day window following the GW trigger (bottom panel). For each experiment, limits are calculated separately for each energy decade, assuming a spectral fluence F ( E ) = F up × [ E/ GeV] -2 in that decade only. Also shown are predictions by neutrino emission models. In the upper plot, models from Kimura et al. (2017) for both extended emission (EE) and prompt emission are scaled to a distance of 40 Mpc, and shown for the case of on-axis viewing angle ( θ obs glyph[lessorsimilar] θ j ) and selected off-axis angles to indicate the dependence on this parameter. The shown off-axis angles are measured in excess of the jet opening half angle θ j . GW data and the redshift of the host-galaxy constrain the viewing angle to θ obs ∈ [0 · , 36 · ] (see Section 3). In the lower plot, models from Fang & Metzger (2017) are scaled to a distance of 40 Mpc. All fluences are shown as the per flavor sum of neutrino and anti-neutrino fluence, assuming equal fluence in all flavors, as expected for standard neutrino oscillation parameters.  \n<!-- image -->  \nThe three detectors complement each other in the energy bands in which they are most sensitive (see Fig. 2).  \nThis non-detection is consistent with our expectations from a typical GRB observed off-axis, or with a low-luminosity GRB. Optimistic scenarios for on-axis gamma-attenuated emission are constrained by the present non-detection.  \nWhile the location of this source was nearly ideal for Auger, it was well above the horizon for IceCube and ANTARES for prompt observations. This limited the sensitivity of the latter two detectors, particularly below ∼ 100 TeV.  \nFor source locations near, or below the horizon, a factor of ∼ 10 increase in fluence sensitivity to prompt emission from an E -2 neutrino spectrum is expected.  \nWith the discovery of a nearby binary neutron star merger, the ongoing enhancement of detector sensitivity (Abbott et al. 2016) and the growing network of GW detectors (Aso et al. 2013; Iyer et al. 2011), we can expect that several binary neutron star mergers will be observed in the near future. Not only will this allow stacking analyses of neutrino emission, but it will also bring about sources with favorable orientation and direction.  \nThe ANTARES, IceCube, and Pierre Auger Collaborations are planning to continue the rapid search for neutrino candidates from identified GW sources. A coincident neutrino, with a typical position uncertainty of ∼ 1 deg 2 could significantly improve the fast localization of joint events compared to the GW-only case. In addition, the first joint GW and highenergy neutrino discovery might thereby be known to the wider astronomy community within minutes after the event, opening a rich field of multimessenger astronomy with particle, electromagnetic, and gravitational waves combined.', 'ACKNOWLEDGMENTS': "(ANTARES) The ANTARES authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat 'a l''energie atomique et aux 'energies alternatives (CEA), Commission Europ'eenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cit'e (ANR-10LABX-0023 and ANR-11-IDEX-0005-02), Labex OCEVU (ANR-11-LABX-0060) and the A*MIDEX project (ANR11-IDEX-0001-02), R'egion ˆ Ile-de-France (DIM-ACAV), R'egion Alsace (contrat CPER), R'egion Provence-AlpesCˆote d'Azur, D'epartement du Var and Ville de La Seyne-surMer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Econom'ıa y Competitividad (MINECO): Plan Estatal de Investigaci'on (refs. FPA2015-65150-C3-1-P, 2-P and -3-P, (MINECO/FEDER)), Severo Ochoa Centre of Excellence and MultiDark Consolider (MINECO), and Prometeo and Grisol'ıa programs (Generalitat Valenciana), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities.  \n(IceCube) The IceCube collaboration acknowledges the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin - Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Initiative and Networking Fund of the Helmholtz Association, Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Villum Fonden, Danish National Research Foundation (DNRF), Denmark.  \n(Auger) The successful installation, commissioning, and operation of the Pierre Auger Observatory would not have been possible without the strong commitment and effort from the technical and administrative staff in Malargue. We are very grateful to the following agencies and organizations for financial support:  \nArgentina - Comisi'on Nacional de Energ'ıa At'omica; Agencia Nacional de Promoci'on Cient'ıfica y Tecnol'ogica (ANPCyT); Consejo Nacional de Investigaciones Cient'ıficas y T'ecnicas (CONICET); Gobierno de la Provincia de Mendoza; Municipalidad de Malargue; NDM Holdings and Valle Las Le˜nas; in gratitude for their continuing cooperation over land access; Australia - the Australian Research Council; Brazil - Conselho Nacional de Desenvolvimento Cient'ıfico e Tecnol'ogico (CNPq); Financiadora de Estudos e Projetos (FINEP); Fundac¸˜ao de Amparo 'a Pesquisa do Estado de Rio de Janeiro (FAPERJ); S˜ao Paulo Research Foundation (FAPESP) Grants No. 2010/073596 and No. 1999/05404-3; Minist'erio da Ciˆencia, Tecnologia, Inovac¸ ˜oes e Comunicac¸ ˜oes (MCTIC); Czech Republic - Grant No. MSMT CR LG15014, LO1305, LM2015038 and CZ.02.1.01/0.0/0.0/16 013/0001402; France - Centre de Calcul IN2P3/CNRS; Centre National de la Recherche Scientifique (CNRS); Conseil R'egional Ile-de-  \nFrance; D'epartement Physique Nucl'eaire et Corpusculaire (PNC-IN2P3/CNRS); D'epartement Sciences de l'Univers (SDU-INSU/CNRS); Institut Lagrange de Paris (ILP) Grant No. LABEX ANR-10-LABX-63 within the Investissements d'Avenir Programme Grant No. ANR-11-IDEX0004-02; Germany - Bundesministerium fur Bildung und Forschung (BMBF); Deutsche Forschungsgemeinschaft (DFG); Finanzministerium Baden-Wurttemberg; Helmholtz Alliance for Astroparticle Physics (HAP); HelmholtzGemeinschaft Deutscher Forschungszentren (HGF); Ministerium fur Innovation, Wissenschaft und Forschung des Landes Nordrhein-Westfalen; Ministerium fur Wissenschaft, Forschung und Kunst des Landes Baden-Wurttemberg; Italy - Istituto Nazionale di Fisica Nucleare (INFN); Istituto Nazionale di Astrofisica (INAF); Ministero dell'Istruzione, dell'Universit'a e della Ricerca (MIUR); CETEMPS Center of Excellence; Ministero degli Affari Esteri (MAE); Mexico - Consejo Nacional de Ciencia y Tecnolog'ıa (CONACYT) No. 167733; Universidad Nacional Aut'onoma de M'exico (UNAM); PAPIIT DGAPA-UNAM; The Netherlands - Ministerie van Onderwijs, Cultuur en Wetenschap; Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO); Stichting voor Fundamenteel Onderzoek der Materie (FOM); Poland - National Centre for Research and Development, Grants No. ERA-NET-ASPERA/01/11 and No. ERANET-ASPERA/02/11; National Science Centre, Grants No. 2013/08/M/ST9/00322, No. 2013/08/M/ST9/00728 and No. HARMONIA 5-2013/10/M/ST9/00062, UMO2016/22/M/ST9/00198; Portugal - Portuguese national funds and FEDER funds within Programa Operacional Factores de Competitividade through Fundac¸˜ao para a Ciˆencia e a Tecnologia (COMPETE); Romania - Romanian Authority for Scientific Research ANCS; CNDI-UEFISCDI partnership projects Grants No. 20/2012 and No. 194/2012 and PN 16 42 01 02; Slovenia - Slovenian Research Agency; Spain - Comunidad de Madrid; Fondo Europeo de Desarrollo Regional (FEDER) funds; Ministerio de Econom'ıa y Competitividad; Xunta de Galicia; European Community 7th Framework Program Grant No. FP7-PEOPLE-2012-IEF328826; USA - Department of Energy, Contracts No. DEAC02-07CH11359, No. DE-FR02-04ER41300, No. DEFG02-99ER41107 and No. DE-SC0011689; National Science Foundation, Grant No. 0450696; The Grainger Foundation; Marie Curie-IRSES/EPLANET; European Particle Physics Latin American Network; European Union 7th Framework Program, Grant No. PIRSES-2009-GA-246806; European Union's Horizon 2020 research and innovation programme (Grant No. 646623); and UNESCO.  \n(NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigaci'on, the Vicepresid'encia i Conselleria d'Innovaci'o, Recerca i Turisme and the Conselleria d'Educaci'o i Universitat del Govern de les Illes Balears, the Conselleria d'Educaci'o, Investigaci'o, Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research, Development and Innovation Office Hungary (NKFI), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for provision of computational resources.  \n(LIGO and Virgo) The authors gratefully acknowledge the support of the United States National Science Foundation  \nSavchenko, V., et al. 2017, Tech. rep. Troja, E., Piro, L., van Eerten, H., et al. 2017, Nature, doi:10.1038/nature24290 Veitch, J., et al. 2015, Phys. Rev. D, 91, 042003  \nWandkowski, N., Weaver, C., & the IceCube Collaboration. 2017, PoS(ICRC2017)976, arXiv:1710.01191  \nWaxman, E., & Bahcall, J. 1997, Phys. Rev. Lett., 78, 2292"}