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For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of high-energy astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos, since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields. In this paper, we present three different approaches for correlating the arrival directions of neutrinos with the arrival directions of UHECRs. The neutrino data are provided by the IceCube Neutrino Observatory and ANTARES, while the UHECR data with energies above similar to 50 EeV are provided by the Pierre Auger Observatory and the Telescope Array. All experiments provide increased statistics and improved reconstructions with respect to our previous results reported in 2015. The first analysis uses a high-statistics neutrino sample optimized for point-source searches to search for excesses of neutrino clustering in the vicinity of UHECR directions. The second analysis searches for an excess of UHECRs in the direction of the highest-energy neutrinos. The third analysis searches for an excess of pairs of UHECRs and highest-energy neutrinos on different angular scales. None of the analyses have found a significant excess, and previously reported overfluctuations are reduced in significance. Based on these results, we further constrain the neutrino flux spatially correlated with UHECRs.
A. Albert, S. Alves, M. Andr??, M. Anghinolfi, M. A., S. Ardid, et al. (2022). Search for Spatial Correlations of Neutrinos with Ultra-high-energy Cosmic Rays. THE ASTROPHYSICAL JOURNAL, 934(2), 1-21 [10.3847/1538-4357/ac6def].
Search for Spatial Correlations of Neutrinos with Ultra-high-energy Cosmic Rays
A. Albert;S. Alves;M. Andr??;M. Anghinolfi;M. A.;S. Ardid;J. -J. Aubert;J. Aublin;B. Baret;S. Basa;B. Belhorma;M. Bendahman;V. Bertin;S. Biagi;M. Bissinger;J. Boumaaza;M. Bouta;M. C. Bouwhuis;H. Br??nza??;R. Bruijn;J. Brunner;J. Busto;B. Caiffi;D. Calvo;A. Capone;L. Caramete;J. Carr;V. Carretero;S. Celli;M. Chabab;T. N. Chau;R. Cherkaoui El Moursli;T. Chiarusi;M. Circella;A. Coleiro;R. Coniglione;P. Coyle;A. Creusot;A. F. D??az;C. Distefano;I. Di Palma;A. Domi;C. Donzaud;D. Dornic;D. Drouhin;T. Eberl;T. van Eeden;D. van Eijk;N. El Khayati;A. Enzenh??fer;P. Fermani;G. Ferrara;F. Filippini;L. Fusco;Y. Gatelet;P. Gay;H. Glotin;R. Gozzini;R. Gracia Ruiz;K. Graf;C. Guidi;S. Hallmann;H. van Haren;A. J. Heijboer;Y. Hello;J. J. Hern??ndez-Rey;J. H??ssl;J. Hofest??dt;F. Huang;G. Illuminati;C. W. James;B. Jisse-Jung;M. De Jong;P. de Jong;M. Kadler;O. Kalekin;U. Katz;N. R. Khan-Chowdhury;A. Kouchner;I. Kreykenbohm;V. Kulikovskiy;R. Lahmann;R. Le Breton;S. LeStum;D. Lef??vre;E. Leonora;G. Levi;D. Lopez-Coto;S. Loucatos;L. Maderer;J. Manczak;M. Marcelin;A. Margiotta;A. Marinelli;J. A. Mart??nez-Mora;B. Martino;K. Melis;P. Migliozzi;A. Moussa;R. Muller;L. Nauta;S. Navas;E. Nezri;B. ??. Fearraigh;A. P??un;G. E. P??v??la??;C. Pellegrino;M. Perrin-Terrin;V. Pestel;P. Piattelli;C. Pieterse;C. Poir??;V. Popa;T. Pradier;N. Randazzo;D. Real;S. Reck;G. Riccobene;A. Romanov;A. S??nchez-Losa;F. Salesa Greus;D. F. E. Samtleben;M. Sanguineti;P. Sapienza;J. Schnabel;J. Schumann;F. Sch??ssler;J. Seneca;M. Spurio;Th. Stolarczyk;M. Taiuti;Y. Tayalati;S. J. Tingay;B. Vallage;V. Van Elewyck;F. Versari;S. Viola;D. Vivolo;J. Wilms;S. Zavatarelli;A. Zegarelli;J. D. Zornoza;J. Z????iga;R. Abbasi;M. Ackermann;J. Adams;J. A. Aguilar;M. Ahlers;M. Ahrens;J. M. Alameddine;C. Alispach;A. A. Alves Jr.;N. M. Amin;K. Andeen;T. Anderson;G. Anton;C. Arg??elles;Y. Ashida;S. Axani;X. Bai;A. Balagopal V.;A. Barbano;S. W. Barwick;B. Bastian;V. Basu;S. Baur;R. Bay;J. J. Beatty;K. -H. Becker;J. Becker Tjus;C. Bellenghi;S. BenZvi;D. Berley;E. Bernardini;D. Z. Besson;G. Binder;D. Bindig;E. Blaufuss;S. Blot;M. Boddenberg;F. Bontempo;J. Borowka;S. B??ser;O. Botner;J. B??ttcher;E. Bourbeau;F. Bradascio;J. Braun;B. Brinson;S. Bron;J. Brostean-Kaiser;S. Browne;A. Burgman;R. T. Burley;R. S. Busse;M. A. Campana;E. G. Carnie-Bronca;C. Chen;Z. Chen;D. Chirkin;K. Choi;B. A. Clark;K. Clark;L. Classen;G. H. Collin;J. M. Conrad;P. Coppin;P. Correa;D. F. Cowen;R. Cross;C. Dappen;P. Dave;C. De Clercq;J. J. DeLaunay;D. Delgado L??pez;H. Dembinski;K. Deoskar;A. Desai;P. Desiati;K. D. de Vries;G. de Wasseige;M. de With;T. DeYoung;A. Diaz;J. C. D??az-V??lez;M. Dittmer;H. Dujmovic;M. Dunkman;M. A. DuVernois;E. Dvorak;T. Ehrhardt;P. Eller;H. Erpenbeck;J. Evans;P. A. Evenson;K. L. Fan;A. R. Fazely;A. Fedynitch;N. Feigl;S. Fiedlschuster;A. T. Fienberg;K. Filimonov;C. Finley;L. Fischer;D. Fox;A. Franckowiak;E. Friedman;A. Fritz;P. F??rst;T. K. Gaisser;J. Gallagher;E. Ganster;A. Garcia;S. Garrappa;L. Gerhardt;A. Ghadimi;C. Glaser;T. Glauch;T. Gl??senkamp;J. G. Gonzalez;S. Goswami;D. Grant;T. Gr??goire;S. Griswold;C. G??nther;P. Gutjahr;C. Haack;A. Hallgren;R. Halliday;L. Halve;F. Halzen;M. Ha Minh;K. Hanson;J. Hardin;A. A. Harnisch;A. Haungs;D. Hebecker;K. Helbing;F. Henningsen;E. C. Hettinger;S. Hickford;J. Hignight;C. Hill;G. C. Hill;K. D. Hoffman;R. Hoffmann;B. Hokanson-Fasig;K. Hoshina;M. Huber;T. Huber;K. Hultqvist;M. H??nnefeld;R. Hussain;K. Hymon;S. In;N. Iovine;A. Ishihara;M. Jansson;G. S. Japaridze;M. Jeong;M. Jin;B. J. P. Jones;D. Kang;W. Kang;X. Kang;A. Kappes;D. Kappesser;L. Kardum;T. Karg;M. Karl;A. Karle;M. Kauer;M. Kellermann;J. L. Kelley;A. Kheirandish;K. Kin;T. Kintscher;J. Kiryluk;S. R. Klein;R. Koirala;H. Kolanoski;T. Kontrimas;L. K??pke;C. Kopper;S. Kopper;D. J. Koskinen;P. Koundal;M. Kovacevich;M. Kowalski;T. Kozynets;E. Kun;N. Kurahashi;N. Lad;C. Lagunas Gualda;J. L. Lanfranchi;M. J. Larson;F. Lauber;J. P. Lazar;J. W. Lee;K. Leonard;A. Leszczy??ska;Y. Li;M. Lincetto;Q. R. Liu;M. Liubarska;E. Lohfink;C. J. Lozano Mariscal;F. Lucarelli;A. Ludwig;W. Luszczak;Y. Lyu;W. Y. Ma;J. Madsen;K. B. M. Mahn;Y. Makino;S. Mancina;I. Martinez-Soler;R. Maruyama;K. Mase;T. McElroy;F. McNally;J. V. Mead;K. Meagher;S. Mechbal;A. Medina;M. Meier;S. Meighen-Berger;J. Micallef;D. Mockler;T. Montaruli;R. W. Moore;R. Morse;M. Moulai;R. Naab;R. Nagai;U. Naumann;J. Necker;L. V. Nguy???n;H. Niederhausen;M. U. Nisa;S. C. Nowicki;A. Obertacke Pollmann;M. Oehler;B. Oeyen;A. Olivas;E. O???Sullivan;H. Pandya;D. V. Pankova;N. Park;G. K. Parker;E. N. Paudel;L. Paul;C. P??rez de los Heros;L. Peters;J. Peterson;S. Philippen;S. Pieper;M. Pittermann;A. Pizzuto;M. Plum;Y. Popovych;A. Porcelli;M. Prado Rodriguez;P. B. Price;B. Pries;G. T. Przybylski;C. Raab;J. Rack-Helleis;A. Raissi;M. Rameez;K. Rawlins;I. C. Rea;A. Rehman;P. Reichherzer;R. Reimann;G. Renzi;E. Resconi;S. Reusch;W. Rhode;M. Richman;B. Riedel;E. J. Roberts;S. Robertson;G. Roellinghoff;M. Rongen;C. Rott;T. Ruhe;D. 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Sciutto;M. Scornavacche;A. Segreto;S. Sehgal;R. C. Shellard;G. Sigl;G. Silli;O. Sima;R. Smau;R. ??m??da;P. Sommers;J. F. Soriano;R. Squartini;M. Stadelmaier;D. Stanca;S. Stani??;J. Stasielak;P. Stassi;A. Streich;M. Su??rez-Dur??n;T. Sudholz;T. Suomij??rvi;A. D. Supanitsky;Z. Szadkowski;A. Tapia;C. Taricco;C. Timmermans;O. Tkachenko;P. Tobiska;C. J. Todero Peixoto;B. Tom??;Z. Torr??s;A. Travaini;P. Travnicek;C. Trimarelli;M. Tueros;R. Ulrich;M. Unger;L. Vaclavek;M. Vacula;J. F. Vald??s Galicia;L. Valore;E. Varela;A. V??squez-Ram??rez;D. Veberi??;C. Ventura;I. D. Vergara Quispe;V. Verzi;J. Vicha;J. Vink;S. Vorobiov;H. Wahlberg;C. Watanabe;A. A. Watson;L. Wiencke;H. Wilczy??ski;D. Wittkowski;B. Wundheiler;A. Yushkov;O. Zapparrata;E. Zas;D. Zavrtanik;M. Zavrtanik;L. Zehrer;T. Abu-Zayyad;M. Allen;Y. Arai;R. Arimura;E. Barcikowski;J. W. Belz;D. R. Bergman;S. A. Blake;I. Buckland;R. Cady;B. G. Cheon;J. Chiba;M. Chikawa;K. Fujisue;K. Fujita;R. Fujiwara;M. Fukushima;R. Fukushima;G. Furlich;N. Globus;R. Gonzalez;W. Hanlon;M. Hayashi;N. Hayashida;H. He;K. Hibino;R. Higuchi;K. Honda;D. Ikeda;T. Inadomi;N. Inoue;T. Ishii;H. Ito;D. Ivanov;H. Iwakura;A. Iwasaki;H. M. Jeong;S. Jeong;C. C. H. Jui;K. Kadota;F. Kakimoto;O. Kalashev;K. Kasahara;S. Kasami;S. Kawakami;S. Kawana;K. Kawata;I. Kharuk;E. Kido;H. B. Kim;J. H. Kim;J. H. Kim;S. W. Kim;Y. Kimura;S. Kishigami;Y. Kubota;S. Kurisu;V. Kuzmin;M. Kuznetsov;Y. J. Kwon;K. H. Lee;B. Lubsandorzhiev;K. Machida;H. Matsumiya;T. Matsuyama;J. N. Matthews;R. Mayta;M. Minamino;K. Mukai;I. Myers;S. Nagataki;K. Nakai;R. Nakamura;T. Nakamura;T. Nakamura;Y. Nakamura;A. Nakazawa;E. Nishio;T. Nonaka;H. Oda;S. Ogio;M. Ohnishi;H. Ohoka;Y. Oku;T. Okuda;Y. Omura;M. Ono;R. Onogi;A. Oshima;S. Ozawa;I. H. Park;M. Potts;M. S. Pshirkov;J. Remington;D. C. Rodriguez;G. I. Rubtsov;D. Ryu;H. Sagawa;R. Sahara;Y. Saito;N. Sakaki;T. Sako;N. Sakurai;K. Sano;K. Sato;T. Seki;K. Sekino;P. D. Shah;Y. Shibasaki;F. Shibata;N. Shibata;T. Shibata;H. Shimodaira;B. K. Shin;H. S. Shin;D. Shinto;J. D. Smith;P. Sokolsky;N. Sone;B. T. Stokes;T. A. Stroman;Y. Takagi;Y. Takahashi;M. Takamura;M. Takeda;R. Takeishi;A. Taketa;M. Takita;Y. Tameda;H. Tanaka;K. Tanaka;M. Tanaka;Y. Tanoue;S. B. Thomas;G. B. Thomson;P. Tinyakov;I. Tkachev;H. Tokuno;T. Tomida;S. Troitsky;R. Tsuda;Y. Tsunesada;Y. Uchihori;S. Udo;T. Uehama;F. Urban;D. Warren;T. Wong;M. Yamamoto;K. Yamazaki;K. Yashiro;F. Yoshida;Y. Yoshioka;Y. Zhezher;Z. Zundel
2022
Abstract
For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of high-energy astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos, since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields. In this paper, we present three different approaches for correlating the arrival directions of neutrinos with the arrival directions of UHECRs. The neutrino data are provided by the IceCube Neutrino Observatory and ANTARES, while the UHECR data with energies above similar to 50 EeV are provided by the Pierre Auger Observatory and the Telescope Array. All experiments provide increased statistics and improved reconstructions with respect to our previous results reported in 2015. The first analysis uses a high-statistics neutrino sample optimized for point-source searches to search for excesses of neutrino clustering in the vicinity of UHECR directions. The second analysis searches for an excess of UHECRs in the direction of the highest-energy neutrinos. The third analysis searches for an excess of pairs of UHECRs and highest-energy neutrinos on different angular scales. None of the analyses have found a significant excess, and previously reported overfluctuations are reduced in significance. Based on these results, we further constrain the neutrino flux spatially correlated with UHECRs.
A. Albert, S. Alves, M. Andr??, M. Anghinolfi, M. A., S. Ardid, et al. (2022). Search for Spatial Correlations of Neutrinos with Ultra-high-energy Cosmic Rays. THE ASTROPHYSICAL JOURNAL, 934(2), 1-21 [10.3847/1538-4357/ac6def].
A. Albert; S. Alves; M. Andr??; M. Anghinolfi; M. A.; S. Ardid; J.-J. Aubert; J. Aublin; B. Baret; S. Basa; B. Belhorma; M. Bendahman; V. Bertin; S. B...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/898102
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
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