6533b851fe1ef96bd12a8e85
RESEARCH PRODUCT
Search for magnetically-induced signatures in the arrival directions of ultra-high-energy cosmic rays measured at the Pierre Auger Observatory
Maris I. C.Pekala J.Smda R.Supk J.Aab A.Abreu P.Aglietta M.Albury J. M.Allekotte I.Almela A.Castillo J. A.Alvarez-muniz J.Batista R. A.Anastasi G. A.Anchordoqui L.Andrada B.Andringa S.Aramo C.Ferreira P. R. A.Asorey H.Assis P.Avila G.Badescu A. M.Bakalova A.Balaceanu A.Barbato F.Luz R. J. B.Becker K. H.Bellido J. A.Berat C.Bertaina M. E.Bertou X.Biermann P. L.Bister T.Biteau J.Blanco A.Blazek J.Bleve C.Bohacova M.Boncioli D.Bonifazi C.Arbeletche L. B.Borodai N.Botti A. M.Brack J.Bretz T.Briechle F. L.Buchholz P.Bueno A.Buitink S.Buscemi M.Caballero-mora K. S.Caccianiga L.Calcagni L.Cancio A.Canfora F.Caracas I.Carceller J. M.Caruso R.Castellina A.Catalani F.Cataldi G.Cazon L.Cerda M.Chinellato J. A.Choi K.Chudoba J.Chytka L.Clay R. W.Cerutti A. C. C.Colalillo R.Coleman A.Coluccia M. R.Conceicao R.Condorelli A.Consolati G.Contreras F.Convenga F.Covault C. E.Dasso S.Daumiller K.Dawson B. R.Day J. A.De Almeida R. M.De Jesus J.De Jong S. J.Mauro G. D.Neto J. R. T. D. M.Mitri I. D.De Oliveira J.Franco D. D. O.De Souza V.Debatin J.Rio M. D.Deligny O.Dhital N.Matteo A. D.Castro M. L. D.Dobrigkeit C.D'olivo J. C.Dorosti Q.Anjos R. C. D.Dova M. T.Ebr J.Engel R.Epicoco I.Erdmann M.Escobar C. O.Etchegoyen A.Falcke H.Farmer J.Farrar G.Fauth A. C.Fazzini N.Feldbusch F.Fenu F.Fick B.Figueira J. M.Filipcic A.Fodran T.Freire M. M.Fujii T.Fuster A.Galea C.Galelli C.Garcia B.Vegas A. L. G.Gemmeke H.Gesualdi F.Gherghel-lascu A.Ghia P. L.Giaccari U.Giammarchi M.Giller M.Glombitza J.Gobbi F.Golup G.Berisso M. G.Vitale P. F. G.Gongora J. P.Gonzalez N.Goos I.Gora D.Gorgi A.Gottowik M.Grubb T. D.Guarino F.Guedes G. P.Guido E.Hahn S.Halliday R.Hampel M. R.Hansen P.Harari D.Harvey V. M.Haungs A.Hebbeker T.Heck D.Hill G. C.Hojvat C.Horandel J. R.Horvath P.Hrabovsky M.Huege T.Hulsman J.Insolia A.Isar P. G.Johnsen J. A.Jurysek J.Kaapa A.Kampert K. H.Keilhauer B.Kemp J.Klages H. O.Kleifges M.Kleinfeller J.Kopke M.Mezek G. K.Lago B. L.Lahurd D.Lang R. G.De Oliveira M. A. L.Lenok V.Letessier-selvon A.Lhenry-yvon I.Presti D. L.Lopes L.Lopez R.Lorek R.Luce Q.Lucero A.Payeras A. M.Malacari M.Mancarella G.Mandat D.Manning B. C.Manshanden J.Mantsch P.Marafico S.Mariazzi A. G.Maris I. C.Marsella G.Martello D.Martinez H.Bravo O. M.Mastrodicasa M.Mathes H. J.Matthews J.Matthiae G.Mayotte E.Mazur P. O.Medina-tanco G.Melo D.Menshikov A.Merenda K. -D.Michal S.Micheletti M. I.Miramonti L.Mockler D.Mollerach S.Montanet F.Morello C.Mostafa M.Muller A. L.Muller M. A.Mulrey K.Mussa R.Muzio M.Namasaka W. M.Nellen L.Niculescu-oglinzanu M.Niechciol M.Nitz D.Nosek D.Novotny V.Nozka L.Nucita A.Nunez L. A.Palatka M.Pallotta J.Panetta M. P.Papenbreer P.Parente G.Parra A.Pech M.Pedreira F.Pekala J.Pelayo R.Pena-rodriguez J.Armand J. P.Perlin M.Perrone L.Peters C.Petrera S.Pierog T.Pimenta M.Pirronello V.Platino M.Pont B.Pothast M.Privitera P.Prouza M.Puyleart A.Querchfeld S.Rautenberg J.Ravignani D.Reininghaus M.Ridky J.Riehn F.Risse M.Ristori P.Rizi V.De Carvalho W. R.Rojo J. R.Roncoroni M. J.Roth M.Roulet E.Rovero A. C.Ruehl P.Saffi S. J.Saftoiu A.Salamida F.Salazar H.Salina G.Gomez J. D. S.Sanchez F.Santos E. M.Santos E.Sarazin F.Sarmento R.Sarmiento-cano C.Sato R.Savina P.Schafer C.Scherini V.Schieler H.Schimassek M.Schimp M.Schluter F.Schmidt D.Scholten O.Schovanek P.Schroder F. G.Schroder S.Sciutto S. J.Scornavacche M.Shellard R. C.Sigl G.Silli G.Sima O.Smida R.Sommers P.Soriano J. F.Souchard J.Squartini R.Stadelmaier M.Stanca D.Stanic S.Stasielak J.Stassi P.Streich A.Suarez-duran M.Sudholz T.Suomijarvi T.Supanitsky A. D.Supik J.Szadkowski Z.Taboada A.Tapia A.Timmermans C.Tobiska P.Peixoto C. J. T.Tome B.Elipe G. T.Travaini A.Travnicek P.Trimarelli C.Trini M.Tueros M.Ulrich R.Unger M.Urban M.Vaclavek L.Vacula M.Galicia J. F. V.Valino I.Valore L.Vliet A. V.Varela E.Cardenas B. V.Vasquez-ramirez A.Veberic D.Ventura C.Quispe I. D. V.Verzi V.Vicha J.Villasenor L.Vink J.Vorobiov S.Wahlberg H.Watson A. A.Weber M.Weindl A.Wiencke L.Wilczynski H.Winchen T.Wirtz M.Wittkowski D.Wundheiler B.Yushkov A.Zapparrata O.Zas E.Zavrtanik D.Zavrtanik M.Zehrer L.Zepeda A.Ziolkowski M.Zuccarello F.subject
electric [charge]AstronomydeflectionThrustmagnetic fieldAstrophysics01 natural sciencesmass spectrumhelium: nucleusbenchmarksurface [detector]Cosmic ray experimentsUltra-high-energy cosmic ray010303 astronomy & astrophysicsPhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)astro-ph.HEAstrophysics::Instrumentation and Methods for AstrophysicsCosmic ray experiments; Ultra high energy cosmic raysAugerobservatoryacceleration [cosmic radiation]Astrophysics - High Energy Astrophysical PhenomenasignaturePrincipal axis theoremActive galactic nucleusCherenkov counter: waterAstrophysics::High Energy Astrophysical PhenomenaUHE [cosmic radiation]energy spectrumFOS: Physical sciencesnucleus [helium]Cosmic rayElectric chargeCosmic ray experimentGLASTdetector: fluorescence0103 physical sciencesddc:530thrustcosmic radiation: UHEHigh Energy Physicscosmic radiation: accelerationAGNAstrophysiquePierre Auger Observatoryfluorescence [detector]010308 nuclear & particles physicsdetector: surfacecharge: electricwater [Cherenkov counter]Astronomy and AstrophysicsUltra high energy cosmic raysAstronomiesensitivityGalaxycoherencefluxgamma raymultipletcorrelationExperimental High Energy Physicsgalaxy[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]RAIOS CÓSMICOSdescription
We search for signals of magnetically-induced effects in the arrival directions of ultra-high-energy cosmic rays detected at the Pierre Auger Observatory. We apply two different methods. One is a search for sets of events that show a correlation between their arrival direction and the inverse of their energy, which would be expected if they come from the same point-like source, they have the same electric charge and their deflection is relatively small and coherent. We refer to these sets of events as "multiplets". The second method, called "thrust", is a principal axis analysis aimed to detect the elongated patterns in a region of interest. We study the sensitivity of both methods using a benchmark simulation and we apply them to data in two different searches. The first search is done assuming as source candidates a list of nearby active galactic nuclei and starburst galaxies. The second is an all-sky blind search. We report the results and we find no statistically significant features. We discuss the compatibility of these results with the indications on the mass composition inferred from data of the Pierre Auger Observatory.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2020-06-01 |