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Update on the searches for anisotropies in UHECR arrival directions with the Pierre Auger Observatory and the Telescope Array

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Date
2024
Author
Caccianiga L.; Anchordoqui L.; Bianciotto M.; Biteau J.; Deligny O.; Deval L.; di Matteo A.; Giaccari U.G.; Golup G.; Kim J.; Kuznetsov M.; Mariani F.M.; Rubtsov G.; Tinyakov P.; Urban F.; Abdul Halim A.; Abreu P.; Aglietta M.; Allekotte I.; Almeida Cheminant K.; Almela A.; Aloisio R.; Alvarez-Muñiz J.; Ammerman Yebra J.; Anastasi G.A.; Anchordoqui L.; Andrada B.; Andringa S.; Aramo C.; Araújo Ferreira P.R.; Arnone E.; Arteaga Velázquez J.C.; Asorey H.; Assis P.; Avila G.; Avocone E.; Badescu A.M.; Bakalova A.; Balaceanu A.; Barbato F.; Bartz Mocellin A.; Bellido J.A.; Berat C.; Bertaina M.E.; Bhatta G.; Bianciotto M.; Biermann P.L.; Binet V.; Bismark K.; Bister T.; Biteau J.; Blazek J.; Bleve C.; Blümer J.; Bohácová M.; Boncioli D.; Bonifazi C.; Bonneau Arbeletche L.; Borodai N.; Brack J.; Brichetto Orchera P.G.; Briechle F.L.; Bueno A.; Buitink S.; Buscemi M.; Büsken M.; Bwembya A.; Caballero-Mora K.S.; Cabana-Freire S.; Caccianiga L.; Caracas I.; Caruso R.; Castellina A.; Catalani F.; Cataldi G.; Cazon L.; Cerda M.; Cermenati A.; Chinellato J.A.; Chudoba J.; Chytka L.; Clay R.W.; Cobos Cerutti A.C.; Colalillo R.; Coleman A.; Coluccia M.R.; Conceição R.; Condorelli A.; Consolati G.; Conte M.; Convenga F.; dos Santos D.C.; Costa P.J.; Covault C.E.; Cristinziani M.; Cruz Sanchez C.S.; Dasso S.; Daumiller K.; Dawson B.R.; de Almeida R.M.; de Jesús J.; de Jong S.J.; de Mello Neto J.R.T.; De Mitri I.; de Oliveira J.; de Oliveira Franco D.; de Palma F.; de Souza V.; De Vito E.; Del Popolo A.; Deligny O.; Denner N.; di Matteo A.; Dobre M.; Dobrigkeit C.; D'Olivo J.C.; Domingues Mendes L.M.; dos Anjos J.C.; dos Anjos R.C.; Ebr J.; Ellwanger F.; Emam M.; Engel R.; Epicoco I.; Erdmann M.; Etchegoyen A.; Evoli C.; Falcke H.; Farmer J.; Farrar G.; Fauth A.C.; Fazzini N.; Feldbusch F.; Fenu F.; Fernandes A.; Fick B.; Figueira J.M.; Filipcic A.; Fitoussi T.; Flaggs B.; Fodran T.; Fujii T.; Fuster A.; Galea C.; Galelli C.; García B.; Gaudu C.; Gemmeke H.; Gesualdi F.; Gherghel-Lascu A.; Ghia P.L.; Giaccari U.; Giammarchi M.; Glombitza J.; Gobbi F.; Gollan F.; Golup G.; Gómez Berisso M.; Gómez Vitale P.F.; Gongora J.P.; González J.M.; González N.; Goos I.; Góra D.; Gorgi A.; Gottowik M.; Grubb T.D.; Guarino F.; Guedes G.P.; Guido E.; Hahn S.; Hamal P.; Hampel M.R.; Hansen P.; Harari D.; Harvey V.M.; Haungs A.; Hebbeker T.; Hojvat C.; Hörandel J.R.; Horvath P.; Hrabovský M.; Huege T.; Insolia A.; Isar P.G.; Janecek P.; Johnsen J.A.; Jurysek J.; Kääpä A.; Kampert K.H.; Keilhauer B.; Khakurdikar A.; Kizakke Covilakam V.V.; Klages H.O.; Kleifges M.; Knapp F.; Kunka N.; Lago B.L.; Langner N.; Leigui de Oliveira M.A.; Lema-Capeans Y.; Lenok V.; LetessierSelvon A.; Lhenry-Yvon I.; Lo Presti D.; Lopes L.; Lu L.; Luce Q.; Lundquist J.P.; Machado Payeras A.; Majercakova M.; Mandat D.; Manning B.C.; Mantsch P.; Marafico S.; Mariani F.M.; Mariazzi A.G.; Maris I.C.; Marsella G.; Martello D.; Martinelli S.; Martínez Bravo O.; Martins M.A.; Mastrodicasa M.; Mathes H.J.; Matthews J.; Matthiae G.; Mayotte E.; Mayotte S.; Mazur P.O.; Medina-Tanco G.; Meinert J.; Melo D.; Menshikov A.; Merx C.; Michal S.; Micheletti M.I.; Miramonti L.; Mollerach S.; Montanet F.; Morejon L.; Morello C.; Müller A.L.; Mulrey K.; Mussa R.; Muzio M.; Namasaka W.M.; Negi S.; Nellen L.; Nguyen K.; Nicora G.; Niculescu-Oglinzanu M.; Niechciol M.; Nitz D.; Nosek D.; Novotny V.; Nožka L.; Nucita A.; Núñez L.A.; Oliveira C.; Palatka M.; Pallotta J.; Panja S.; Parente G.; Paulsen T.; Pawlowsky J.; Pech M.; Pȩkala J.; Pelayo R.; Pereira L.A.S.; Pereira Martins E.E.; Perez Armand J.; Pérez Bertolli C.; Perrone L.; Petrera S.; Petrucci C.; Pierog T.; Pimenta M.; Platino M.; Pont B.; Pothast M.; Pourmohammad Shahvar M.; Privitera P.; Prouza M.; Puyleart A.; Querchfeld S.; Rautenberg J.; Ravignani D.; Reininghaus M.; Ridky J.; Riehn F.; Risse M.; Rizi V.; de Carvalho W.R.; Rodriguez E.; Rodriguez Rojo J.; Roncoroni M.J.; Rossoni S.; Roth M.; Roulet E.; Rovero A.C.; Ruehl P.; Saftoiu A.; Saharan M.; Salamida F.; Salazar H.; Salina G.; Sanabria Gomez J.D.; Sánchez F.; Santos E.M.; Santos E.; Sarazin F.; Sarmento R.; Sato R.; Savina P.; Schäfer C.M.; Scherini V.; Schieler H.; Schimassek M.; Schimp M.; Schlüter F.; Schmidt D.; Scholten O.; Schoorlemmer H.; Schovánek P.; Schröder F.G.; Schulte J.; Schulz T.; Sciutto S.J.; Scornavacche M.; Segreto A.; Sehgal S.; Shivashankara S.U.; Sigl G.; Silli G.; Sima O.; Simon F.; Smau R.; Šmída R.; Sommers P.; Soriano J.F.; Squartini R.; Stadelmaier M.; Stanca D.; Stanic S.; Stasielak J.; Stassi P.; Strähnz S.; Straub M.; Suárez-Durán M.; Suomijärvi T.; Supanitsky A.D.; Svozilikova Z.; Szadkowski Z.; Tapia A.; Taricco C.; Timmermans C.; Tkachenko O.; Tobiska P.; Todero Peixoto C.J.; Tomé B.; Torrès Z.; Travaini A.; Travnicek P.; Trimarelli C.; Tueros M.; Unger M.; Vaclavek L.; Vacula M.; Valdés Galicia J.F.; Valore L.; Varela E.; Vásquez-Ramírez A.; Veberic D.; Ventura C.; Vergara Quispe I.D.; Verzi V.; Vicha J.; Vink J.; Vlastimil J.; Vorobiov S.; Watanabe C.; Watson A.A.; Weindl A.; Wiencke L.; Wilczynski H.; Wittkowski D.; Wundheiler B.; Yue B.; Yushkov A.; Zapparrata O.; Zas E.; Zavrtanik D.; Zavrtan M.; Abbasi R.U.; Abe Y.; Abu-Zayyad T.; Allen M.; Arai Y.; Arimura R.; Barcikowski E.; Belz J.W.; Bergman D.R.; Blake S.A.; Buckland I.; Cheon B.G.; Chikawa M.; Fedynitch A.; Fujii T.; Fujisue K.; Fujita K.; Fujiwara R.; Fukushima M.; Furlich G.; Gerber Z.; Globus N.; Hanlon W.; Hayashida N.; He H.; Hibi R.; Hibino K.; Higuchi R.; Honda K.; Ikeda D.; Inoue N.; Ishii T.; Ito H.; Ivanov D.; Iwasaki A.; Jeong H.M.; Jeong S.; Jui C.C.H.; Kadota K.; Kakimoto F.; Kalashev O.; Kasahara K.; Kasami S.; Kawakami S.; Kawata K.; Kharuk I.; Kido E.; Kim H.B.; Kim J.H.; Kim S.W.; Kimura Y.; Komae I.; Komori K.; Kusumori Y.; Kuznetsov M.; Kwon Y.J.; Lee K.H.; Lee M.J.; Lubsandorzhiev B.; Lundquist J.P.; Matsuyama T.; Matthews J.A.; Matthews J.N.; Mayta R.; Miyashita K.; Mizuno K.; Mori M.; Murakami M.; Myers I.; Nagataki S.; Nakai K.; Nakamura T.; Nishio E.; Nonaka T.; Ogio S.; Ohoka H.; Okazaki N.; Oku Y.; Okuda T.; Omura Y.; Onishi M.; Ono M.; Oshima A.; Oshima H.; Ozawa S.; Park I.H.; Park K.Y.; Potts M.; Pshirkov M.S.; Remington J.; Rodriguez D.C.; Rott C.; Rubtsov G.I.; Ryu D.; Sagawa H.; Saito R.; Sakaki N.; Sako T.; Sakurai N.; Sato D.; Sato K.; Sato S.; Sekino K.; Shah P.D.; Shibata N.; Shibata T.; Shikita J.; Shimodaira H.; Shin B.K.; Shin H.S.; Shinto D.; Smith J.D.; Sokolsky P.; Stokes B.T.; Stroman T.A.; Takagi Y.; Takahashi K.; Takamura M.; Takeda M.; Takeishi R.; Taketa A.; Takita M.; Tameda Y.; Tanaka K.; Tanaka M.; Thomas S.B.; Thomson G.B.; Tinyakov P.; Tkachev I.; Tokuno H.; Tomida T.; Troitsky S.; Tsuda R.; Tsunesada Y.; Udo S.; Urban F.; Vaiman I.A.; Warren D.; Wong T.; Yamazaki K.; Yashiro K.; Yoshida F.; Zhezher Y.; Zundel Z.

Citación

       
TY - GEN T1 - Update on the searches for anisotropies in UHECR arrival directions with the Pierre Auger Observatory and the Telescope Array Y1 - 2024 UR - http://hdl.handle.net/11407/8899 PB - et al.; Institute for Cosmic Ray Research (ICRR) Univeristy of Tokyo; International Union of Pure and Applied Physics (IUPAP); JPS; Nagoya Convention and Visitors Bureau; Nagoya University AB - The origin of ultra-high-energy cosmic rays (UHECRs), particles from outer space with energies E ≥ 1 EeV, is still unknown, though the near-isotropy of their arrival direction distribution excludes a dominant Galactic contribution, and interactions with background photons prevent them from travelling cosmologically large distances. This suggests that their sources must be searched for in nearby galaxy groups and clusters. Deflections by intergalactic and Galactic magnetic fields are expected to hinder such searches but not preclude them altogether. So far, the only anisotropy detected with statistical significance ≥ 5σ is a modulation in right ascension in the data from the Pierre Auger Observatory at E ≥ 8 EeV interpretable as a 7% dipole moment. Various hints for higher-energy, smaller-scale anisotropies have been reported. UHECR arrival direction data from both the Pierre Auger Observatory and the Telescope Array experiment have been searched for anisotropies by a working group with members from both collaborations; combining the two datasets requires a cross-calibration procedure due to the different systematic uncertainties on energy measurements but allows us to perform analyses that are less model-dependent than what can be done with partial sky coverage. We report a significant dipole pointing away from the Galactic Center and a ∼4.6σ anisotropy found when comparing the directions of UHECRs with a catalog of starburst galaxies. © Copyright owned by the author(s) under the terms of the Creative Commons. ER - @misc{11407_8899, author = {}, title = {Update on the searches for anisotropies in UHECR arrival directions with the Pierre Auger Observatory and the Telescope Array}, year = {2024}, abstract = {The origin of ultra-high-energy cosmic rays (UHECRs), particles from outer space with energies E ≥ 1 EeV, is still unknown, though the near-isotropy of their arrival direction distribution excludes a dominant Galactic contribution, and interactions with background photons prevent them from travelling cosmologically large distances. This suggests that their sources must be searched for in nearby galaxy groups and clusters. Deflections by intergalactic and Galactic magnetic fields are expected to hinder such searches but not preclude them altogether. So far, the only anisotropy detected with statistical significance ≥ 5σ is a modulation in right ascension in the data from the Pierre Auger Observatory at E ≥ 8 EeV interpretable as a 7% dipole moment. Various hints for higher-energy, smaller-scale anisotropies have been reported. UHECR arrival direction data from both the Pierre Auger Observatory and the Telescope Array experiment have been searched for anisotropies by a working group with members from both collaborations; combining the two datasets requires a cross-calibration procedure due to the different systematic uncertainties on energy measurements but allows us to perform analyses that are less model-dependent than what can be done with partial sky coverage. We report a significant dipole pointing away from the Galactic Center and a ∼4.6σ anisotropy found when comparing the directions of UHECRs with a catalog of starburst galaxies. © Copyright owned by the author(s) under the terms of the Creative Commons.}, url = {http://hdl.handle.net/11407/8899} }RT Generic T1 Update on the searches for anisotropies in UHECR arrival directions with the Pierre Auger Observatory and the Telescope Array YR 2024 LK http://hdl.handle.net/11407/8899 PB et al.; Institute for Cosmic Ray Research (ICRR) Univeristy of Tokyo; International Union of Pure and Applied Physics (IUPAP); JPS; Nagoya Convention and Visitors Bureau; Nagoya University AB The origin of ultra-high-energy cosmic rays (UHECRs), particles from outer space with energies E ≥ 1 EeV, is still unknown, though the near-isotropy of their arrival direction distribution excludes a dominant Galactic contribution, and interactions with background photons prevent them from travelling cosmologically large distances. This suggests that their sources must be searched for in nearby galaxy groups and clusters. Deflections by intergalactic and Galactic magnetic fields are expected to hinder such searches but not preclude them altogether. So far, the only anisotropy detected with statistical significance ≥ 5σ is a modulation in right ascension in the data from the Pierre Auger Observatory at E ≥ 8 EeV interpretable as a 7% dipole moment. Various hints for higher-energy, smaller-scale anisotropies have been reported. UHECR arrival direction data from both the Pierre Auger Observatory and the Telescope Array experiment have been searched for anisotropies by a working group with members from both collaborations; combining the two datasets requires a cross-calibration procedure due to the different systematic uncertainties on energy measurements but allows us to perform analyses that are less model-dependent than what can be done with partial sky coverage. We report a significant dipole pointing away from the Galactic Center and a ∼4.6σ anisotropy found when comparing the directions of UHECRs with a catalog of starburst galaxies. © Copyright owned by the author(s) under the terms of the Creative Commons. OL Spanish (121)
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Abstract
The origin of ultra-high-energy cosmic rays (UHECRs), particles from outer space with energies E ≥ 1 EeV, is still unknown, though the near-isotropy of their arrival direction distribution excludes a dominant Galactic contribution, and interactions with background photons prevent them from travelling cosmologically large distances. This suggests that their sources must be searched for in nearby galaxy groups and clusters. Deflections by intergalactic and Galactic magnetic fields are expected to hinder such searches but not preclude them altogether. So far, the only anisotropy detected with statistical significance ≥ 5σ is a modulation in right ascension in the data from the Pierre Auger Observatory at E ≥ 8 EeV interpretable as a 7% dipole moment. Various hints for higher-energy, smaller-scale anisotropies have been reported. UHECR arrival direction data from both the Pierre Auger Observatory and the Telescope Array experiment have been searched for anisotropies by a working group with members from both collaborations; combining the two datasets requires a cross-calibration procedure due to the different systematic uncertainties on energy measurements but allows us to perform analyses that are less model-dependent than what can be done with partial sky coverage. We report a significant dipole pointing away from the Galactic Center and a ∼4.6σ anisotropy found when comparing the directions of UHECRs with a catalog of starburst galaxies. © Copyright owned by the author(s) under the terms of the Creative Commons.
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http://hdl.handle.net/11407/8899
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