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Investigating the UHECR characteristics from cosmogenic neutrino limits with the measurements of the Pierre Auger Observatory

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Date
2024
Author
Petrucci C.; 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.; Correia dos Santos D.; 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.; Deval L.; 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.; Letessier-Selvon 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.; Pekala 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.; Rodrigues de Carvalho W.; 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.; Zavrtanik M.

Citación

       
TY - GEN T1 - Investigating the UHECR characteristics from cosmogenic neutrino limits with the measurements of the Pierre Auger Observatory Y1 - 2024 UR - http://hdl.handle.net/11407/8850 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 - Cosmogenic neutrinos are expected to originate in the extragalactic propagation of ultra-high-energy cosmic rays (UHECRs), as a result of their interactions with background photons. Due to these reactions, the visible Universe in UHECRs is more limited than in neutrinos, which instead could reach us without interacting after traveling cosmological distances. In this contribution, we exploit a multimessenger approach by computing the expected energy spectrum and mass composition of UHECRs at Earth corresponding to combinations of spectral parameters and mass composition at their sources, as well as parameters related to the UHECR source distribution, and by determining, at the same time, the associated cosmogenic neutrino fluxes. By comparing the expected UHECR observables to the energy spectrum and mass composition measured at the Pierre Auger Observatory above 1017.8 eV and the expected neutrino fluxes to the most updated neutrino limits, we show the dependence of the neutrino fluxes on the characteristics of the the properties of the potential sources of UHECRs, such as their cosmological evolution and maximum redshift. In addition, the fraction of protons compatible with the data is also investigated in terms of expected neutrino fluxes. © Copyright owned by the author(s) under the terms of the Creative Commons. ER - @misc{11407_8850, author = {}, title = {Investigating the UHECR characteristics from cosmogenic neutrino limits with the measurements of the Pierre Auger Observatory}, year = {2024}, abstract = {Cosmogenic neutrinos are expected to originate in the extragalactic propagation of ultra-high-energy cosmic rays (UHECRs), as a result of their interactions with background photons. Due to these reactions, the visible Universe in UHECRs is more limited than in neutrinos, which instead could reach us without interacting after traveling cosmological distances. In this contribution, we exploit a multimessenger approach by computing the expected energy spectrum and mass composition of UHECRs at Earth corresponding to combinations of spectral parameters and mass composition at their sources, as well as parameters related to the UHECR source distribution, and by determining, at the same time, the associated cosmogenic neutrino fluxes. By comparing the expected UHECR observables to the energy spectrum and mass composition measured at the Pierre Auger Observatory above 1017.8 eV and the expected neutrino fluxes to the most updated neutrino limits, we show the dependence of the neutrino fluxes on the characteristics of the the properties of the potential sources of UHECRs, such as their cosmological evolution and maximum redshift. In addition, the fraction of protons compatible with the data is also investigated in terms of expected neutrino fluxes. © Copyright owned by the author(s) under the terms of the Creative Commons.}, url = {http://hdl.handle.net/11407/8850} }RT Generic T1 Investigating the UHECR characteristics from cosmogenic neutrino limits with the measurements of the Pierre Auger Observatory YR 2024 LK http://hdl.handle.net/11407/8850 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 Cosmogenic neutrinos are expected to originate in the extragalactic propagation of ultra-high-energy cosmic rays (UHECRs), as a result of their interactions with background photons. Due to these reactions, the visible Universe in UHECRs is more limited than in neutrinos, which instead could reach us without interacting after traveling cosmological distances. In this contribution, we exploit a multimessenger approach by computing the expected energy spectrum and mass composition of UHECRs at Earth corresponding to combinations of spectral parameters and mass composition at their sources, as well as parameters related to the UHECR source distribution, and by determining, at the same time, the associated cosmogenic neutrino fluxes. By comparing the expected UHECR observables to the energy spectrum and mass composition measured at the Pierre Auger Observatory above 1017.8 eV and the expected neutrino fluxes to the most updated neutrino limits, we show the dependence of the neutrino fluxes on the characteristics of the the properties of the potential sources of UHECRs, such as their cosmological evolution and maximum redshift. In addition, the fraction of protons compatible with the data is also investigated in terms of expected neutrino fluxes. © Copyright owned by the author(s) under the terms of the Creative Commons. OL Spanish (121)
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Abstract
Cosmogenic neutrinos are expected to originate in the extragalactic propagation of ultra-high-energy cosmic rays (UHECRs), as a result of their interactions with background photons. Due to these reactions, the visible Universe in UHECRs is more limited than in neutrinos, which instead could reach us without interacting after traveling cosmological distances. In this contribution, we exploit a multimessenger approach by computing the expected energy spectrum and mass composition of UHECRs at Earth corresponding to combinations of spectral parameters and mass composition at their sources, as well as parameters related to the UHECR source distribution, and by determining, at the same time, the associated cosmogenic neutrino fluxes. By comparing the expected UHECR observables to the energy spectrum and mass composition measured at the Pierre Auger Observatory above 1017.8 eV and the expected neutrino fluxes to the most updated neutrino limits, we show the dependence of the neutrino fluxes on the characteristics of the the properties of the potential sources of UHECRs, such as their cosmological evolution and maximum redshift. In addition, the fraction of protons compatible with the data is also investigated in terms of expected neutrino fluxes. © Copyright owned by the author(s) under the terms of the Creative Commons.
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http://hdl.handle.net/11407/8850
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