Pith. sign in

REVIEW

Features of the energy spectrum of cosmic rays above 2.5{times} 10¹⁸ eV using the Pierre Auger Observatory

Not yet reviewed by Pith; the record is open.

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 2008.06488 v2 pith:4GKH5JZS submitted 2020-08-14 astro-ph.HE

Features of the energy spectrum of cosmic rays above 2.5{times} 10¹⁸ eV using the Pierre Auger Observatory

The Pierre Auger Collaboration: A. Aab , P. Abreu , M. Aglietta , J.M. Albury , I. Allekotte , A. Almela , J. Alvarez Castillo , J. Alvarez-Mu\~niz
show 374 more authors
R. Alves Batista G.A. Anastasi L. Anchordoqui B. Andrada S. Andringa C. Aramo P.R. Ara\'ujo Ferreira H. Asorey P. Assis G. Avila A.M. Badescu A. Bakalova A. Balaceanu F. Barbato R.J. Barreira Luz K.H. Becker J.A. Bellido C. Berat M.E. Bertaina X. Bertou P.L. Biermann T. Bister J. Biteau A. Blanco J. Blazek C. Bleve M. Boh\'a\v{c}ov\'a D. Boncioli C. Bonifazi L. Bonneau Arbeletche N. Borodai A.M. Botti J. Brack T. Bretz F.L. Briechle P. Buchholz A. Bueno S. Buitink M. Buscemi K.S. Caballero-Mora L. Caccianiga L. Calcagni A. Cancio F. Canfora I. Caracas J.M. Carceller R. Caruso A. Castellina F. Catalani G. Cataldi L. Cazon M. Cerda J.A. Chinellato K. Choi J. Chudoba L. Chytka R.W. Clay A.C. Cobos Cerutti R. Colalillo A. Coleman M.R. Coluccia R. Concei\c{c}\~ao A. Condorelli G. Consolati F. Contreras F. Convenga C.E. Covault S. Dasso K. Daumiller B.R. Dawson J.A. Day R.M. de Almeida J. de Jes\'us S.J. de Jong G. De Mauro J.R.T. de Mello Neto I. De Mitri J. de Oliveira D. de Oliveira Franco V. de Souza E. De Vito J. Debatin M. del R\'io O. Deligny H. Dembinski N. Dhital C. Di Giulio A. Di Matteo M.L. D\'iaz Castro C. Dobrigkeit J.C. D'Olivo Q. Dorosti R.C. dos Anjos M.T. Dova J. Ebr R. Engel I. Epicoco M. Erdmann C.O. Escobar A. Etchegoyen H. Falcke J. Farmer G. Farrar A.C. Fauth N. Fazzini F. Feldbusch F. Fenu B. Fick J.M. Figueira A. Filip\v{c}i\v{c} T. Fodran M.M. Freire T. Fujii A. Fuster C. Galea C. Galelli B. Garc\'ia A.L. Garcia Vegas H. Gemmeke F. Gesualdi A. Gherghel-Lascu P.L. Ghia U. Giaccari M. Giammarchi M. Giller J. Glombitza F. Gobbi F. Gollan G. Golup M. G\'omez Berisso P.F. G\'omez Vitale J.P. Gongora N. Gonz\'alez I. Goos D. G\'ora A. Gorgi M. Gottowik T.D. Grubb F. Guarino G.P. Guedes E. Guido S. Hahn R. Halliday M.R. Hampel P. Hansen D. Harari V.M. Harvey A. Haungs T. Hebbeker D. Heck G.C. Hill C. Hojvat J.R. H\"orandel P. Horvath M. Hrabovsk\'y T. Huege J. Hulsman A. Insolia P.G. Isar J.A. Johnsen J. Jurysek A. K\"a\"ap\"a K.H. Kampert B. Keilhauer J. Kemp H.O. Klages M. Kleifges J. Kleinfeller M. K\"opke G. Kukec Mezek B.L. Lago D. LaHurd R.G. Lang M.A. Leigui de Oliveira V. Lenok A. Letessier-Selvon I. Lhenry-Yvon D. Lo Presti L. Lopes R. L\'opez R. Lorek Q. Luce A. Lucero A. Machado Payeras M. Malacari G. Mancarella D. Mandat B.C. Manning J. Manshanden P. Mantsch S. Marafico A.G. Mariazzi I.C. Mari\c{s} G. Marsella D. Martello H. Martinez O. Mart\'inez Bravo M. Mastrodicasa H.J. Mathes J. Matthews G. Matthiae E. Mayotte P.O. Mazur G. Medina-Tanco D. Melo A. Menshikov K.-D. Merenda S. Michal M.I. Micheletti L. Miramonti D. Mockler S. Mollerach F. Montanet C. Morello M. Mostaf\'a A.L. M\"uller M.A. Muller K. Mulrey R. Mussa M. Muzio W.M. Namasaka L. Nellen P.H. Nguyen M. Niculescu-Oglinzanu M. Niechciol D. Nitz D. Nosek V. Novotny L. No\v{z}ka A Nucita L.A. N\'u\~nez M. Palatka J. Pallotta M.P. Panetta P. Papenbreer G. Parente A. Parra M. Pech F. Pedreira J. P\k{e}kala R. Pelayo J. Pe\~na-Rodriguez J. Perez Armand M. Perlin L. Perrone C. Peters S. Petrera T. Pierog M. Pimenta V. Pirronello M. Platino B. Pont M. Pothast P. Privitera M. Prouza A. Puyleart S. Querchfeld J. Rautenberg D. Ravignani M. Reininghaus J. Ridky F. Riehn M. Risse P. Ristori V. Rizi W. Rodrigues de Carvalho G. Rodriguez Fernandez J. Rodriguez Rojo M.J. Roncoroni M. Roth E. Roulet A.C. Rovero P. Ruehl S.J. Saffi A. Saftoiu F. Salamida H. Salazar G. Salina J.D. Sanabria Gomez F. S\'anchez E.M. Santos E. Santos F. Sarazin R. Sarmento C. Sarmiento-Cano R. Sato P. Savina C. Sch\"afer V. Scherini H. Schieler M. Schimassek M. Schimp F. Schl\"uter D. Schmidt O. Scholten P. Schov\'anek F.G. Schr\"oder S. Schr\"oder A. Schulz S.J. Sciutto M. Scornavacche R.C. Shellard G. Sigl G. Silli O. Sima R. \v{S}m\'ida P. Sommers J.F. Soriano J. Souchard R. Squartini M. Stadelmaier D. Stanca S. Stani\v{c} J. Stasielak P. Stassi A. Streich M. Su\'arez-Dur\'an T. Sudholz T. Suomij\"arvi A.D. Supanitsky J. \v{S}up\'ik Z. Szadkowski A. Taboada A. Tapia C. Timmermans O. Tkachenko P. Tobiska C.J. Todero Peixoto B. Tom\'e G. Torralba Elipe A. Travaini P. Travnicek C. Trimarelli M. Trini M. Tueros R. Ulrich M. Unger M. Urban L. Vaclavek M. Vacula J.F. Vald\'es Galicia I. Vali\~no L. Valore A. van Vliet E. Varela B. Vargas C\'ardenas A. V\'asquez-Ram\'irez D. Veberi\v{c} C. Ventura I.D. Vergara Quispe V. Verzi J. Vicha L. Villase\~nor J. Vink S. Vorobiov H. Wahlberg A.A. Watson M. Weber A. Weindl L. Wiencke H. Wilczy\'nski T. Winchen M. Wirtz D. Wittkowski B. Wundheiler A. Yushkov O. Zapparrata E. Zas D. Zavrtanik M. Zavrtanik L. Zehrer A. Zepeda M. Ziolkowski F. Zuccarello
This is my paper
classification astro-ph.HE
keywords textrmtimesstatabovecosmicenergyfeaturesrays
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
0 comments
read the original abstract

We report a measurement of the energy spectrum of cosmic rays above $2.5{\times} 10^{18}$ eV based on $215,030$ events. New results are presented: at about $1.3{\times} 10^{19}$ eV, the spectral index changes from $2.51 \pm 0.03 \textrm{ (stat.)} \pm 0.05 \textrm{ (sys.)}$ to $3.05 \pm 0.05 \textrm{ (stat.)}\pm 0.10\textrm{ (sys.)}$, evolving to $5.1\pm0.3\textrm{ (stat.)} \pm 0.1\textrm{ (sys.)}$ beyond $5{\times} 10^{19}$ eV, while no significant dependence of spectral features on the declination is seen in the accessible range. These features of the spectrum can be reproduced in models with energy-dependent mass composition. The energy density in cosmic rays above $5{\times} 10^{18}$ eV is $(5.66 \pm 0.03 \textrm{ (stat.)} \pm 1.40 \textrm{ (sys.)} ) {\times} 10^{53}~$erg Mpc$^{-3}$.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.