Features of the Energy Spectrum of Cosmic Rays above 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mn>2.5</mml:mn><mml:mo>×</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mn>18</mml:mn></mml:msup><mml:mtext> </mml:mtext><mml:mtext> </mml:mtext><mml:mi>eV</mml:mi></mml:math>
 Using the Pierre Auger Observatory

Aab, A.; Abreu, P.; Aglietta, M.; Albury, Justin M.; Allekotte, I.; Almela, A.; Castillo, J.; Álvarez-Muñiz, J.; Batista, Rafael Alves; Anastasi, Gioacchino Alex; Anchordoqui, Luis A.; Andrada, Belén; Andringa, S.; Aramo, C.; Ferreira, Paulo Ricardo Araújo; Asorey, H.; Assis, P.; Ávila, G.; Badescu, A. M.; Bakalová, Alena; Bălăceanu, Alexandru; Barbato, Felicia; Luz, Ricardo Jorge Barreira; Becker, Karl‐Heinz; Bellido, J. A.; Bérat, C.; Bertaina, M.; Bertou, X.; Biermann, Peter L.; Bister, Teresa; Biteau, J.; Blanco, A.; Blažek, Jiří; Bleve, C.; Bohã̌cov́a, M.; Boncioli, D.; Bonifazi, C.; Arbeletche, Luan Bonneau; Borodai, N.; Botti, Ana Martina; Brack, Jeffrey; Bretz, T.; Briechle, Florian Lukas; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, Mario; Caballero-Mora, K. S.; Caccianiga, Lorenzo; Calcagni, L.; Cancio, A.; Canfora, F.; Caracas, Ioana; Carceller, Juan Miguel; Caruso, R.; Castellina, A.; Catalani, Fernando; Cataldi, G.; Cazón, L.; Cerda, Marcos; Chinellato, J. A.; Choi, Ki Young; Chudoba, J.; Chytka, L.; Clay, R. W.; Cerutti, Agustín Cobos; Colalillo, R.; Coleman, Alan; Coluccia, M. R.; Conceição, R.; Condorelli, Antonio; Consolati, G.; Contreras, F.; Convenga, Fabio; Covault, C. E.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Day, J. A.; Almeida, R. M. de; Jesús, Joaquín de; Jong, S. J. De; Mauro, G. De; Neto, J. R. T. de Mello; Mitri, I. De; Oliveira, Jaime de; Franco, D.; Souza, Vítor de; Vito, Emanuele De; Debatin, J.; Río, Mariano del; Deligny, O.; Dembinski, H.-P.; Dhital, N.; Giulio, C. Di; Matteo, Armando di; Castro, M. L. Díaz; Dobrigkeit, C.; D’Olivo, J. C.; Dorosti, Q.; Anjos, Rita Cassia dos; Dova, M. T.; Ebr, Jan; Engel, R.; Epicoco, Italo; Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Falcke, H.; Farmer, John; Farrar, Glennys R.; Fauth, A. C.; Fazzini, N.; Feldbusch, Fridtjof; Fenu, Francesco; Fick, B.; Figueira, J. M.; Filipčić, A.; Fodran, Tomáš; Freire, M. M.; Fujii, Toshihiro; Fuster, Alan; Galea, C.; Galelli, Claudio; García, Beatriz; Vegas, Adrianna Luz García; Gemmeke, H.; Gesualdi, Flavia; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Glombitza, Jonas; Gobbi, Fabian; Gollan, Fernando; Golup, G.; Berisso, M. Gómez; Vitale, Primo F. Gómez; Gongora, Juan Pablo; González, Nicolás Martín; Goos, Isabel; Góra, D.; Gorgi, A.; Gottowik, Marvin; Grubb, Trent D.; Guarino, F.; Guedes, G. P.; Guido, Eleonora; Hahn, S.; Halliday, R.; Hampel, Matías Rolf; Hansen, P.; Harari, D.; Harvey, Violet M.; Haungs, A.; Hebbeker, T.; Heck, D.; Hill, G. C.; Hojvat, C.; Hörandel, J. R.; Horváth, P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Johnsen, Jeffrey A.; Jurýšek, Jakub; Kääpä, Alex; Kampert, K. H.; Keilhauer, B.; Kemp, J.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Köpke, Marcel; Mezek, G. Kukec; Lago, Bruno L.; LaHurd, D.; Lang, Rodrigo Guedes; Oliveira, M. A. Leigui de; Lenok, Vladimir; Letessier‐Selvon, A.; Lhenry-Yvon, I.; Presti, Domenico Lo; Lopes, L.; López, R.; Lorek, R.; Luce, Quentin; Lucero, A.; Payeras, Allan Machado; Malacari, M.; Mancarella, G.; Mandát, Dušan; Manning, Bradley C.; Manshanden, Julien; Mantsch, P.; Marafico, Sullivan; Mariazzi, A. G.; Maris, Ioana Codrina; Marsella, G.; Martello, D.; Martínez, H.; Bravo, O. Martínez; Mastrodicasa, Massimo; Mathes, H. J.; Matthews, John; Matthiae, G.; Mayotte, E.; Mazur, Péter; Medina‐Tanco, G.; Melo, D.; Menshikov, A.; Merenda, Kevin-Druis; Michal, Stanislav; Micheletti, M. I.; Miramonti, L.; Mockler, D.; Mollerach, Silvia; Montanet, F.; Morello, C.; Mostafá, M.; Müller, Ana L.; Müller, M. A.; Mulrey, K.; Mussa, R.; Muzio, Marco Stein; Namasaka, Wilson M.; Nellen, L.; Nguyen, P.; Niculescu-Oglinzanu, M.; Niechciol, Marcus; Nitz, D.; Nosek, D.; Novotný, Vladimír; Nožka, L.; Nucita, A. A.; Núñez, Luis A.; Palatka, M.; Pallotta, J.; Panetta, M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.; Pedreira, F.; Pękala, Jan; Pelayo, R.; Peña-Rodríguez, Jesús; Armand, Johnnier Perez; Perlín, M.; Perrone, L.; Peters, C. F. W.; Petrera, S.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.; Pont, Bjarni; Pothast, Mart; Privitera, P.; Prouza, M.; Puyleart, Andrew; Querchfeld, S.; Rautenberg, J.; Ravignani, D.; Reininghaus, Maximilian; Řídký, J.; Riehn, Felix; Risse, M.; Ristori, P.; Rizi, V.; Carvalho, W. Rodrigues de; Fernandez, G. Rodriguez; Rojo, Juan; Roncoroni, Matías J.; Roth, M.; Roulet, Esteban; Rovero, A. C.; Ruehl, Philip; Saffi, S. J.; Sǎftoiu, A.; Salamida, F.; Salazar, H.; Salina, G.; Gómez, J. D. Sanabria; Sánchez, F.; Santos, Edivaldo Moura; Santos, Eva; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.; Savina, Pierpaolo; Schäfer, C.; Scherini, V.; Schieler, H.; Schimassek, Martin; Schimp, Michael; Schlüter, Felix; Schmidt, D.; Scholten, Olaf; Schovánek, Petr; Schröder, Frank G.; Schröder, S.; Schulz, Alexander; Sciutto, S. J.; Scornavacche, Marina; Shellard, R. C.; Sigl, Guenter; Silli, Gaia; Sima, O.; Šmída, R.; Sommers, P.; Soriano, Jorge F.; Souchard, Julien; Squartini, R.; Stadelmaier, Maximilian; Stanca, Denis; Stanič, S.; Stasielak, J.; Stassi, P.; Streich, Alexander; Suárez-Durán, Mauricio; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.; Šupík, J.; Szadkowski, Z.; Taboada, A.; Tapia, A.; Timmermans, C.; Tkachenko, Olena; Tobiška, Petr; Peixoto, C. J. Todero; Tomé, B.; Elipe, G. Torralba; Travaini, Andres; Trávničék, P.; Trimarelli, Caterina; Trini, M.; Tueros, M.; Ulrich, R.; Unger, Michael; Urban, M.; Vaclavek, Lukáš; Vacula, Martin; Galicia, J. F. Valdés; Valiño, I.; Valore, L.; Vliet, A. van; Varela, E.; Cárdenas, B. Vargas; Vásquez-Ramírez, Adriana; Veberič, D.; Ventura, Cynthia; Quispe, Indira D. Vergara; Verzi, V.; Vícha, J.; Villaseñor, L.; Vink, Jacco; Vorobiov, S.; Wahlberg, H.; Watson, Alan; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, Marcus; Wittkowski, David; Wundheiler, B.; Yushkov, A.; Zapparrata, Orazio; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zehrer, Lukas; Zepeda, A.; Ziolkowski, M.; Zuccarello, F.

doi:10.1103/physrevlett.125.121106

Cited by 125 publications

(79 citation statements)

References 59 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…4No evidence for any dependence of the energy spectrum on declination has been found other than a mild excess from the Southern Hemisphere that is consistent with the anisotropy observed above 8 × 10 18 eV. A discussion of the significance of these measurements from astrophysical perspectives can be found in [54].…”

Section: Discussionmentioning

confidence: 64%

Measurement of the cosmic-ray energy spectrum above2.5×1018 eVusing the Pierre Auger Observatory

Aab¹,

Abreu²,

Aglietta³

et al. 2020

Phys. Rev. D

Self Cite

156

107

View full text Add to dashboard Cite

We report a measurement of the energy spectrum of cosmic rays for energies above 2.5 × 10 18 eV based on 215,030 events recorded with zenith angles below 60°. A key feature of the work is that the estimates of the energies are independent of assumptions about the unknown hadronic physics or of the primary mass composition. The measurement is the most precise made hitherto with the accumulated exposure being so large that the measurements of the flux are dominated by systematic uncertainties except at energies above 5 × 10 19 eV. The principal conclusions are (1) The flattening of the spectrum near 5 × 10 18 eV, the so-called "ankle," is confirmed. (2) The steepening of the spectrum at around 5 × 10 19 eV is confirmed. (3) A new feature has been identified in the spectrum: in the region above the ankle the spectral index γ of the particle flux (∝ E −γ) changes from 2.51 AE 0.03 ðstatÞ AE 0.05 ðsystÞ to 3.05 AE 0.05 ðstatÞ AE 0.10 ðsystÞ before changing sharply to 5.1 AE 0.3 ðstatÞ AE 0.1 ðsystÞ above 5 × 10 19 eV. (4) No evidence for any dependence of the spectrum on declination has been found other than a mild excess from the Southern Hemisphere that is consistent with the anisotropy observed above 8 × 10 18 eV.

show abstract

Section: Discussionmentioning

confidence: 64%

Measurement of the cosmic-ray energy spectrum above2.5×1018 eVusing the Pierre Auger Observatory

Aab¹,

Abreu²,

Aglietta³

et al. 2020

Phys. Rev. D

Self Cite

156

107

View full text Add to dashboard Cite

show abstract

“…However, as already mentioned, the two great experiments, the Pierre Auger Observatory and the Telescope Array, also reported around 20 UHECR cases of energies above 10 20 eV observed already with the newest tools and methods (see e.g., Ref. [58] where 15 events with energies above 10 20 eV are mentioned collectively). To list just a few such events in detail we mention the Pierre Auger Observatory measurements which contain an event with energy 1.4 × 10 20 eV [59] -or 1.3 × 10 20 eV [60], and the Telescope Array announcement concerning an event of similar energy 1.39 × 10 20 eV [48].…”

Section: Credo Within the Cosmic-ray Landscapementioning

confidence: 85%

“…It is a great achievement that today we can tell that the UHECR spectrum has been quite well measured-see for example two recent Pierre Auger Observatory papers [58,61], and that a lot of effort and resources are being currently invested into explaining the nature of the observed spectrum suppression (GZK-like versus acceleration limit). Nevertheless the current results are still inconclusive, and it is, therefore, advisable to continue research in the highest energy regime of cosmic rays, and to try alternative methods whenever possible.…”

Section: Credo Within the Cosmic-ray Landscapementioning

confidence: 99%

Cosmic-Ray Extremely Distributed Observatory

et al. 2020

View full text Add to dashboard Cite

The Cosmic-Ray Extremely Distributed Observatory (CREDO) is a newly formed, global collaboration dedicated to observing and studying cosmic rays (CR) and cosmic-ray ensembles (CRE): groups of at least two CR with a common primary interaction vertex or the same parent particle. The CREDO program embraces testing known CR and CRE scenarios, and preparing to observe unexpected physics, it is also suitable for multi-messenger and multi-mission applications. Perfectly matched to CREDO capabilities, CRE could be formed both within classical models (e.g., as products of photon–photon interactions), and exotic scenarios (e.g., as results of decay of Super-Heavy Dark Matter particles). Their fronts might be significantly extended in space and time, and they might include cosmic rays of energies spanning the whole cosmic-ray energy spectrum, with a footprint composed of at least two extensive air showers with correlated arrival directions and arrival times. As the CRE are predominantly expected to be spread over large areas and, due to the expected wide energy range of the contributing particles, such a CRE detection might only be feasible when using all available cosmic-ray infrastructure collectively, i.e., as a globally extended network of detectors. Thus, with this review article, the CREDO Collaboration invites the astroparticle physics community to actively join or to contribute to the research dedicated to CRE and, in particular, to pool together cosmic-ray data to support specific CRE detection strategies.

show abstract

“…Ref. [58] where 15 events with energies above 10 20 eV are mentioned collectively). To list just a few such events in detail we mention the Pierre Auger Observatory measurements which contain an event with energy 1.4 × 10 20 eV [59] -or 1.3 × 10 20 eV [60], and the Telescope Array announcement concerning an event of similar energy 1.39 × 10 20 eV [48].…”

Section: Credo Within the Cosmic Ray Landscapementioning

confidence: 99%

Cosmic Ray Extremely Distributed Observatory

Homola¹,

Beznosko²,

Bhatta³

et al. 2020

Preprint

View full text Add to dashboard Cite

The Cosmic Ray Extremely Distributed Observatory (CREDO) is a newly formed, global collaboration dedicated to observing and studying cosmic rays (CR) and cosmic ray ensembles (CRE): groups of a minimum of two CR with a common primary interaction vertex or the same parent particle. The CREDO program embraces testing known CR and CRE scenarios, and preparing to observe unexpected physics, it is also suitable for multi-messenger and multi-mission applications. Perfectly matched to CREDO capabilities, CRE could be formed both within classical models (e.g. as products of photon-photon interactions), and exotic scenarios (e.g. as results of decay of Super Heavy Dark Matter particles), their fronts might be significantly extended in space and time, and they might include cosmic rays of energies spanning the whole cosmic ray energy spectrum. CRE are expected to be partially observable on Earth even if the initiating interaction or process occurs as far as ~1 Gpc away. They would have a footprint composed of at least two extensive air showers with correlated arrival directions and arrival times. Since CRE are mostly expected to be spread over large areas and, because of the expected wide energy range of the contributing particles, CRE detection might only be feasible when using available cosmic ray infrastructure collectively, i.e. as a globally extended network of detectors. Thus, with this review article, the CREDO Collaboration invites the astroparticle physics community to actively join or to contribute to the research dedicated to CRE, and in particular to share any cosmic ray data useful for the specific CRE detection strategies.

show abstract

Features of the Energy Spectrum of Cosmic Rays above 2.5×1018 eV Using the Pierre Auger Observatory

Cited by 125 publications

References 59 publications

Measurement of the cosmic-ray energy spectrum above2.5×1018 eVusing the Pierre Auger Observatory

Measurement of the cosmic-ray energy spectrum above2.5×1018 eVusing the Pierre Auger Observatory

Cosmic-Ray Extremely Distributed Observatory

Cosmic Ray Extremely Distributed Observatory

Contact Info

Product

Resources

About