The Pierre Auger Observatory Upgrade - Preliminary Design Report

Collaboration, The Pierre Auger; Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allison, P.; Almela, A.; Castillo, J.; J., Alvarez-Muñiz,; Batista, Rafael Alves; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.; Arqueros, F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.; Barber, K. B.; Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blaess, S. G.; Blanco, A.; Blanco, M.; Blazek, J.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Borodai, N.; Brack, J.; Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.; Buchholz, P.; Bueno, A.; S., Buitink,; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato, J.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição, R.; F., Contreras,; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault, C. E.; Cronin, J.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Almeida, R. M. de; Jong, S. J. de; G., De Mauro,; Neto, J. R. T. de Mello; Mitri, I. De; J., de Oliveira,; Souza, V. de; Peral, L. del; Deligny, O.; H., Dembinski,; Dhital, N.; Giulio, C. Di; Matteo, A. Di; Diaz, J. C.; Castro, M. L. Díaz; Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev, A.; Hasankiadeh, Q. Dorosti; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; H., Falcke,; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fernandes, M.; Fick, B.; Figueira, J. M.; Filevich, A.; A., Filipčič,; Fox, B. D.; Fratu, O.; Freire, M. M.; Fuchs, B.; Fujii, T.; García, B.; Garcia-Pinto, D.; Gate, F.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; M., Giammarchi,; Giller, M.; Głas, D.; Glaser, C.; Glass, H.; Golup, G.; Berisso, M. Gómez; Vitale, Primo F. Gómez; González, N.; Gookin, B.; J., Gordon,; Gorgi, A.; Gorham, P.; Gouffon, P.; Griffith, N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; N., Hemery,; Herve, A. E.; Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.; M., Hrabovský,; Huber, D.; Huege, T.; Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Johnsen, J. A.; Josebachuili, M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.; Kégl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Krömer, O.; Kuempel, D.; Mezek, G. Kukec; Kunka, N.; LaHurd, D.; Latronico, L.; Lauer, R.; Lauscher, M.; Lautridou, P.; Coz, S. Le; Lebrun, D.; Lebrun, P.; Oliveira, M. A. Leigui de; Letessier-Selvon, A.; Lhenry-Yvon, I.; K., Link,; Lopes, L.; López, R.; Casado, A. López; Louedec, K.; Lu, L.; Lucero, A.; Malacari, M.; Maldera, S.; M., Mallamaci,; Maller, J.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Bravo, O. Martínez; Martraire, D.; Meza, J. J. Masías; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, John; Matthiae, G.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Meissner, R.; Mello, V. B. B.; D., Melo,; A., Menshikov,; Messina, S.; Meyhandan, R.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet, F.; Morello, C.; Mostafá, M.; Moura, C. A.; Muller, M. A.; Müller, G.; Müller, S.; Mussa, R.; Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; M., Niechciol,; Niemietz, L.; Niggemann, T.; D., Nitz,; Nosek, D.; V., Novotny,; Nožka, L.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pacheco, N.; Selmi-Dei, D. Pakk; Palatka, M.; Pallotta, J.; Papenbreer, P.; G., Parente,; Parra, A.; Paul, T.; Pech, M.; Pȩkala, J.; R., Pelayo,; Pepe, I. M.; Perrone, L.; Petermann, E.; C., Peters,; Petrera, S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; M., Platino,; Plum, M.; Porcelli, A.; Porowski, C.; Prado, R. R.; P., Privitera,; Prouza, M.; Purrello, V.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.; Reinert, D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori, P.; V., Rizi,; Carvalho, W. Rodrigues de; Fernandez, G. Rodriguez; Rojo, Juan; Rodríguez-Frías, M. D.; Rogozin, D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Greus, F. Salesa; Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santos, E.; M., Santos, E.; F., Sarazin,; Sarkar, B.; Sarmento, R.; Sato, R.; Scarso, C.; M., Schauer,; Scherini, V.; Schieler, H.; Schmidt, D.; Scholten, O.; Schoorlemmer, H.; Schovánek, P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.; O., Sima,; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Squartini, R.; Srivastava, Y. N.; D., Stanca,; Stanič, S.; Stapleton, J.; Stasielak, J.; Stephan, M.; Stutz, A.; Suarez, F.; Suomijärvi, T.; Supanitsky, A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.; A., Tapia,; Tepe, A.; Theodoro, V. M.; C., Timmermans,; Peixoto, C. J. Todero; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Elipe, G. Torralba; Machado, D. Torres; Travnicek, P.; Trini, M.; Ulrich, R.; Unger, M.; M., Urban,; Galicia, J. F. Valdés; I., Valiño,; Valore, L.; Aar, G. van; Bodegom, P. van; Berg, A. M. van den; Velzen, S. van; Vliet, A. van; Varela, E.; Vargas, Cárdenas, B.; Varner, G.; Vasquez, R.; Vázquez, J. R.; Vázquez, R. A.; D., Veberič,; Verzi, V.; Vicha, J.; Videla, M.; L., Villaseñor,; Vlcek, B.; Vorobiov, S.; H., Wahlberg,; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt, K.; A., Weindl,; Werner, F.; Widom, A.; Wiencke, L.; H., Wilczyński,; Winchen, T.; D., Wittkowski,; Wundheiler, B.; Wykes, S.; Yang, L.; Yapici, T.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zepeda, A.; Zhu, Y.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.

doi:10.48550/arxiv.1604.03637

Cited by 96 publications

(140 citation statements)

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“…The forthcoming Run 3 at the LHC, for which proton-oxygen and oxygen-oxygen collisions have been approved, can therefore bring useful data to solve this puzzle. Another fundamental line of action is represented by the upgrade of the Pierre Auger Observatory, AugerPrime [11], currently underway, whose main goal will be that of improving the sensitivity to the composition at all the energies.…”

Section: Pos(panic2021)330mentioning

confidence: 99%

Probing hadronic interactions with the Pierre Auger Observatory

Fenu¹

2022

Proceedings of Particles and Nuclei International Conference 2021 — PoS(PANIC2021)

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The study of ultra-high energy cosmic rays provides information about the hadronic interactions in an energy and kinematic region well beyond those explored in accelerators. The Pierre Auger Observatory is the largest cosmic ray observatory ever built (3000 km 2 ), operating since 2004 in the Argentinian Pampa. Its hybrid design allows one to measure the longitudinal and lateral distribution of extensive air showers and the establishment of an almost model-independent, calorimetric, energy scale. The observatory is sensitive to the electromagnetic and to the muonic components of extensive air showers, which are directly related to the energy and type of the primary particle and to the hadronic interaction parameters. In this contribution an overview of the results obtained by the Auger collaboration in the field of particle physics will be given. We will show the proton-Air cross section at 38.7 and 55.5 TeV. Our data indicate that hadronic interaction models fail in the predictions of the muon densities on the surface, too low with respect to the measured ones. Possible future lines of research to investigate this inconsistency will be identified.

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Section: Pos(panic2021)330mentioning

confidence: 99%

Probing hadronic interactions with the Pierre Auger Observatory

Fenu¹

2022

Proceedings of Particles and Nuclei International Conference 2021 — PoS(PANIC2021)

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“…The AugerPrime upgrade [39] of the Pierre Auger Observatory has been specifically designed to improve mass composition in the whole energy range. Along the line of a hybrid design, each SD will be equipped with a top scintillator layer.…”

Section: Future Prospects: Augerprimementioning

confidence: 99%

Recent results from the Pierre Auger Observatory

Petrera

2019

Preprint

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In this paper some recent results from the Pierre Auger Collaboration are presented. These are the measurement of the energy spectrum of cosmic rays over a wide range of energies (10 17.5 to above 10 20 eV), studies of the cosmic-ray mass composition with the fluorescence and surface detector of the Observatory, the observation of a large-scale anisotropy in the arrival direction of cosmic rays above 8 × 10 18 eV and indications of anisotropy at intermediate angular scales above 4 × 10 19 eV. The astrophysical implications of the spectrum and composition results are also discussed. Finally the progress of the upgrade of the Observatory, AugerPrime is presented.

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“…However, especially these mass measurements suffer from relatively low statistics and large uncertainties for E 40 EeV. The planned upgrade of the Pierre Auger Observatory [10] will be able to provide significant improvements in that respect.…”

Section: Introductionmentioning

confidence: 99%

Extragalactic Sources and Propagation of UHECRs

Vliet

Batista

Sigl

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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With the publicly available astrophysical simulation framework for propagating extraterrestrial UHE particles, CRPropa 3, it is now possible to study realistic UHECR source scenarios including deflections in Galactic and extragalactic magnetic fields in an efficient way. Here we discuss three recent studies that have already been done in that direction. The first one investigates what can be expected in the case of maximum allowed intergalactic magnetic fields. Here is shown that, even if voids contain strong magnetic fields, deflections of protons with energies ≳ 60 EeV from nearby sources might be small enough to allow for UHECR astronomy. The second study looks into several scenarios with a smaller magnetization focusing on large-scale anisotropies. Here is shown that the local source distribution can have a more significant effect on the large-scale anisotropy than the EGMF model. A significant dipole component could, for instance, be explained by a dominant source within 5 Mpc distance. The third study looks into whether UHECRs can come from local radio galaxies. If this is the case it is difficult to reproduce the observed low level of anisotropy. Therefore is concluded that the magnetic field strength in voids in the EGMF model used here is too low and/or there are additional sources of UHECRs that were not taken into account in these simulations.

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The Pierre Auger Observatory Upgrade - Preliminary Design Report

Cited by 96 publications

References 0 publications

Probing hadronic interactions with the Pierre Auger Observatory

Probing hadronic interactions with the Pierre Auger Observatory

Recent results from the Pierre Auger Observatory

Extragalactic Sources and Propagation of UHECRs

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