The depth of the shower maximum of air showers measured with AERA

Pont, Bjarni; Abreu, Pedro; Aglietta, M.; Albury, Justin M.; Allekotte, I.; Almela, A.; Álvarez-Muñiz, J.; Batista, Rafael Alves; Anastasi, Gioacchino Alex; Anchordoqui, Luis A.; Andrada, Belén; Andringa, S.; Aramo, C.; Ferreira, Paulo Ricardo Araújo; Velázquez, Juan Carlos Arteaga; Asorey, H.; Assis, P.; Ávila, G.; Badescu, Alina Mihaela; 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.; Binet, Virginia; Bismark, Kathrin; Bister, Teresa; Biteau, J.; Blažek, Jiří; Bleve, C.; Bohã̌cov́a, M.; Boncioli, D.; Bonifazi, C.; Arbeletche, Luan Bonneau; Borodai, N.; Botti, Ana Martina; Brack, Jeffrey; Bretz, T.; Orchera, P. Gabriel Brichetto; Briechle, Florian Lukas; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, Mario; Büsken, Max; Caballero-Mora, K. S.; Caccianiga, Lorenzo; Canfora, F.; Caracas, Ioana; Carceller, Juan Miguel; Caruso, R.; Castellina, A.; Catalani, Fernando; Cataldi, G.; Cazón, L.; Cerda, Marcos; Chinellato, J.; 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; Santos, Diego Correia dos; Covault, C. E.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Day, Jarryd A.; Almeida, R. M. de; Jesús, Joaquín de; Jong, Sijbrand J. de; Mauro, G. De; Neto, João de Mello; Mitri, I. De; Oliveira, Jaime de; Franco, D.; Palma, F. de; Souza, Vítor de; Vito, Emanuele De; Río, Mariano del; Deligny, O.; Deval, Luca; Matteo, Armando di; Dobrigkeit, C.; D’Olivo, Juan Carlos; Mendes, Luis Miguel Domingues; Anjos, Rita dos; Santos, Diego dos; Dova, M. T.; Ebr, Jan; Engel, R.; Epicoco, Italo; Erdmann, M.; Escobar, C.; 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.; Fitoussi, Thomas; 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.; Glombitza, Jonas; Gobbi, Fabian; Gollan, Fernando; Golup, G.; Berisso, M. Gómez; Vitale, Primo F. Gómez; Gongora, Juan Pablo; González, Juan Manuel; González, Nicolás Martín; Goos, Isabel; Góra, Dariusz; Gorgi, A.; Gottowik, Marvin; Grubb, Trent D.; Guarino, F.; Guedes, G. P.; Guido, Eleonora; Hahn, Steffen; Hamal, P.; Hampel, Matías Rolf; Hansen, Patricia María; 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.; Insolia, A.; Isar, P. G.; Janeček, Petr; Johnsen, Jeffrey A.; Jurýšek, Jakub; Kääpä, Alex; Kampert, Karl-Heinz; Karastathis, N.; Keilhauer, B.; Kemp, J.; Khakurdikar, Abha; Covilakam, Varada Varma Kizakke; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Köpke, Marcel; Kunka, Norbert; Lago, Bruno L.; Lang, Rodrigo Guedes; Langner, Niklas; Oliveira, Marcelo Augusto Leigui de; Lenok, Vladimir; Letessier‐Selvon, A.; Lhenry-Yvon, I.; Presti, Domenico Lo; Lopes, L.; López, Rebeca; Lu, Lu; Luce, Quentin; Lundquist, Jon Paul; Payeras, Allan Machado; Mancarella, G.; Mandát, Dušan; Manning, Bradley C.; Manshanden, Julien; Mantsch, P.; Marafico, Sullivan; Mariazzi, Analisa; Maris, Ioana Codrina; Marsella, G.; Martello, D.; Martinelli, Sara; Bravo, O. Martínez; Mastrodicasa, Massimo; Mathes, H. J.; Matthews, James; Matthiae, G.; Mayotte, E.; Mazur, Péter; Medina‐Tanco, G.; Melo, D.; Menshikov, Alexander; Merenda, Kevin-Druis; Michal, Stanislav; Micheletti, M. 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C.; Ruehl, Philip; Sǎftoiu, A.; Salamida, F.; Salazar, H.; Salina, G.; Gomez, Jose 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, David; Scholten, Olaf; Schovánek, Petr; Schröder, Frank G.; Schröder, Sonja; Schulte, Josina; Sciutto, S. J.; Scornavacche, Marina; Segreto, A.; Sehgal, Srijan; 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.; Szadkowski, Z.; Tapia, A.; Taricco, Carla; Timmermans, C.; Tkachenko, Olena; Tobiška, Petr; Peixoto, C. J. Todero; Tomé, B.; Torrès, Zoé; Travaini, Andres; Trávničék, P.; Trimarelli, Caterina; Tueros, M.; Ulrich, R.; Unger, Michael; Vaclavek, Lukáš; Vacula, Martin; Galicia, J. F. Valdés; Valore, L.; Varela, E.; Vásquez-Ramírez, Adriana; Veberič, D.; Ventura, Cynthia; Quispe, Indira D. Vergara; Verzi, V.; Vícha, J.; Vink, Jacco; Vorobiov, S.; Wahlberg, H.; Watanabe, Clara Keiko Oliveira; Watson, Alan; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński, H.; Wirtz, Marcus; Wittkowski, David; Wundheiler, B.; Yushkov, A.; Zapparrata, Orazio; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zehrer, Lukas

doi:10.22323/1.395.0387

Cited by 8 publications

(13 citation statements)

References 4 publications

(5 reference statements)

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“…The low-energy enhancements TALE [142] of TA and HEAT [53] of Auger measure the X max of FD events which reach their points of maximum shower development high in the atmosphere. The radio arrays AERA [179], LOFAR [180], Tunka-Rex [181],…”

Section: Primary Composition: 100 Pev-1 Eevmentioning

confidence: 99%

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Coleman,

Eser,

Mayotte

et al. 2022

Preprint

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Pin down the shower energy observable to use μ as a composition-only Reduce hadronic uncertainties interaction model E threshold (TBD) Other messengers Galactic * μ / em separation † * depending on analysis progress † depending on detector configuration• At least one next-generation experiment needs to be able to make high-precision measurements to explore new particle physics and measure particle rigidity on an event-by-event basis. Of the planned next-generation experiments, GCOS is the best positioned to meet this recommendation.• As a complementary effort, experiments with sufficient exposure ( 5 × 10 5 km 2 sr yr) are needed to search for Lorentz-invariance violation (LIV), SHDM, and other BSM physics at the Cosmic and Energy Frontiers, and to identify UHECR sources at the highest energies.• Full-sky coverage with low cross-hemisphere systematic uncertainties is critical for astrophysical studies. To this end, next generation experiments should be space-based or multi-site. Common sites between experiments are encouraged.• Based on the productive results from inter-collaboration and inter-disciplinary work, we recommend the continued progress/formation of joint analyses between experiments and with other intersecting fields of research (e.g., magnetic fields).• The UHECR community should continue its efforts to advance diversity, equity, inclusion, and accessibility. It also needs to take steps to reduce its environmental impacts and improve open access to its data to reduce the scientific gap between countries.vi

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Section: Primary Composition: 100 Pev-1 Eevmentioning

confidence: 99%

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Coleman,

Eser,

Mayotte

et al. 2022

Preprint

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“…Built on the experience gained with the construction and operation of the Auger Engineering Radio Array [695], the goal is to install an antenna on top of each WCD to detect the radio signal induced in EAS by geomagnetic charge separation in the shower [696] and the Askaryan effect [577]. The RD is most efficient for the detection of inclined showers [697], and the radio footprint at ground is known to contain information on X max [698], the depth at which the shower reaches the maximum in its development. The RD will provide a clean measurement of the electromagnetic shower component, ideal to separate neutrino-induced cascades from hadronic showers.…”

Section: Gcosmentioning

confidence: 99%

High-Energy and Ultra-High-Energy Neutrinos

Ackermann,

Agarwalla,

Alvarez-Muñiz

et al. 2022

Preprint

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Astrophysical neutrinos are excellent probes of astroparticle physics and high-energy physics. With energies far beyond solar, supernovae, atmospheric, and accelerator neutrinos, high-energy and ultrahigh-energy neutrinos probe fundamental physics from the TeV scale to the EeV scale and beyond. They are sensitive to physics both within and beyond the Standard Model through their production mechanisms and in their propagation over cosmological distances. They carry unique information about their extreme non-thermal sources by giving insight into regions that are opaque to electromagnetic radiation. This white paper describes the opportunities astrophysical neutrino observations offer for astrophysics and high-energy physics, today and in coming years.Fully opening the HE and UHE neutrino windows requires a multi-pronged approach that explores a broad range of proposed experimental techniques. With upcoming neutrino telescopes, the goal is to improve the sensitivity ten-fold in the HE range and hundred-fold in the UHE range. In the HE range, we are moving into the high-statistics era, where subtle features may be resolved and multiple sources may be discovered. In the UHE range, neutrino flux predictions and physics tests are well-motivated, but we will likely need new techniques to enable discoveries. The ongoing efforts to develop new instruments will improve sensitivity, increase statistics, and expand the energy range. A broad range of experimental approaches, with complementary capabilities, must be developed and tested in the coming decades. Because it is not clear which techniques will prevail, we advocate for a broad portfolio of experiments in the HE and UHE neutrino sector. Owing to their potential, HE and UHE neutrinos should be at the forefront of the high-energy physics program, as they push the boundaries for the neutrino, cosmic, energy, theory, and instrumentation frontiers. 4 Experimental landscape 32 4.1 Overview 32 4.2 High-energy range 35 4.3 Ultra-High Energy Range (> 100-PeV) 45

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“…X max (left) and its standard deviation (right) measured by various experiments, among them a few radio arrays. The possible tension between LOFAR [34] and Auger [35] is under investigation by a joint working group (courtesy of Bjarni Pont [36]). absolute energy scales of different cosmic-ray observatories [32,33].…”

Section: Energymentioning

confidence: 99%

“…Today, this is the largest radio array dedicated to cosmic-ray detection. Planned as an engineering array, several antenna types and data-acquisition systems have been tested, and a number of pioneering analyses have been performed, e.g., on energy [59] and X max reconstruction [35] including a thorough study of systematic uncertainties. As a result, the accuracy can compete with the fluorescence telescopes.…”

Section: Radio Detection At the Pierre Auger Observatorymentioning

confidence: 99%

Digital Radio Arrays for the Detection of Air Showers Initiated by Ultra-High-Energy Particles (Epiphany 2022)

Schröder¹

2022

Preprint

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Digital radio arrays have become an effective tool to measure air showers at energies around and above 100 PeV. Compared to optical techniques, the radio technique is not restricted to clear nights. Thanks to recent progress on computational analysis techniques, radio arrays can provide an equally accurate measurement of the energy and the depth of the shower maximum. Stand-alone radio arrays offer an economic way towards huge apertures, e.g., for the search for ultra-high-energy neutrinos, but still require technical demonstration on large scales. Hybrid arrays combining radio antennas and particle detectors have already started to contribute to cosmic-ray physics in the energy range of the presumed Galactic-toextragalactic transition. In particular, the combination of radio and muon detectors can pave a path to unprecedented accuracy for the mass composition of cosmic rays. This proceeding reviews recent developments regarding the radio technique and highlights selected running and planned antennas arrays, such as GCOS, GRAND, the SKA, the AugerPrime Upgrade of the Pierre Auger Observatory, and IceCube-Gen2.

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The depth of the shower maximum of air showers measured with AERA

Abstract: The depth of the shower maximum of air showers measured with AERA Bjarni Pont , * on behalf of the Pierre Auger Collaboration

Cited by 8 publications

References 4 publications

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers

High-Energy and Ultra-High-Energy Neutrinos

Digital Radio Arrays for the Detection of Air Showers Initiated by Ultra-High-Energy Particles (Epiphany 2022)

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