Auger@TA: In-situ Cross-Calibration of the World's Largest Cosmic Ray Observatories
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arXiv
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| Natura: | Preprint |
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2025
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| author | Mocellin, Adriel G B Caraça-Valente, J. Covault, C. Dalcan, E. Fujii, T. Im, S. James, R. Johnsen, J. Kampert, K. H. Kern, H. Matthews, J. N. Mayotte, E. Mayotte, S. Moskala, X. Que, H. Rautenberg, J. Roth, M. Sagawa, H. Sako, T. Sarazin, F. Sato, R. Schmidt, D. Thomas, S. B. Wörner, G. |
| author_facet | Mocellin, Adriel G B Caraça-Valente, J. Covault, C. Dalcan, E. Fujii, T. Im, S. James, R. Johnsen, J. Kampert, K. H. Kern, H. Matthews, J. N. Mayotte, E. Mayotte, S. Moskala, X. Que, H. Rautenberg, J. Roth, M. Sagawa, H. Sako, T. Sarazin, F. Sato, R. Schmidt, D. Thomas, S. B. Wörner, G. |
| contents | The Pierre Auger Observatory (Auger) and the Telescope Array (TA) are the world's two largest ultra-high-energy cosmic ray (UHECR) observatories. They operate in the Southern and Northern hemispheres, respectively, at similar latitudes but with distinct surface detector (SD) designs. A significant challenge in studying UHECR physics across the full sky is the apparent discrepancy in flux measurements between the two experiments. This discrepancy could arise from astrophysical differences and/or systematic effects related to their detector designs and sensitivities to extensive air shower components. To address this, the Auger@TA working group aims to cross-calibrate the two observatories with a self-triggering micro-Auger array within the TA array. This micro-array consists of eight Auger Surface Detector (SD) stations equipped with Water Cherenkov Detectors (WCDs) and AugerPrime Surface Scintillator Detectors. Seven SD stations, configured with a centered-1-PMT design, are arranged in a hexagonal pattern with one station in the center, with 1.5 km spacing, mirroring the Auger layout. The eighth station, which features a standard 3-PMT Auger station, is located in conjunction with a TA detector at the center of the hexagon, forming a triplet for high-statistics and low-uncertainty cross-calibration. A custom communication system that uses readily available components enables seamless communication between stations and remote access to each station through a central computer. The micro-array is now fully deployed, and initial data-taking is about to start. This presentation will detail the instrumentation, communication systems, central data acquisition system, expected performance of the micro-array, and preliminary results as appropriate. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_20911 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Auger@TA: In-situ Cross-Calibration of the World's Largest Cosmic Ray Observatories Mocellin, Adriel G B Caraça-Valente, J. Covault, C. Dalcan, E. Fujii, T. Im, S. James, R. Johnsen, J. Kampert, K. H. Kern, H. Matthews, J. N. Mayotte, E. Mayotte, S. Moskala, X. Que, H. Rautenberg, J. Roth, M. Sagawa, H. Sako, T. Sarazin, F. Sato, R. Schmidt, D. Thomas, S. B. Wörner, G. High Energy Astrophysical Phenomena Instrumentation and Methods for Astrophysics High Energy Physics - Phenomenology The Pierre Auger Observatory (Auger) and the Telescope Array (TA) are the world's two largest ultra-high-energy cosmic ray (UHECR) observatories. They operate in the Southern and Northern hemispheres, respectively, at similar latitudes but with distinct surface detector (SD) designs. A significant challenge in studying UHECR physics across the full sky is the apparent discrepancy in flux measurements between the two experiments. This discrepancy could arise from astrophysical differences and/or systematic effects related to their detector designs and sensitivities to extensive air shower components. To address this, the Auger@TA working group aims to cross-calibrate the two observatories with a self-triggering micro-Auger array within the TA array. This micro-array consists of eight Auger Surface Detector (SD) stations equipped with Water Cherenkov Detectors (WCDs) and AugerPrime Surface Scintillator Detectors. Seven SD stations, configured with a centered-1-PMT design, are arranged in a hexagonal pattern with one station in the center, with 1.5 km spacing, mirroring the Auger layout. The eighth station, which features a standard 3-PMT Auger station, is located in conjunction with a TA detector at the center of the hexagon, forming a triplet for high-statistics and low-uncertainty cross-calibration. A custom communication system that uses readily available components enables seamless communication between stations and remote access to each station through a central computer. The micro-array is now fully deployed, and initial data-taking is about to start. This presentation will detail the instrumentation, communication systems, central data acquisition system, expected performance of the micro-array, and preliminary results as appropriate. |
| title | Auger@TA: In-situ Cross-Calibration of the World's Largest Cosmic Ray Observatories |
| topic | High Energy Astrophysical Phenomena Instrumentation and Methods for Astrophysics High Energy Physics - Phenomenology |
| url | https://arxiv.org/abs/2510.20911 |