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Future ground arrays for ultrahigh-energy cosmic rays: recent updates and perspectives

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Figure

Figure 1. Schematic view of arrays of detectors and large-field-of-view fluorescence telescopes, detecting signals from EAS in-duced by UHECRs [https://www.auger.org].
Figure 2. Overview of three important observables reported by the Pierre Auger Observatory and Telescope Array Experiment: energyspectrum [6–8] mass composition [9–11] and arrival direction [12–15] with energy ranges indicated above: 8 EeV (red), 57 EeV (blue)and 100 EeV (green).
Figure 3. Ongoing upgrades of AugerPrime (left) [19] and TAcomposition using a measurement of the number of muons×4 (right)[20]
Figure 4. The UHECR observatories and their exposures at the highest energies as a function of time; including AGASA [29], HighResolution Fly’s Eye [30], Auger [16], TA [17, 18]
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