The JEM-EUSO Program for UHECR Studies from Space

Parizot, E.; Casolino, M.; Picozza, P.; Ebisuzaki, Toshikazu; Bertaina, M.; Fuglesang, C.; Haungs, A.; Kajino, F.; Климов, П. А.; Olinto, Angela V.; Ricci, M.; Sagawa, H.; Szabelski, J.; Wiencke, L.

doi:10.1051/epjconf/202328306007

Cited by 6 publications

(2 citation statements)

References 30 publications

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“…The ultimate goal of the JEM-EUSO program [9] is the detection and reconstruction of UHE-CRs from space with improved statistics with respect to the current generation of UHECR detectors. In this framework, Mini-EUSO has proved to be an invaluable instrument to address the detection capability of a future, larger space-based detector, like the future POEMMA [3].…”

Section: Discussionmentioning

confidence: 99%

Analysis of EAS-like events detected by the Mini-EUSO telescope

Battisti,

Bertaina,

Arnone

et al. 2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

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The Mini-EUSO telescope is the first space-based detector of the JEM-EUSO program. It was launched for the International Space Station on August 22 𝑛𝑑 , 2019 to observe from the ISS orbit (∼420 km altitude) various phenomena occurring in the Earth's atmosphere through a UVtransparent window located in the Russian Zvezda Module. The dimension of the window defines and constrains the dimension of the optics, based on a set of two Fresnel lenses of 25 cm diameter each, almost two orders of magnitude smaller than the system foreseen for a larger space-based detector, like the original JEM-EUSO detector or the future POEMMA. As a consequence, the energy threshold of Mini-EUSO is very high, above 10 21 eV. Nevertheless, a series of events that resemble the shape and the time duration of EAS-induced events have been detected in Mini-EUSO data. This contribution presents the most interesting cases, showing that the vast majority of the EAS-like events can be traced back to ground sources repeatedly flashing and triggered many times by Mini-EUSO. Some non-repeated EAS-like events are also present. In these cases, it is possible to exclude their cosmic origin through the comparison with simulated events. Since it is clear that those events can not be originated by a UHECR, we decided to rename them "Short Light Transients" or SLTs. Finally, it was possible to associate some of the SLTs with atmospheric activity. This analysis confirms the validity of the JEM-EUSO detection principle and shows that it is possible for a space-based detector to distinguish between events induced by UHECRs and events with a different origin.

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Section: Discussionmentioning

confidence: 99%

Analysis of EAS-like events detected by the Mini-EUSO telescope

Battisti,

Bertaina,

Arnone

et al. 2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

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“…The Joint Exploratory Missions for an Extreme Universe Space Observatory (JEM-EUSO) Program [7] consists of a series of telescopes and experiments operated on the ground (EUSO-TA [8]), on stratospheric balloons (EUSO-Balloon [9], EUSO-SPB1 [10], and EUSO-SPB2 [11]), and in the space inside the International Space Station (ISS-Mini-EUSO [12]). They all contribute in growing the knowledge and extending the capability to develop the technology to detect Ultra-High Energy Cosmic Rays (UHECRs) from space (aboard orbiting satellites) by observing the fluorescence and Cherenkov light emitted during their path through the Earth's atmosphere and the Cherenkov emission from Earth skimming neutrinos.…”

Section: Introductionmentioning

confidence: 99%

Use of Silicon Photomultipliers in the Detectors of the JEM-EUSO Program

Bisconti

2023

Instruments

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The JEM-EUSO program aims to study ultra-high energy cosmic rays from space. To achieve this goal, it has realized a series of experiments installed on the ground (EUSO-TA), various on stratospheric balloons (with the most recent one EUSO-SPB2), and inside the International Space Station (Mini-EUSO), in light of future missions such as K-EUSO and POEMMA. At nighttime, these instruments aim to monitor the Earth’s atmosphere measuring fluorescence and Cherenkov light produced by extensive air showers generated both by very high-energy cosmic rays from outside the atmosphere and by neutrino decays. As the two light components differ in duration (order of microseconds for fluorescence light and a few nanoseconds for Cherenkov light) they each require specialized sensors and acquisition electronics. So far, the sensors used for the fluorescence camera are the Multi-Anode Photomultiplier Tubes (MAPMTs), while for the Cherenkov one, new systems based on Silicon PhotoMultipliers (SiPMs) have been developed. In this contribution, a brief review of the experiments is followed by a discussion of the tests performed on the optical sensors. Particular attention is paid to the development, test, and calibration conducted on SiPMs, also in view to optimize the geometry, mass, and weight in light of the installation of mass-critical applications such as balloon- and space-borne instrumentation.

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