Performance and air-shower reconstruction techniques for the JEM-EUSO mission

Bertaina, M.; Biktemerova, S.; Bittermann, K.; Bobík, P.; Campana, D.; Fenu, Francesco; Gorgi, A.; Guarino, F.; Guzmán, A.; Higashide, K.; Medina‐Tanco, G.; Mernik, T.; Naumov, D.; Putiš, M.; Frías, Rodríguez; Sáez-Cano, G.; Santangelo, A.; Shinozaki, K.; Toscano, S.

doi:10.1016/j.asr.2014.02.018

Cited by 20 publications

(15 citation statements)

References 33 publications

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“…Several algorithms have been developed for this purpose. In this work, two have been used, namely the LTTPatternRecognition and the PWISE algorithms [11,13]. A detailed discussion of the two algorithms is out of the scope of this publication but both of them are looking for signal excesses concentrated in space and moving in a coherent way.…”

Section: Energy and X Max Reconstructionmentioning

confidence: 99%

“…The procedure is used for a first estimate of the shower parameters, like energy and X max . The method, already described in [11], has been significantly improved and, therefore, a detailed description of the algorithms has been done. A schematic view of this algorithm is given in Fig.…”

Section: Energy and X Max Reconstructionmentioning

confidence: 99%

“…13 of [14] the dependence of the angular reconstruction from the position in the field of view is reported (Table 1). 11 The radial distance of a spot on the focal surface as function of the radial distance of a source in the field of view. Such distances are respectively measured in mm and km.…”

Section: Energy and X Max Reconstructionmentioning

confidence: 99%

See 2 more Smart Citations

Performances of JEM–EUSO: energy and X max reconstruction

Adams¹,

Ahmad²,

Albert³

et al. 2015

Exp Astron

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by a large international collaboration, is designed to be launched within this 11 decade. In this article, we present the reconstruction of the energy of the 12 observed events and we also address the X max reconstruction. After discussing 13 the algorithms developed for the energy and X max reconstruction, we present such an energy range, and will unveil the sources of UHE cosmic rays and 10 the mechanisms of their production. JEM-EUSO is also being designed to 11 explore the neutrino and photon flux at UHE and, therefore, the discrimination 12 capability of the mission for these particles, with respect to charged UHECRs, of 3×3 mm size, covering a field of view on ground of roughly 500 × 500 m. 21The detector therefore consists of more than 3 · 10 5 pixels, which cover a field 22 of view of 500 km diameter. The structure of the focal surface can be seen in of the instrument, we refer the reader to [5], [6], [7]. For each observed event, 4 the arrival time, arrival direction, energy, and X max must be reconstructed to 5 recover the full observational information. 6In this paper, we present the algorithms developed to reconstruct the en-7 ergy and X max parameters for events observed by JEM-EUSO. These studies instrument and has been used in the present study. 222 Energy and X max reconstruction 23The PmtToShowerReco is the energy and X max reconstruction procedure de-24 veloped to reconstruct events observed by JEM-EUSO. The reconstruction is 25 structured in several subsequent steps, each of which performing a sub-task. 26The procedure is used for a first estimate of the shower parameters, like en-27 ergy and X max . The method, already described in [9], has been significantly 28 improved and, therefore, a detailed description of the algorithms has been 29 done. A schematic view of this algorithm is given in Fig. 2. 31The signal track selection 32The PmtToShowerReco receives the information in input on the timing and 33 position for all the counts detected on the focal surface. For the analysis we 34 only consider triggered events since this is the condition for data to be sent 35 to ground. More details on the trigger logic can be found in [10]. The PDMs 36 associated with a trigger (and neighboring PDMs) will therefore be sent to 37 ground. In Fig. 3, an example of simulated data received from the instrument 38 can be seen, including both signal and background. This is representing a 39shower event of 3·10 20 eV and 50 degrees zenith angle. At regular intervals, the 40shower spot crosses the PMTs gaps perpendicularly and, therefore, a decrease 41 in the detected intensity has to be expected. In Fig. 4, the counts detected The JEM-EUSO Collaboration we only see the counts that originated from the shower unlike in Fig. 3. The This particular shower is, therefore, clearly evolving to the right of the image 10 for a time duration of roughly 50 GTUs. 11The first task of the reconstruction must be the identification of the pixels 12and GTUs with signal. Several algorithms have been developed for this pur- is o...

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Section: Energy and X Max Reconstructionmentioning

confidence: 99%

Section: Energy and X Max Reconstructionmentioning

confidence: 99%

See 1 more Smart Citation

Performances of JEM–EUSO: energy and X max reconstruction

Adams¹,

Ahmad²,

Albert³

et al. 2015

Exp Astron

Self Cite

View full text Add to dashboard Cite

show abstract

“…According to other simulations, Cherenkov light, either reflected from Earth or generated within the mirror medium by an upward-going particle can also potentially generate instant flashes with a spot produced in the focal plane [24,25]. The probability of this kind of events is small, but its importance calls for a dedicated analysis.…”

Section: Instant Track-like Flashesmentioning

confidence: 99%

Early Results from TUS, the First Orbital Detector of Extreme Energy Cosmic Rays

Zotov

2018

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

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TUS is the world's first orbital detector of extreme energy cosmic rays (EECRs), which operates as a part of the scientific payload of the Lomonosov satellite since May 19, 2016. TUS employs the nocturnal atmosphere of the Earth to register ultraviolet (UV) fluorescence and Cherenkov radiation from extensive air showers generated by EECRs as well as UV radiation from lightning strikes and transient luminous events, micro-meteors and space debris. The first months of its operation in orbit have demonstrated an unexpectedly rich variety of UV radiation in the atmosphere. We briefly review the design of TUS and present a few examples of events recorded in a mode dedicated to registering EECRs.

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“…One goal of the mission was to demonstrate the capability of the instrument to measure the UV background from space under various conditions to better estimate the performance of the planned JEM-EUSO space-based UHECR telescope (see [6]). Given the short data taking time and EUSO-Balloon's energy threshold for cosmic-ray shower detection around 10 18 eV, no actual cosmic-ray detection was expected.…”

Section: Introductionmentioning

confidence: 99%

Search for significant background fluctuations in the EUSO-Balloon data

Jung¹,

Parizot²,

Suino³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The EUSO-Balloon instrument recorded data during a stratospheric flight in August 2014, to measure the UV background during a moonless night, from an altitude of ∼ 38 km, with a field of view of ±5.5 • . In this paper, we report on the search for coherent fluctuations of this background over areas ranging from ∼ 1 km 2 up to the entire field of view, on timescales from a few µs to ∼ 100 µs. In addition to the expected laser track events induced by shootings from a helicopter flying in the field-of-view of EUSO-Balloon during part of the mission, three unidentified and significant events, probably related to human activity, are discussed.

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Performance and air-shower reconstruction techniques for the JEM-EUSO mission

Cited by 20 publications

References 33 publications

Performances of JEM–EUSO: energy and X max reconstruction

Performances of JEM–EUSO: energy and X max reconstruction

Early Results from TUS, the First Orbital Detector of Extreme Energy Cosmic Rays

Search for significant background fluctuations in the EUSO-Balloon data

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