The current status of orbital experiments for UHECR studies

Panasyuk, M. I.; Casolino, M.; Garipov, G.; Ebisuzaki, Toshikazu; Gorodetzky, P.; Khrenov, B. A.; Климов, П. А.; Morozenko, V. S.; Sakaki, N.; Saprykin, O.; Sharakin, S.; Takizawa, Y.; Ткачев, Л.; Yashin, I. V.; Zotov, M. Yu.

doi:10.1088/1742-6596/632/1/012097

Cited by 18 publications

(22 citation statements)

References 46 publications

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“…To eliminate the off-axis aberration an additional corrective element was introduced into the telescope system in form of a Fresnel lens in front of the photodetector. Two versions of the detector were developed: Baseline and Mylti-Eye Telescope System (METS) [9,10]. 1 1 EeV = 10 18 eV 2 KLYPVE is a Russian acronym for extreme energy cosmic rays.…”

Section: From Klypve To K-eusomentioning

confidence: 99%

Status of the KLYPVE-EUSO detector for EECR study on board the ISS

Климов¹,

Casolino²

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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For the JEM-EUSO CollaborationKLYPVE-EUSO is a mission led by the Russian Space Agency to place an ultra-high energy cosmic ray observatory on board the Russian Segment (RS) of the ISS. The concept of the detector is based on the mirror-type detector proposed by SINP MSU in 2010 and improved by the joint studies with the JEM-EUSO collaboration. The current configuration is based on a Schmidt type optical system. This allows to increase the Field of View to 40 degrees and makes the experiment competitive with large ground-based observatories, with the advantage of the uniform exposure over the whole celestial sphere. The laboratory models of mirror-concentrator and photo detector module are being developed and manufactured. The launch of the experiment is scheduled to 2022 followed by the installation on the RS of the ISS and at least two years of operation.

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Section: From Klypve To K-eusomentioning

confidence: 99%

Status of the KLYPVE-EUSO detector for EECR study on board the ISS

Климов¹,

Casolino²

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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“…It was estimated by Olinto et al (2015) that with the annual exposure ∼ 5 × 10 4 km 2 sr above ∼ 60 EeV, JEM-EUSO will collect 429 events/yr, or about 2,145 events in 5 years. KLYPVE will have the annual exposure ∼ 1.2 × 10 4 km 2 sr above 50 EeV (Panasyuk et al 2015;Sakaki et al 2015) and thus will be able to detect more than 100 events every year of operation, and more than 600 events during its planned lifetime. It was concluded that with its huge annual exposure (almost an order of magnitude larger than that of the Pierre Auger Observatory) and the planned 5-year operation time, JEM-EUSO has excellent opportunities for confirming the existence of the TA hotspot at high confidence level.…”

Section: Scientific Backgroundmentioning

confidence: 99%

“…GRBs are believed to be sources of ultra-high energy cosmic rays (UHECR) (Waxman 2006;Abu-Zayyad et al 2012;Tokuno et al 2012;Abraham et al 2004;Panasyuk et al 2012;Takahashi 2009;Halzen and Klein 2010;Gorham et al 2009) and gravitational waves (GW) whose detection has been reported recently (Cutler and Thorne 2002;Abramovici et al 1992;Abbott et al 2016a), and is a prime example of multi-messenger astronomy. The rapid-response in the observation of electromagnetic counterparts to GW (Abbott et al 2016b) is important to obtain the rich information in physical processes of GRBs giving rise to each messenger and the time delay between them.…”

Section: Scientific Backgroundmentioning

confidence: 99%

“Lomonosov” Satellite—Space Observatory to Study Extreme Phenomena in Space

et al. 2017

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V. A. Sadovnichii et al. zations to study some of extreme phenomena in space related to astrophysics, astroparticle physics, space physics, and space biology. The primary goals of this experiment are to study: -Ultra-high energy cosmic rays (UHECR) in the energy range of the Greizen-ZatsepinKuzmin (GZK) cutoff; -Ultraviolet (UV) transient luminous events in the upper atmosphere; -Multi-wavelength study of gamma-ray bursts in visible, UV, gamma, and X-rays; -Energetic trapped and precipitated radiation (electrons and protons) at low-Earth orbit (LEO) in connection with global geomagnetic disturbances; -Multicomponent radiation doses along the orbit of spacecraft under different geomagnetic conditions and testing of space segments of optical observations of space-debris and other space objects; -Instrumental vestibular-sensor conflict of zero-gravity phenomena during space flight. This paper is directed towards the general description of both scientific goals of the project and scientific equipment on board the satellite. The following papers of this issue are devoted to detailed descriptions of scientific instruments.

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“…GRBs are potential candidates of the next generation cosmological standard candles (Lipunov et al 2001;Amati et al 2008;Ghirlanda et al 2006;Panaitescu and Vestrand 2008); and they are also prime examples for multimessenger astrophysical observation because their direct photon measurements can be augmented through observations of the air showers that result from the entry of their ultra-highenergy cosmic ray (UHECR) particles into the atmosphere (e.g. TA (Abu-Zayyad et al 2012;Tokuno et al 2012), Auger (Abraham et al 2004), TUS (Panasyuk et al 2015), JEM-EUSO (Takahashi 2009)), of neutrinos (e.g. ICECUBE (Halzen and Klein 2010), ANITA (Gorham et al 2009)), and searches for GW (e.g.…”

Section: Introductionmentioning

confidence: 99%

Wide-Field Gamma-Spectrometer BDRG: GRB Monitor On-Board the Lomonosov Mission

et al. 2017

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The study of GRB prompt emissions (PE) is one of the main goals of the Lomonosov space mission. The payloads of the GRB monitor (BDRG) with the widefield optical cameras (SHOK) and the ultra-fast flash observatory (UFFO) onboard the Lomonosov satellite are intended for the observation of GRBs, and in particular, their prompt emissions. The BDRG gamma-ray spectrometer is designed to obtain the temporal and spectral information of GRBs in the energy range of 10-3000 keV as well as to provide GRB triggers on several time scales (10 ms, 1 s and 20 s) for ground and space telescopes, including the UFFO and SHOK. The BDRG instrument consists of three identical detector boxes with axes shifted by 90 • from each other. This configuration allows us to localize a GRB source in the sky with an accuracy of ∼ 2 • .Each BDRG box contains a phoswich NaI(Tl)/CsI(Tl) scintillator detector. A thick CsI(Tl) crystal in size of ∅130 × 17 mm is placed underneath the NaI(Tl) as an active shield in the soft energy range and as the main detector in the hard energy range. The ratio of the CsI(Tl) to NaI(Tl) event rates at varying energies can be employed as an independent metric to distinguish legitimate GRB signals from false positives originating from electrons in near-Earth vicinities.The data from three detectors are collected in a BA BDRG information unit, which generates a GRB trigger and a set of data frames in output format. The scientific data output is ∼ 500 Mb per day, including ∼ 180 Mb of continuous data for events with durations in excess of 100 ms for 16 channels in each detector, detailed energy spectra, and sets of frames with ∼ 5 Mb of detailed information for each burst-like event. A number of pre-flight tests including those for the trigger algorithm and calibration were carried out to confirm the reliability of the BDRG for operation in space.

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The current status of orbital experiments for UHECR studies

Abstract: 4 A discussion of the Super-EUSO [48] and OWL [49] missions goes beyond the scope of the article. 5 See http://euso-balloon.lal.in2p3.fr

Cited by 18 publications

References 46 publications

Status of the KLYPVE-EUSO detector for EECR study on board the ISS

Status of the KLYPVE-EUSO detector for EECR study on board the ISS

“Lomonosov” Satellite—Space Observatory to Study Extreme Phenomena in Space

Wide-Field Gamma-Spectrometer BDRG: GRB Monitor On-Board the Lomonosov Mission

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