Event-by-event study of CR composition with the SPHERE experiment using the 2013 data

Antonov, R. A.; Aulova, T. V.; Bonvech, E. A.; Чернов, Д. В.; Dzhatdoev, T.; Finger, M.; Finger, M.; Галкин, В. И.; Подгрудков, Д.; Роганова, Т. М.

doi:10.1088/1742-6596/632/1/012090

Cited by 10 publications

(27 citation statements)

References 8 publications

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“…In [42] we show that about 40 % of protons could be selected vs. Nitrogen nuclei at 10 PeV, 0-20 • zenith angle range, 400 m observation altitude (with 1 % contamination of Nitrogen). This quantity is representative for the selection performance of the light component.…”

Section: Uncertainty Of the Spectrum Of Light Nucleimentioning

confidence: 82%

“…Thus, the relative statistical uncertainty would be ǫ Stat ≈ 1/ √ N sel ≈ 0.07. The dominant systematic uncertainties are: 1) The spread of the primary energy for the light component nuclei vs. the primary composition ǫ E−Syst ≈ 1-3 % [42] (see below for more details). ǫ E−Syst is effectively the relative difference of mean reconstructed energy for proton and Helium primaries.…”

Section: Uncertainty Of the Spectrum Of Light Nucleimentioning

confidence: 99%

“…Here we neglected the migration of events between energy bins (this effect is important only at the highest energies) and the energy scale uncertainty. We also assumed the energy reconstruction approach of [55,42,28]. Namely, we normalize the LDF of an observed EAS (with the unknown primary energy denoted as E Exp ) to composite model LDFs for a selection of model events.…”

Section: Uncertainty Of the Spectrum Of Light Nucleimentioning

confidence: 99%

“…In [40,41] the possibility to reconstruct the all-nuclei spectrum of primary CR using the observations performed with this detector was demonstrated. Moreover, a method for an event-byevent study of the CR mass composition in the energy range 10-100 PeV using the LDF steepness was devised [42].…”

Section: Introductionmentioning

confidence: 99%

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Spatial and temporal structure of EAS reflected Cherenkov light signal

Antonov

Bonvech

Чернов

et al. 2019

Astroparticle Physics

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A compact device lifted over the ground surface might be used to observe optical radiation of extensive air showers (EAS). Here we consider spatial and temporal characteristics of Vavilov-Cherenkov radiation ("Cherenkov light") reflected from the snow surface of Lake Baikal, as registered by the SPHERE-2 detector. We perform detailed full direct Monte Carlo simulations of EAS development and present a dedicated highly modular code intended for detector response simulations. Detector response properties are illustrated by example of several model EAS events. The instrumental acceptance of the SPHERE-2 detector was calculated for a range of observation conditions. We introduce the concept of "composite model quantities", calculated for detector responses averaged over photoelectron count fluctuations, but retaining EAS development fluctuations. The distortions of EAS Cherenkov light lateral distribution function (LDF) introduced by the SPHERE-2 telescope are understood by comparing composite model LDF with the corresponding function as would be recorded by an ideal detector situated at the ground surface. We show that the uncertainty of snow optical properties does not change our conclusions, and, moreover, that the expected performance of the SPHERE experiment in the task of cosmic ray mass composition study in the energy region ∼10 PeV is comparable with other contemporary experiments. Finally, we compare the reflected Cherenkov light method with other experimental techniques and briefly discuss its prospects. (T.A. Dzhatdoev) include CASA-BLANCA [16], BASJE [17], TACT [18] and the optical part of the Yakutsk array [19]. EAS fluorescent light was observed with HiRes [20] and the optical detectors of TA [21, 22] TALE [23] and PAO [15]. EAS radio emission is also studied in various experiments, such as LOPES [24], PAO [25], and LORA [26].The size of ground-based EAS detector arrays and their complexity is growing with time, and so does the difficulty of their deployment, calibration, and operation. Indeed, in order to work as an ensemble, the detectors must be distributed over a large area, sometimes hundreds [13] or thousands [15] square kilometers, and, moreover, they must be constantly power-supplied, be able to transfer information obtained with them, and kept fairly well timesynchronized.A long time ago it was pointed out that a compact device lifted over the snow-covered Earth surface is able to register reflected Cherenkov light [27]. This method is free from the above-mentioned difficulties of ground-based experiments. Moreover, a detector looking down at reflected Cherenkov light typically has a quasi-continious spatial sensitivity, i.e. it can observe light emitted from a substantial fraction of the snow-covered surface. This allows

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Section: Uncertainty Of the Spectrum Of Light Nucleimentioning

confidence: 82%

Section: Uncertainty Of the Spectrum Of Light Nucleimentioning

confidence: 99%

Section: Uncertainty Of the Spectrum Of Light Nucleimentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Spatial and temporal structure of EAS reflected Cherenkov light signal

Antonov

Bonvech

Чернов

et al. 2019

Astroparticle Physics

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“…Hovewer, in [11] we show that it is possible to improve the separationy of the event classes by utilizing multivariate analysis methods. In [11] we used the Bayesian multivariate pattern recognition technique assuming a multidimensional Gaussian distribution of event features [14]. Figures 11 and 12 show the fraction of Nitrogen nuclei classified as protons vs. proton selection efficiency.…”

Section: Multidimensional Methods For Superhigh Energy Cr Composition mentioning

confidence: 87%

Cosmic ray study by means of reflected EAS Cherenkov light method with the SPHERE-2 detector

Чернов¹,

Подгрудков²,

Antonov³

et al. 2017

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

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The approach to cosmic ray (CR) study with reflected optical Vavilov-Cherenkov radiation (Cherenkov light) was proposed long ago. At present the SPHERE-2 detector is the only existing apparatus that have detected a significant sample of extensive air showers (EAS) by means of this method. At the same time the recorded data allows detailed reconstruction of EAS lateral distribution function (LDF) used to study primary CR mass composition. We report on the status and results of the SPHERE experiment with the emphasis on the peculiarities of the reflected Cherenkov light technique. Detector response simulation was performed by means of full direct Monte Carlo simulation with account of realistic background and noise patterns recorded during the observational runs. Instrumental acceptance was simulated for various energies, charge numbers and zenith angles of primary nuclei. Primary energy of observed showers was estimated with a typical statistical uncertainty 10-20% depending on the primary nucleus parameters. The typical systematic uncertainty of the estimated energy vs the primary charge number was found to be below 3%. The primary all-nuclei spectrum was reconstructed. The fraction of light nuclei vs energy in the energy range 10-100 PeV was estimated by means of an event-by-event approach using the LDF steepness parameter.

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