Tunka-133: Results of 3 year operation Prosin, V.V.; Berezhnev, S.F.; Budnev, N.M. ...
Nuclear instruments & methods in physics research. Section A, Accelerators, spectrometers, detectors and associated equipment,
08/2014, Letnik:
756
Journal Article
Recenzirano
Odprti dostop
The EAS Cherenkov light array Tunka-133, with ~3km2 geometric area, is taking data since 2009. The array permits a detailed study of cosmic ray energy spectrum and mass composition in the PeV energy ...range. After a short description of the methods of EAS parameter reconstruction, we present the all-particle energy spectrum and results of studying CR composition, based on 3 seasons of array operation. In the last part of the paper, we discuss possible interpretations of the obtained results.
The Tunka-133 EAS Cherenkov light array: Status of 2011 Berezhnev, S.F.; Besson, D.; Budnev, N.M. ...
Nuclear instruments & methods in physics research. Section A, Accelerators, spectrometers, detectors and associated equipment,
11/2012, Letnik:
692
Journal Article
Recenzirano
Odprti dostop
A new EAS Cherenkov light array, Tunka-133, with ∼1km2 geometrical area has been installed at the Tunka Valley (50km from Lake Baikal) in 2009. The array permits a detailed study of cosmic ray energy ...spectrum and mass composition in the energy range 1016–1018eV with a uniform method. We describe the array construction, DAQ and methods of the array calibration. The method of energy reconstruction and absolute calibration of measurements are discussed. The analysis of spatial and time structure of EAS Cherenkov light allows to estimate the depth of the EAS maximum Xmax.
The results on the all particles energy spectrum and the mean depth of the EAS maximum Xmax vs. primary energy derived from the data of two winter seasons (2009–2011) are presented. Preliminary results of joint operation of the Cherenkov array with antennas for the detection of EAS radio signals are shown. Plans for future upgrades – deployment of remote clusters, radioantennas and a scintillator detector network and a prototype of the HiSCORE gamma-telescope – are discussed.
The Tunka-133 Cherenkov light array for the detection of extensive air showers (EAS) acquires data over the five winters from 2009 to 2014. The direction of arrival, the shower core coordinates on ...the plane of observation, the primary energy, and the depth of the shower maximum are reconstructed for each EAS. A differential all-particle energy spectrum is obtained in the energy range of 6 × 10
15
–3 × 10
18
eV over 1540 h, along with the energy dependence of the average depth of the shower maximum in the range of 6 × 10
16
–3 × 10
18
eV. Based on this dependence, the variation in the average composition of the primary cosmic rays is estimated as a function of energy.
The EAS Cherenkov array Tunka-133, with about 3km2 sensitive area, has been installed in the Tunka Valley, Siberia. The accessible energy range is 1015–1018eV. In this contribution, a description of ...the array and main results obtained so far are presented. A current update of the array includes the deployment of scintillation stations, radio antennas, as well as optical stations. The deployments of these optical stations are the first step towards Tunka-HiSCORE, a wide-angle, large field-of-view gamma-ray telescope.
The result of ambient noise tomography for the Kambalny Volcano (South Kamchatka), where the first time in the entire history of observations a violent phreatic eruption was observed in March–April ...2017, is presented. The results obtained clarify the structure of the upper part of the edifice of the Kambalny Volcano and are consistent with independent data on body waves, as well as with geological information. According to seismotomographic data of the surface waves, low-velocity anomalies are distinguished in the model of the structure of the volcanic edifice. They are asymmetric relative to the volcano cone and are allocated to loose pyroclastic deposits of past eruptions and to deep sources of hydrothermal activity. Perhaps the migration of fluids in these hydrothermal vents to the north and west of the volcano and their interaction with the magma chamber in the upper crust caused the explosive eruption.
The results of an analysis of data from the SERP-Е-184 experiment devoted to studying mechanisms of the production of charmed particles in proton–nucleus interactions at 70 GeV and their decays are ...presented. The data in question were obtained upon irradiating the SVD-2 active target consisting of carbon, silicon, and lead plates with a beam of 70-GeV protons. A detailed simulation on the basis of the FRITIOF7.02 and GEANT3.21 code packages made it possible to optimize event-selection criteria and to calculate the detection efficiency for Λ
c
+
baryons. After selecting a signal from the threebody decay of a Λ
c
+
baryon, the inclusive cross section for its production at near-threshold energies, its lifetime, and the parameter of the
A
dependence of the cross section were found. The Λ
c
+
-baryon yields are tabulated along with data from other experiments and theoretical predictions.
The Tunka-HISCORE wide-angle Cherenkov array, one part of the planned TAIGA integrated gamma observatory intended for investigations in the field of high-energy (>30 TeV) gamma-ray astronomy and ...cosmic-ray physics, is deployed in the Tunka Valley (Buryat Republic). The first results from operating a prototype array composed of nine stations spread over an area of ∼0.1 square kilometers during the winter of 2013–2014 are presented. Data processing techniques are described, along with data on the accuracy of reconstructing the position of a shower’s axis, energy, and angle of arrival. The differential spectrum of all cosmic-ray particles in a shower in the energy range of 2 × 10
14
to 2 × 10
16
eV is presented and compared to the available data.
A new array for studying ultra-high energy cosmic rays was inaugurated in 2009 in the Tunka Valley, about 50 km from Lake Baikal. Having an area of 1 km
2
, the new facility allows us to study cosmic ...rays with energies of 10
15
–10
18
eV via the a unified method for registering Cherenkov radiation from extensive air showers (EASes) and is making a substantial contribution to understanding the origin of ultra-high energy cosmic rays. We describe the current state of the experiment, the new methodological approach, our initial results, and the plans for further development of the array.
With the HiSCORE (Hundred*i Square kilometer Cosmic ORigin Explorer) experiment we aim at the exploration of the accelerator sky using indirect air shower observations of cosmic rays from 100 TeV to ...1 EeV and gamma rays above 10 TeV to several PeV. In this paper the HiSCORE detector is discribed and the results of the first prototype deployment are shown. Several components are discussed like the photomultiplier tubes, the clip-sum-trigger and the DRS4 based data acquisition. We present data taken with a first prototype station in April 2012 at Tunka.
Data from the SVD-2 experiment that were obtained at the IHEP accelerator in 70-GeV/c proton-nucleus interactions are analyzed with the aim of searches for an exotic {theta}{sup +} baryon that decays ...through the pK{sup 0}{sub S} channel. The reaction pN {yields} pK{sup 0}{sub S} + X characterized by a bounded multiplicity of charged secondaries is used for this analysis. A resonance of mass M = 1526 {+-} 3(stat.) {+-} 3(syst.) MeV/c{sup 2} and width {gamma} < 24 MeV/c{sup 2} is observed in the invariant-mass spectrum of the pK{sup 0}{sub S} system at a statistical significance of 5.6{sigma}. The mass and the width of this resonance correspond to the recently found positive-strangeness {theta}{sup +} baryon, which was predicted to be an exotic baryon consisting of five quarks (pentaquark), uudds-bar. The total cross section for the production of a {theta}{sup +} baryon in pA interactions is estimated at a value within the range 30-120 {mu}b for x{sub F} {>=} 0. An analysis of the A dependence of the cross section for {theta}{sup +}-baryon production does not reveal a significant deviation from the A dependence for inelastic events ({approx}A{sup 0.7})
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