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8 results on '"E.A. Osipova"'

1. A comparison of the cosmic-ray energy scales of Tunka-133 and KASCADE-Grande via their radio extensions Tunka-Rex and LOPES

Author

W.D. Apel, J.C. Arteaga-Velázquez, L. Bähren, P.A. Bezyazeekov, K. Bekk, M. Bertaina, P.L. Biermann, J. Blümer, H. Bozdog, I.M. Brancus, N.M. Budnev, E. Cantoni, A. Chiavassa, K. Daumiller, V. de Souza, F. Di Pierro, P. Doll, R. Engel, H. Falcke, O. Fedorov, B. Fuchs, H. Gemmeke, O.A. Gress, C. Grupen, A. Haungs, D. Heck, R. Hiller, J.R. Hörandel, A. Horneffer, D. Huber, T. Huege, P.G. Isar, K.-H. Kampert, D. Kang, Y. Kazarina, M. Kleifges, E.E. Korosteleva, D. Kostunin, O. Krömer, J. Kuijpers, L.A. Kuzmichev, K. Link, N. Lubsandorzhiev, P. Łuczak, M. Ludwig, H.J. Mathes, M. Melissas, R.R. Mirgazov, R. Monkhoev, C. Morello, J. Oehlschläger, E.A. Osipova, A. Pakhorukov, N. Palmieri, L. Pankov, T. Pierog, V.V. Prosin, J. Rautenberg, H. Rebel, M. Roth, G.I. Rubtsov, C. Rühle, A. Saftoiu, H. Schieler, A. Schmidt, S. Schoo, F.G. Schröder, O. Sima, G. Toma, G.C. Trinchero, A. Weindl, R. Wischnewski, J. Wochele, J. Zabierowski, A. Zagorodnikov, and J.A. Zensus

Subjects
Physics, QC1-999
Abstract

The radio technique is a promising method for detection of cosmic-ray air showers of energies around 100PeV and higher with an array of radio antennas. Since the amplitude of the radio signal can be measured absolutely and increases with the shower energy, radio measurements can be used to determine the air-shower energy on an absolute scale. We show that calibrated measurements of radio detectors operated in coincidence with host experiments measuring air showers based on other techniques can be used for comparing the energy scales of these host experiments. Using two approaches, first via direct amplitude measurements, and second via comparison of measurements with air shower simulations, we compare the energy scales of the air-shower experiments Tunka-133 and KASCADE-Grande, using their radio extensions, Tunka-Rex and LOPES, respectively. Due to the consistent amplitude calibration for Tunka-Rex and LOPES achieved by using the same reference source, this comparison reaches an accuracy of approximately 10% – limited by some shortcomings of LOPES, which was a prototype experiment for the digital radio technique for air showers. In particular we show that the energy scales of cosmic-ray measurements by the independently calibrated experiments KASCADE-Grande and Tunka-133 are consistent with each other on this level. Keywords: Cosmic rays, Radio detection, LOPES, Tunka-Rex, Tunka-133, KASCADE-Grande

Published
2016
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2. The primary cosmic-ray energy spectrum measured with the Tunka-133 array

Author

N.M. Budnev, A. Chiavassa, O.A. Gress, T.I. Gress, A.N. Dyachok, N.I. Karpov, N.N. Kalmykov, E.E. Korosteleva, V.A. Kozhin, L.A. Kuzmichev, B.K. Lubsandorzhiev, N.B. Lubsandorzhiev, R.R. Mirgazov, E.A. Osipova, M.I. Panasyuk, L.V. Pankov, E.G. Popova, V.V. Prosin, V.S. Ptuskin, Yu.A. Semeney, A.A. Silaev, A.A. Silaev(junior), A.V. Skurikhin, C. Spiering, L.G. Sveshnikova, and A.V. Zagorodnikov

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Computational physics, Amplitude, Air shower, Calibration, Ultra-high-energy cosmic ray, Astrophysics - High Energy Astrophysical Phenomena, Cherenkov radiation, Energy (signal processing)
Abstract

The EAS Cherenkov light array Tunka-133, with $\sim$ 3 km$^2$ geometric area, is taking data since 2009.The array permits a detailed study of energy spectrum and mass composition of cosmic rays in the energy range from $6\cdot 10^{15}$ to $10^{18}$ eV. We describe the methods of time and amplitude calibration of the array and the methods of EAS parameters reconstruction. We present the all-particle energy spectrum, based on 7 seasons of operation., Comment: 12 pages,18 figures

Published
2021
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3. The Tunka-Grande experiment

Author

R.D. Monkhoev, N.M. Budnev, A. Chiavassa, A.N. Dyachok, A.R. Gafarov, O.A. Gress, T.I. Gress, O.G. Grishin, A.L. Ivanova, N.N. Kalmykov, Yu.A. Kazarina, E.E. Korosteleva, V.A. Kozhin, L.A. Kuzmichev, V.V. Lenok, B.K. Lubsandorzhiev, N.B. Lubsandorzhiev, R.R. Mirgazov, R. Mirzoyan, E.A. Osipova, A.L. Pakhorukov, M.I. Panasyuk, L.V. Pankov, V.A. Poleschuk, E.G. Popova, E.B. Postnikov, V.V. Prosin, V.S. Ptuskin, A.A. Pushnin, V.S. Samoliga, Y.A. Semeney, L.G. Sveshnikova, A.A. Silaev, A.A. Silaev Jr., A.V. Skurikhin, V.P. Sulakov, V.A. Tabolenko, D.M. Voronin, O.L. Fedorov, C. Spiering, A.V. Zagorodnikov, D.P. Zhurov, and V.L. Zurbanov

Subjects
Physics, Photon, COSMIC cancer database, Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Cosmic ray, Scintillator, 01 natural sciences, Electromagnetic radiation, Spectral line, Massless particle, 0103 physical sciences, 010306 general physics, Instrumentation, Mathematical Physics
Abstract

The investigation of energy spectrum and mass composition of primary cosmic rays in the energy range 10(16)–10(18) eV and the search for diffuse cosmic gamma rays are of the great interest for understanding mechanisms and nature of high-energy particle sources, the problem of great importance in modern astrophysics. Tunka-Grande scintillator array is a part of the experimental complex TAIGA (Tunka Advanced Instrument for Cosmic Ray and Gamma Astronomy) which is located in the Tunka Valley, about 50 km from Lake Baikal. The purpose of this array is the study of diffuse gamma rays and cosmic rays of ultra-high energies by detecting extensive air showers. We describe the design, specifications of the read-out, data acquisition (DAQ) and control systems of the array.

Published
2017

4. Registration of atmospheric neutrinos with the BAIKAL Neutrino Telescope NT-96

Author

V.A. Balkanov, I.A. Belolaptikov, L.B. Bezrukov, N.M. Budnev, A.G. Chensky, I.A. Danilchenko, Zh.-A.M. Djilkibaev, G.V. Domogatsky, A.A. Doroshenko, S.V. Fialkovsky, O.N. Gaponenko, A.A. Garus, T.I. Gress, A.M. Klabukov, A.I. Klimov, S.I. Klimushin, A.P. Koshechkin, V.F. Kulepov, L.A. Kuzmichev, V.E. Kuznetzov, J.J. Laudinskaite, S.V. Lovtzov, B.K. Lubsandorzhiev, M.B. Milenin, R.R. Mirgazov, N.I. Moseiko, V.A. Netikov, E.A. Osipova, A.I. Panfilov, Yu.V. Parfenov, A.A. Pavlov, E.N. Pliskovsky, P.G. Pokhil, E.G. Popova, M.I. Rozanov, V.Yu. Rubtzov, I.A. Sokalski, Ch. Spiering, O. Streicher, B.A. Tarashansky, T. Thon, R.V. Vasiljev, R. Wischnewski, and I.V. Yashin

Subjects
Physics, Muon, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Neutrino telescope, Flux, Astronomy and Astrophysics, Astrophysics, law.invention, Telescope, law, High Energy Physics::Experiment, Underwater, Neutrino, Zenith
Abstract

We present first neutrino induced events observed with a deep underwater neutrino telescope. Data from 70 days effective life time of the BAIKAL prototype telescope NT-96 have been analyzed with two different methods. With the standard track reconstruction method, 9 clear upward muon candidates have been identified, in good agreement with 8.7 events expected from Monte Carlo calculations for atmospheric neutrinos. The second analysis is tailored to muons coming from close to the opposite zenith. It yields 4 events, compared to 3.5 from Monte Carlo expectations. From this we derive a 90 % upper flux limit of 1.1 * 10^-13 cm^-2 sec^-1 for muons in excess of those expected from atmospheric neutrinos with zenith angle > 150 degrees and energy > 10GeV.

Published
1999

5. Status of the AMANDA and BAIKAL neutrino telescopes

Author

P. Askebjer, S.W. Barwick, R. Bay, L. Bergström, A. Bouchta, S. Carius, E. Dahlberg, K. Engel, B. Erlandsson, A. Goobar, L. Gray, A. Hallgren, F. Halzen, H. Heukenkamp, P.O. Hulth, S. Hundertmark, J. Jacobsen, S. Johansson, V. Kandhadai, A. Karle, I. Liubarsky, D. Lowder, T. Mikolajski, T.C. Miller, P. Mock, R. Morse, D. Nygren, R. Porrata, P.B. Price, A. Richards, H. Rubinstein, E. Schneider, C. Spiering, O. Streicher, Q. Sun, T. Thon, S. Tilav, C. Walck, C. Wiebusch, R. Wischnewski, G. Yodh, I.A. Belolaptikov, L.B. Bezrukov, B.A. Borisovets, N.M. Budnev, A.G. Chensky, I.A. Danilchenko, Zh.-A.M. Djilkibaev, V.I. Dobrynin, G.V. Domogatsky, A.A. Doroshenko, S.V. Fialkovsky, O.N. Gaponenko, A.A. Garus, T.A. Gress, S.B. Ignat'ev, A.M. Klabukov, A.I. Klimov, S.I. Klimushin, A.P. Koshechkin, V.F. Kulepov, L.A. Kuzmichev, B.K. Lubsandorzhiev, M.B. Milenin, R.R. Mirgazov, A.V. Moroz, N.I. Moseiko, S.A. Nikiforov, E.A. Osipova, D. Pandel, A.I. Panfilov, Yu.V. Parfenov, A.A. Pavlov, D.P. Petukhov, K.A. Pocheikin, P.G. Pokhil, P.A. Pokolev, M.I. Rosanov, V.Yu. Rubzov, S.I. Sinegovsky, I.A. Sokalski, Ch. Spiering, and B.A. Tarashansky

Subjects
Astroparticle physics, Physics, Nuclear and High Energy Physics, Particle physics, Neutrino, Atomic and Molecular Physics, and Optics
Published
1997

6. The Baikal-experiment

Author

I.A. Belolaptikov, L.B. Bezrukov, B.A. Borisovets, E.V. Bugaev, G.V. Domogatsky, A.A. Doroshenko, M.D. Galperin, A.V. Golikov, Zh.-A.M. Jilkibaev, A.M. Klabukov, S.I. Klimushin, B.K. Lubsandorzhiev, A.I. Panfilov, I.A. Sokal'sky, L.N. Stepanov, I.I. Trofimenko, N.M. Budnev, A.G. Chensky, V.I. Dobrynin, A.D. Fomin, A.P. Koshechkin, J.B. Lanin, G.A. Litunenko, A.V. Lopin, V.A. Naumov, M.I. Nemchenko, Yu.A. Parfenov, A.A. Pavlov, V.A. Poleschuk, V.A. Primin, A.A. Schestakov, V.A. Taraschansky, A.V. Yakup, V.L. Zurbanov, E.S. Saslavskaya, V.B. Kabikov, L.A. Kuzmichev, E.A. Osipova, Yu.S. Kusner, P.P. Scherstyankin, G.N. Dudkin, A.M. Ovcharov, V.M. Padalko, J. Krabi, Ch. Spiering, T. Weinert, R. Wischnewski, P. Kakas, D. Kiss, and L. Tankó

Subjects
Physics, Nuclear and High Energy Physics, Angular distribution, Neutrino detector, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, High Energy Physics::Experiment, Cosmic ray, Astrophysics, Neutrino, Atomic and Molecular Physics, and Optics, Particle detector
Abstract

We review the historical development and the present status of the Baikal experiment, and sketch the 6-string detector “NT-200”, which is planned to be deployed until 1993 and to study neutrino astrophysics cosmic rays and particle physics.

Published
1990

7. The optical module of the Baikal deep underwater neutrino telescope

Author

R.I. Bagduev, V. Balkanov, I.A. Belolaptikov, L.B. Bezrukov, N.M. Budnev, B.A. Borisovets, G.V. Domogatsky, L.A. Donskych, A.A. Doroshenko, A.A. Garus, A.V. Golikov, B.M. Gluchovskoj, R. Heller, V.B. Kabikov, M.P. Khripunova, A.M. Klabukov, S.I. Klimushin, A.P. Koshechkin, L.A. Kuzmichov, G.V. Lisovski, B.K. Lubsandorzhiev, T. Mikolajski, E.A. Osipova, P.G. Pokhil, P.A. Pokolev, P.A. Putilov, Ch. Spiering, Z.I. Stepanenko, O. Streicher, T. Thon, A.A. Vorobiev, and R. Wischnewski

Subjects
Physics, Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, Optical Module, Telescope, Phototube, Baikal Deep Underwater Neutrino Telescope, law, Calibration, Electronics, Underwater, Instrumentation, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Remote sensing
Abstract

A deep underwater Cherenkov telescope has been operating since 1993 in stages of growing size at 1.1 km depth in Lake Baikal. The key component of the telescope is the Optical Module (OM) which houses the highly sensitive phototube QUASAR-370. We describe design and parameters of the QUASAR-370, the layout of the optical module, the front-end electronics and the calibration procedures, and present selected results from the five-year operation underwater. Also, future developments with respect to a telescope consisting from several thousand OMs are discussed., Comment: 30 pages, 24 figures

Published
1999
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8. Status of the Lake Baikal Experiment

Author

G.V. Domogatsky, V.A. Balkanov, I.A. Belolaptikov, L.B. Bezrukov, N.M. Budnev, A.G. Chensky, I.A. Danilchenko, Zh.-A. Djilkibaev, A.A. Doroshenko, S.V. Fialkovsky, O.N. Gaponenko, A.A. Garus, T.I. Gress, A.M. Klabukov, A.I. Klimov, S.I. Klimushin, A.P. Koshechkin, V.F. Kulepov, L.A. Kuzmichev, S.V. Lovzov, B.K. Lubsandorzhiev, M.B. Milenin, R.R. Mirgazov, A.V. Moroz, N.I. Moseiko, S.A. Nikiforov, E.A. Osipova, A.I. Panfilov, Yu.V. Parfenov, A.A. Pavlov, D.P. Petukhov, P.G. Pokhil, P.A. Pokolev, E.G. Popova, M.I. Rozanov, V.Yu. Rubzov, I.A. Sokalski, Ch. Spiering, O. Streicher, B.A. Tarashansky, T. Thon, R. Wischnewski, and I.V. Yashin

Subjects
Nuclear and High Energy Physics, Oceanography, Neutrino detector, Earth science, Astrophysics (astro-ph), FOS: Physical sciences, Environmental science, Underwater, Neutrino, Astrophysics, Atomic and Molecular Physics, and Optics, Lepton
Abstract

We review the present status of the Baikal Underwater Neutrino Experiment and report on neutrino events recorded with the detector stages NT-36 and NT-96., Comment: 5 pages, 4 PostScript figures, uses here.sty and mine.sty, submitted to the Proc. of 5th Int. Workshop on Topics in Astroparticle and Underground Physics (LNGS INFN, Assergi, September 7-11, 1997)

Published
1997

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