GAMMA RAYS STUDIES BASED ON ATMOSPHERIC CHERENKOV TECHNIQUE AT HIGH MOUNTAIN ALTITUDE

2005 ◽  
Vol 20 (29) ◽  
pp. 7016-7019 ◽  
Author(s):  
A. MISHEV ◽  
S. MAVRODIEV ◽  
J. STAMENOV
Keyword(s):  
Energy Range ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Light Flux ◽  
Extensive Air Showers ◽  
Cherenkov Light ◽  
High Mountain ◽  
Flux Analysis ◽  
Air Showers ◽  
Gamma Ray Astronomy

We present a new method for ground based gamma ray astronomy based only on atmospheric Cherenkov light flux analysis. The Cherenkov light flux densities in extensive air showers initiated by different primaries are simulated in the energy range 100 GeV – 100 PeV for different primaries using the CORSIKA 6.003 code at (536 g/cm2). An approximation of lateral distribution of Cherenkov light flux densities in EAS is obtained using a nonlinear fit such as Breit-Wigner. The simulated and reconstructed events are compared and the accuracy in energy and primary mass reconstruction are obtained.

Ground-based Gamma-ray Astronomy

1993 ◽  
Vol 10 (3) ◽  
pp. 183-188 ◽  
Author(s):  
R.W. Clay ◽  
B.R. DawSOn
Keyword(s):  
Energy Range ◽  
Present State ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Signal To Noise ◽  
Gamma Ray Astronomy ◽  
The Past

AbstractGround-based gamma-ray astronomy has slowly developed over the past quarter of a century to a position now where a number of sources are known to produce gamma-rays in the energy range 1011eV to 1018eV. The observations are difficult, with exceptional signal to noise problems, but improved techniques are now allowing observers to proceed with confidence. In this paper the physical bases of the observations are emphasised to show the important issues in the field and the present state of the observations is indicated.

Estimating of Cherenkov Radiation in Extensive Air Showers Using CORSIKA Code for Tunka133 EAS Cherenkov Array

2015 ◽  
Vol 754-755 ◽  
pp. 807-811
Author(s):  
A.A. Al-Rubaiee ◽  
Uda Hashim ◽  
Mohd Khairuddin Md Arshad ◽  
A. Rahim Ruslinda ◽  
R.M. Ayub ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Energy Range ◽  
Cosmic Ray ◽  
High Energy ◽  
Extensive Air Showers ◽  
Cherenkov Light ◽  
Mass Composition ◽  
Air Showers ◽  
Good Ability ◽  
The Given

The simulation of Cherenkov light Lateral distribution function (LDF) in Extensive Air Showers (EAS) initiated primary particles such as primary calcium, argon, proton iron nuclei, neutron and nitrogen have been performed using CORSIKA program for conditions and configurations of Tunka133 EAS Cherenkov array. The simulation was fulfilled at the high energy range 1014-1016eV for four different zenith angles 0o, 10o, 15oand 30o. The results of the simulated Cherenkov light LDF are compared with the measurements of Tunka133 EAS array for the same particles and energy range mentioned above. This comparison may give the good ability to reconstruct the energy spectrum and mass composition of the primary cosmic ray particles in EAS. The main feature of the given approach consists of the possibility to make a library of Cherenkov light LDF samples which could be utilized for analysis of real events which can be detected with different EAS arrays and reconstruction of the primary cosmic rays energy spectrum and mass composition of EAS particles.

Detection of UV Radiation from Extensive Air Showers: Prospects for Cherenkov Gamma-Ray Astronomy

2018 ◽  
Vol 63 (11) ◽  
pp. 1603-1614 ◽  
Author(s):  
E. E. Kholupenko ◽  
A. M. Bykov ◽  
F. A. Aharonyan ◽  
G. I. Vasiliev ◽  
A. M. Krassilchtchikov ◽  
...  
Keyword(s):  
Uv Radiation ◽  
Gamma Ray ◽  
Extensive Air Showers ◽  
Air Showers ◽  
Gamma Ray Astronomy

Solar Flare Energetic Neutral Emission Measurements in the Project Coronas-I

1994 ◽  
Vol 144 ◽  
pp. 635-639
Author(s):  
J. Baláž ◽  
A. V. Dmitriev ◽  
M. A. Kovalevskaya ◽  
K. Kudela ◽  
S. N. Kuznetsov ◽  
...  
Keyword(s):  
Solar Flare ◽  
Energy Range ◽  
Gamma Rays ◽  
Pulse Shape ◽  
Gamma Ray ◽  
Pulse Shape Discrimination ◽  
Shape Discrimination ◽  
Solar Neutron ◽  
Low Altitude

AbstractThe experiment SONG (SOlar Neutron and Gamma rays) for the low altitude satellite CORONAS-I is described. The instrument is capable to provide gamma-ray line and continuum detection in the energy range 0.1 – 100 MeV as well as detection of neutrons with energies above 30 MeV. As a by-product, the electrons in the range 11 – 108 MeV will be measured too. The pulse shape discrimination technique (PSD) is used.

Calibration of a gamma ray astronomy telescope in the 5–50 MeV energy range

1982 ◽  
Vol 199 (3) ◽  
pp. 585-596 ◽  
Author(s):  
J.M. Lavigne ◽  
M. Niel ◽  
G. Vedrenne ◽  
C. Doulade ◽  
G. Giordano ◽  
...  
Keyword(s):  
Energy Range ◽  
Gamma Ray ◽  
Gamma Ray Astronomy

scholarly journals TARANIS XGRE and IDEE Detection Capability of Terrestrial Gamma-Ray Flashes and Associated Electron Beams

2017 ◽  
Author(s):  
David Sarria ◽  
Francois Lebrun ◽  
Pierre-Louis Blelly ◽  
Remi Chipaux ◽  
Philippe Laurent ◽  
...  
Keyword(s):  
Monte Carlo ◽  
Monte Carlo Simulations ◽  
Energy Range ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Electron Beams ◽  
Effective Area ◽  
Detection Rates ◽  
Transient Phenomena ◽  
Preliminary Model

Abstract. With a launch expected in 2018, the TARANIS micro-satellite is dedicated to the study of transient phenomena observed in association with thunderstorms. On-board the spacecraft, XGRE and IDEE are two instruments dedicated to study Terrestrial Gamma-ray Flashes (TGFs) and associated electron beams (TEBs). XGRE can detect electrons (energy range: 1 MeV to 10 MeV) and X/gamma-rays (energy range: 20 keV to 10 MeV), with a very high counting capability (about 10 million counts per second), and the ability to discriminate one type of particle from the other. The IDEE instrument is focused on electrons in the 80 keV to 4 MeV energy range, with the ability to estimate their pitch angles. Monte-Carlo simulations of the TARANIS instruments, using a preliminary model of the spacecraft, allow sensitive area estimates for both instruments. It leads to an averaged effective area of 425 cm2 for XGRE to detect X/gamma rays from TGFs, and the combination of XGRE and IDEE gives an average effective area of 255 cm2 to detect electrons/positrons from TEBs. We then compare these performances to RHESSI, AGILE, and Fermi GBM, using performances extracted from literature for the TGF case, and with the help of Monte-Carlo simulations of their mass models for the TEB case. Combining these data with with the help of the MC-PEPTITA Monte-Carlo simulations of TGF propagation in the atmosphere, we build a self-consistent model of the TGF and TEB detection rates of RHESSI, AGILE, and Fermi. It can then be used to estimate that TARANIS should detect about 225 TGFs/year and 25 TEBs/year.

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