STEREO ARRAY of 30m imaging atmospheric Čerenkov telescopes: A next-generation detector for ground-based high energy gamma-ray astronomy

Konopelko, A.

doi:10.1016/j.astropartphys.2005.06.009

Cited by 11 publications

(12 citation statements)

References 22 publications

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“…Addition-ally, the trigger system of IACTs discriminate against protons, although this is less effective at the lowest energies due to fluctuations in the shower development and a drop in image intensity. In the end, for the lowest energies, electrons become the dominant component of the differential trigger rate for a lowenergy-threshold IACT system [7,5,13]. All proton events passing the analysis cuts are considered as gamma-rays, and thus their reconstructed energy will be lower than the true energy.…”

Section: Introductionmentioning

confidence: 99%

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Earth magnetic field effects on the cosmic electron flux as background for Cherenkov Telescopes at low energies

Supanitsky

Rovero

2012

Astroparticle Physics

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Cosmic ray electrons and positrons constitute an important component of the background for imaging atmospheric Cherenkov Telescope Systems with very low energy thresholds. As the primary energy of electrons and positrons decreases, their contribution to the background trigger rate dominates over protons, at least in terms of differential rates against actual energies. After event reconstruction, this contribution might become comparable to the proton background at energies of the order of few GeV. It is well known that the flux of low energy charged particles is suppressed by the Earth's magnetic field. This effect strongly depends on the geographical location, the direction of incidence of the charged particle and its mass. Therefore, the geomagnetic field can contribute to diminish the rate of the electrons and positrons detected by a given array of Cherenkov Telescopes.In this work we study the propagation of low energy primary electrons in the Earth's magnetic field by using the backtracking technique. We use a more realistic geomagnetic field model than the one used in previous calculations. We consider some sites relevant for new generations of imaging atmospheric Cherenkov Telescopes. We also study in detail the case of 5@5, a proposed low energy Cherenkov Telescope array.

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Section: Introductionmentioning

confidence: 99%

“…All proton events passing the analysis cuts are considered as gamma-rays, and thus their reconstructed energy will be lower than the true energy. This causes the electron dominance to diminish, making the reconstructed flux of both electrons and protons comparable at the lowest energies [5].…”

Section: Introductionmentioning

confidence: 99%

Earth magnetic field effects on the cosmic electron flux as background for Cherenkov Telescopes at low energies

Supanitsky

Rovero

2012

Astroparticle Physics

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“…Provided that the instruments work in stereoscopic mode, the physical scale governing their relative arrangement on the ground is given by the size of the air shower's Cherenkov light pool, and the density and lateral distribution function of the Cherenkov photons. These in turn are functions of the primary gamma-ray energy and zenith angle of incidence, and subject to stochastic fluctuations of the shower development [6,7].…”

Section: Toy Model Arraymentioning

confidence: 99%

Multi-Objective Genetic Algorithm Optimisation for an Array of Cherenkov Telescopes

Souto¹,

Almeida²,

Giaccari³

2017

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

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In the context of the development of the Cherenkov Telescope Array, we have conceived and implemented a multi-objective genetic algorithm (GA) code for the optimisation of an array of Imaging Atmospheric Cherenkov Telescopes (IACTs). The algorithm takes as input a series of cost functions (metrics) each describing a different objetive of the optimisation (such as effective area, angular resolution, etc.), all of which are expressed in terms of the relative position of the telescopes in the plane. The output of the algorithm is a family of geometrical arrangements which correspond to the complete set of solutions to the array optimisation problem, and differ from each other according to the relative weight given to each of the (maybe conflicting) objetives of the optimisation. Since the algorithm works with parallel optimisation it admits as many cost functions as desired, and can incorporate constraints such as budget (cost cap) for the array and topological limitations of the terrain, like geographical accidents where telescopes cannot be installed. It also admits different types of telescopes (hybrid arrays) and the number of telescopes of each type can be treated as a parameter to be optimised -constrained, for example, by the cost of each type or the energy range of interest. The purpose of the algorithm, which converges fast to optimised solutions (if compared to the time for a complete Monte Carlo Simulation of a single configuration), is to provide a tool to investigate the full parameter space of possible geometries, and help in designing complex arrays. It does not substitute a detailed Monte Carlo study, but aims to guide it. In the examples of arrays shown here we have used as metrics simple heuristic expressions describing the fundamentals of the IAC technique, but these input functions can be made as detailed or complex as desired for a given experiment. It is important to stress that the individual characteristics of each telescope are taken as fixed, and only the telescope arrangement is being optimised. Preliminary results will be presented in this contribution for the first time.

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“…(Konopelko et al 2003) experiments. The performance of a single 30 m IACT was discussed in Konopelko (2005) in great detail. Thus the expected raw event detection rate for such a telescope is expected to be about 1.7 kHz.…”

Section: Simulationsmentioning

confidence: 99%

“…and MAGIC in the first few years of their operation are a strong motivation for the further development of the imaging atmospheric Cherenkov technique and is basically driven by a further reduction of the energy threshold for future γ-ray observations. Here we are presenting results for such a detector, a 30 m stand-alone imaging atmospheric Cherenkov telescope (IACT) that may potentially achieve an energy threshold as low as 10 GeV and is representative of a prototype for future low energy telescope arrays (see Konopelko 2005). The performance of such a telescope is basically determined by its efficiency at cosmic ray background rejection in the sub-100 GeV energy range.…”

Section: Introductionmentioning

confidence: 99%

Study on cosmic ray background rejection with a 30 m stand-alone IACT using non-parametric multivariate methods in a sub-100 GeV energy range

Konopelko

Chilingarian

Reimers

2006

J. Phys. G: Nucl. Part. Phys.

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During the last decade ground-based very high-energy γ-ray astronomy achieved a remarkable advancement in the development of the observational technique for the registration and study of γ-ray emission above 100 GeV. It is widely believed that the next step in its future development will be the construction of telescopes of substantially larger size than the currently used 10 m class telescopes. This can drastically improve the sensitivity of the ground-based detectors for γ rays of energy from 10 to 100 GeV. Based on Monte Carlo simulations of the response of a single stand-alone 30 m imaging atmospheric Cherenkov telescope (IACT) the maximal rejection power against background cosmic ray showers for low energy γ-rays was investigated in great detail. An advanced Bayesian multivariate analysis has been applied to the simulated Cherenkov light images of the γ-ray-and proton-induced air showers. The results obtained here quantitatively testify that the separation between the signal and background images degrades substantially at low energies, and consequently the maximum overall quality factor can only be about 3.1 for γ rays in the 10-30 GeV energy range. Various selection criteria as well as optimal combinations of the standard image parameters utilized for effective image separation have been also evaluated.

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STEREO ARRAY of 30m imaging atmospheric Čerenkov telescopes: A next-generation detector for ground-based high energy gamma-ray astronomy

Cited by 11 publications

References 22 publications

Earth magnetic field effects on the cosmic electron flux as background for Cherenkov Telescopes at low energies

Earth magnetic field effects on the cosmic electron flux as background for Cherenkov Telescopes at low energies

Multi-Objective Genetic Algorithm Optimisation for an Array of Cherenkov Telescopes

Study on cosmic ray background rejection with a 30 m stand-alone IACT using non-parametric multivariate methods in a sub-100 GeV energy range

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