Design study of CANGAROO-III, stereoscopic imaging atmospheric Cherenkov telescopes for sub-TeV γ-ray detection

Enomoto, R.; Hara, Shinji; Asahara, A.; Bicknell, G. V.; Edwards, Philip; Gunji, Shuichi; Hara, T.; Jimbo, J.; Kajino, F.; Katagiri, H.; Kataoka, J.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Moriya, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakase, T.; Nishijima, K.; Okumura, Ko; Patterson, Joseph; Sakurazawa, K.; Swaby, D. L.; Takano, K.; Tanimori, T.; Tamura, T.; Tsuchiya, Ken; Uruma, K.; Yanagita, S.; Yoshida, Tatsuo; Yoshikoshi, T.; Akizuki, Yuki

doi:10.1016/s0927-6505(01)00112-8

Cited by 58 publications

(30 citation statements)

References 11 publications

(11 reference statements)

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“…Indeed, there are already such arrays of telescopes planned or in operation such as CANGAROO [21], HESS [22], VERITAS [23] and MAGIC [24]. In particular, CANGAROO and HESS are well located to observe the galactic center for a sizable fraction of their observing time.…”

Section: The Detectability Of Nr Through Gamma-raysmentioning

confidence: 99%

Detection of leptonic dark matter

Baltz

Bergström

2003

Phys. Rev. D

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Weakly interacting massive particles (WIMPs) are among the favored candidates for cold dark matter in the universe. The phenomenology of supersymmetric WIMPs has been quite developed during recent years. However, there are other possibilities which have not been discussed as much. One example is a right-handed massive neutrino, which has recently been proposed in the context of a version of the Zee model for massive neutrinos. This TeV-scale, leptonic WIMP (or LIMP, for short) may at first sight appear to be essentially undetectable. However, we point out that the radiatively induced annihilation rate into leptons and photons is bound to be substantial, and provides a conspicuous gamma-ray signature for annihilations in the galactic halo. This gives a window of opportunity for AirČerenkov Telescopes with ability to observe the galactic center, such as the HESS and CANGAROO arrays, and also for the GLAST space telescope. In addition, the contribution to the positron cosmic ray flux is in principle detectable, but this would require very strong local density enhancements in the dark matter halo distribution.PACS numbers: 95.35.+d, 14.60.St, 95.85.Pw, 95.85.Ry, 98.70.Rz

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Section: The Detectability Of Nr Through Gamma-raysmentioning

confidence: 99%

Detection of leptonic dark matter

Baltz

Bergström

2003

Phys. Rev. D

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“…The time structure of the image can be used in the data analysis as an additional parameter as it is shown in [7]. Recent experiments with large reflectors like CANGAROO [8,9], HESS [10,11], MAGIC [12,13], VERITAS [14,15] made a major contribution to the very fast development of ground-based γ-ray astronomy (see figure 1 in [16]). The detection of low energy events is possible by using a very large telescope, which requires a parabolic shape of the main reflector dish (like that in MAGIC) to avoid broadening of the time profile of the Cherenkov signal.…”

Section: Introductionmentioning

confidence: 99%

The background from single electromagnetic subcascades for a stereo system of air Cherenkov telescopes

Sobczyńska¹

2009

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

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Abstract.The MAGIC experiment, a very large Imaging Air Cherenkov Telescope (IACT) with sensitivity to low energy (E < 100 GeV) VHE gamma rays, has been operated since 2004. It has been found that the γ/hadron separation in IACTs becomes much more difficult below 100 GeV [1]. A system of two large telescopes may eventually be triggered by hadronic events containing Cherenkov light from only one electromagnetic subcascade or two γ subcascades, which are products of the single π 0 decay. This is a possible reason for the deterioration of the experiment's sensitivity below 100 GeV. In this paper a system of two MAGIC telescopes working in stereoscopic mode is studied using Monte Carlo simulations. The detected images have similar shapes to that of primary γ-rays and they have small sizes (mainly below 400 photoelectrons (p.e.)) which correspond to an energy of primary γ-rays below 100 GeV. The background from single or two electromagnetic subcascdes is concentrated at energies below 200 GeV. Finally the number of background events is compared to the number of VHE γ-ray excess events from the Crab Nebula. The investigated background survives simple cuts for sizes below 250 p.e. and thus the experiment's sensitivity deteriorates at lower energies.PACS numbers: 95.55. Ka; 95.55.Vj; 95.75.Mn; 95.85.Pw; 95.85.Ry

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“…The number of excess events was determined from the plots of image orientation angle a for on-and off-source runs (inset) to be 3,417±240 (14.3σ). The γ-ray acceptance efficiency was calculated using the Monte Carlo method 26 . In order to check our simulations, we analysed Crab nebula data obtained in December 1999 and December 2000, and found that the flux was consistent with previous experiments 28 to within 12%.…”

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confidence: 99%

The acceleration of cosmic-ray protons in the supernova remnant RX J1713.7–3946

Enomoto

Tanimori

Naito

et al. 2002

Nature

227

197

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Protons with energies up to ~ 10 15 eV are the main component 1 of cosmic rays, but evidence for the specific locations where they could have been accelerated to these energies has been lacking 2 . Electrons are known to be accelerated to cosmic-ray energies in supernova remnants 3,4 , and the shock waves associated with such remnants, when they hit the surrounding interstellar medium, could also provide the energy to accelerate protons. The signature of such a process would be the decay of pions (π 0 ), which are generated when the protons collide with atoms and molecules in an interstellar cloud: pion decay results in γ-rays with a particular spectral-energy distribution 5,6 . Here we report the observation of cascade showers of optical photons resulting fromγ-rays at energies of ~ 10 12 eV hitting Earth's upper atmosphere, in the direction of the supernova remnant RX J1713.7-3946. The spectrum is a good match to that predicted by pion decay, and cannot be explained by other mechanisms.

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Design study of CANGAROO-III, stereoscopic imaging atmospheric Cherenkov telescopes for sub-TeV γ-ray detection

Cited by 58 publications

References 11 publications

Detection of leptonic dark matter

Detection of leptonic dark matter

The background from single electromagnetic subcascades for a stereo system of air Cherenkov telescopes

The acceleration of cosmic-ray protons in the supernova remnant RX J1713.7–3946

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