The CANGAROO-III project

Mori, M.; Dazeley, S.; Edwards, P. G.; Gunji, Shuichi; Hara, Shinji; Hara, T.; Jiang, Jinbo; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Matsubara, Y.; Mizumoto, Y.; Moriya, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nishijima, K.; Patterson, J. R.; Roberts, M.; Rowell, G.; Sako, T.; Sakurazawa, K.; Sato, Yoshihito; Susukita, R.; Tamura, T.; Tanimori, T.; Yanagita, S.; Yoshida, Tatsuo; Yoshikoshi, T.; Akizuki, Yuki

doi:10.1063/1.1291414

Cited by 14 publications

(5 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Of the upcoming ACTs, the LMC will only be visible to HESS [48] and CAN-GAROO III [49] due to its position in the sky. However, the zenith-angle dependence of the effective area of these instruments greatly decreases the prospects for detection.…”

Section: The γ-Ray Emissionmentioning

confidence: 99%

Gamma-ray and synchrotron emission from neutralino annihilation in the Large Magellanic Cloud

Tasitsiomi

2004

Astroparticle Physics

View full text Add to dashboard Cite

We calculate the expected flux of γ-ray and radio emission from the LMC due to neutralino annihilation. Using rotation curve data to probe the density profile and assuming a minimum disk, we describe the dark matter halo of the LMC using models predicted by N-body simulations. We consider a range of density profiles including the NFW profile, a modified NFW profile proposed by Hayashi et al. (2003) to account for the effects of tidal stripping, and an isothermal sphere with a core. We find that the γ-ray flux expected from these models may be detectable by GLAST for a significant part of the neutralino parameter space. The prospects for existing and upcoming Atmospheric Cherenkov Telescopes (ACTs) are less optimistic, as unrealistically long exposures are required for detection. However, the effects of adiabatic compression due to the baryonic component may improve the chances for detection by ACTs. The maximum flux we predict is well below EGRET's measurements and thus EGRET does not constrain the parameter space. The expected synchrotron emission generally lies below the observed radio emission from the LMC in the frequency range of 19.7 to 8550 MHz. As long as σv < 2 × 10 −26 cm 3 s −1 for a neutralino mass of 50 GeV, the observed radio emission is not primarily due to neutralinos and is consistent with the assumption that the main source is cosmic rays. We find that the predicted fluxes, obtained by integrating over the entire LMC, are not very strongly dependent on the inner slope of the halo profile, varying by less than an order of magnitude for the range of profiles we considered.

show abstract

Section: The γ-Ray Emissionmentioning

confidence: 99%

Gamma-ray and synchrotron emission from neutralino annihilation in the Large Magellanic Cloud

Tasitsiomi

2004

Astroparticle Physics

View full text Add to dashboard Cite

show abstract

“…Their main advantage is the relatively modest investment and ready availability of mirror collectors of up to a few 1000 m 2 , while their main deficiency is a very modest γ /h separation and a rather restricted collection area. Other groups aim for new, optimized ACTs by either bundling telescopes of the proven 10 m class to stereo systems such as CANGAROO III [39], HESS [40] and VERITAS [41] or for a single very large mirror, MAGIC [42] and MACE [43]. These experiments will have thresholds of between 15 and 50 GeV, very high γ /h separation, collection areas up to 1 km 2…”

Section: The Next Generation Of Actsmentioning

confidence: 99%

Status of ground-based GeV/TeV gamma ray astronomy

Lorenz¹

2001

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

View full text Add to dashboard Cite

show abstract

“…The Imaging Atmospheric Cherenkov Telescope (IACT) is the technique that currently achieves the highest sensitivity in the VHE gamma-ray observations. Gamma-ray astronomy has experienced a major breakthrough with the impressive astrophysical results obtained mainly by the current generation of Cherenkov experiments like HESS [7]- [8], VERITAS [9], MAGIC [10], and CANGAROO [11]. IACT gamma-ray astronomy observations are, for the moment, limited by non-gamma ray backgrounds at lower energies, and, at higher energy, by the number of photons that can be detected.…”

Section: Introductionmentioning

confidence: 99%

Development of cold-slumping glass mirrors for imaging Cherenkov telescopes

Vernani

Banham

Citterio

et al. 2008

Advanced Optical and Mechanical Technologies in Telescopes and Instrumentation

View full text Add to dashboard Cite

The development of lightweight glass mirrors manufactured via cold-slumping technique for Imaging Atmospheric Cherenkov Telescope is presented. The mirror elements have a sandwich-like structure where the reflecting and backing facets are composed by glass sheets with an interposed honeycomb aluminum core. The reflecting coating is deposited in high vacuum by means of physical vapor deposition and consists of aluminum with an additional protective layer of SiO2. The mirror fabrication and environmental qualification by accelerated ageing, thermal cycling and coating adhesion are presented together with the optical performances measured as angular resolution and reflectivity obtained on spherical, 1 squared meter mirror prototypes

show abstract

The CANGAROO-III project

Cited by 14 publications

References 1 publication

Gamma-ray and synchrotron emission from neutralino annihilation in the Large Magellanic Cloud

Gamma-ray and synchrotron emission from neutralino annihilation in the Large Magellanic Cloud

Status of ground-based GeV/TeV gamma ray astronomy

Development of cold-slumping glass mirrors for imaging Cherenkov telescopes

Contact Info

Product

Resources

About