Extending the Sensitivity of Air Cerenkov Telescopes

Abstract

Over the last decade, the Imaging Air Cerenkov technique has proven itself to be an extremely powerful means to study very energetic gamma-radiation from a number of astrophysical sources in a regime which is not practically accessible to satellite-based instruments. The further development of this approach in recent years has generally concentrated on increasing the density of camera pixels, increasing the mirror area and using multiple telescopes. Here we present a practical method to substantially improve the sensitivity of Atmospheric Cerenkov Telescopes using wide-field cameras with a relatively course density of photomultiplier tubes. The 2-telescope design considered here is predicted to be more than ~3 times more sensitive than existing/planned arrays in the regime above 300 GeV for continuously emitting sources; up to ~10 times more sensitive for hour-scale emission (relevant for episodic sources, such as AGN); significantly more sensitive in the regime above 10 TeV; and possessing a sky coverage which is roughly an order of magnitude larger than existing instruments. It should be possible to extend this approach for even further improvement in sensitivity and sky coverage.

Refereed Version Accepted for publication in Astroparticle Physics

References in corpus (1)

• A detailed spectral and morphological study of the gamma-ray supernova remnant RX J1713.7-3946 with H.E.S.S

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• Sensitivity of a proposed space-based Cerenkov astrophysical-neutrino telescope (CHANT)
• Gamma-Ray Lines from Radiative Dark Matter Decay
• Characterisation and Testing of CHEC-M - a camera prototype for the Small-Sized Telescopes of the Cherenkov Telescope Array
• Timing analysis techniques at large core distances for multi-TeV gamma ray astronomy
• Experimental approaches for 100 TeV gamma-ray astronomy
• Design Considerations for the Next Generation of Atmospheric Imaging Cherenkov Telescopes
• A Mini-Imaging Air Cherenkov Telescope
• Simulation studies of the high-energy component of a future imaging Cherenkov telescope array