Stereo imaging of the VHE γ-rays with HEGRA & H.E.S.S. (Englisch)

In: AIP Conference Proceedings   ;  558 ,  1  ;  569-573  ;  2001

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At present, the ground-based astronomy of very high energy (VHE) ( E >100  GeV ) γ-rays experiences the challenging transition phase caused by the substantial upgrading of its observational instrumentation. Recently the HEGRA collaboration has evidently demonstrated the power of arrays of imaging atmospheric Čerenkov telescopes and initiated a number of complementary projects, such as H.E.S.S., CANGAROO IV, VERITAS. The common philosophy of those projects is based on the stereoscopic observations of air showers with a number of imaging telescopes simultaneously. Such observations allow to reduce substantially the effective energy threshold of detected γ-ray showers; to improve the angular and energy resolution for individual γ-rays; to gain in suppression of the cosmic ray background. In my talk I have summarized the general advantages and achieved sensitivity of the stereoscopic observations using the HEGRA data taken with an array of 5 imaging telescopes having the energy threshold of 500 GeV. These results completed with the relevant simulations may be extrapolated on a firm ground towards the future H.E.S.S. (phase I) array of four 12 m imaging telescopes with the estimated energy threshold below 100 GeV. Here I discuss in short the anticipated performance of such an array.

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3
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15
Status of VHE astronomy c.2000
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27
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High energy neutrino astronomy: Towards kilometer-scale detectors
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Particle acceleration in supernova remnants
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Theory of high-energy gamma-ray emission of supernova remnants
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115
Gamma-ray pulsars: Models and predictions
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127
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171
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191
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234
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565
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578
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582
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586
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609
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613
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625
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635
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639
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CAT observations of the Blazar MrK421
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RGB 509+056: EGRET’s Highest Energy Detection of a Blazar
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749
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Particle acceleration in magnetic reconnection zones
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823
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827
Test particle acceleration by rotating jet magnetospheres
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831
Jets, disks and spectral states of black holes
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835
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840
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844
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850
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854
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858
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862
Evolving stellar background radiation and gamma-ray optical depth
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866
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870
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878
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