Speaker
Description
The energy spectrum and arrival direction anisotropy of high-energy
cosmic-ray electrons above 1 TeV serve as crucial probes for identifying
nearby acceleration sources. The Tibet AS$\gamma$ experiment, an air
shower array located at an altitude of 4,300 m, aims to observe cosmic-
ray electrons in the energy region above 10 TeV.
In this study, we developed an energy determination method and a
rejection technique for hadronic cosmic rays using Monte Carlo
simulations. By optimizing energy estimation tables specifically for
cosmic-ray electrons, we achieved an energy resolution of 40% at
approximately 10 TeV and 15% at 100 TeV. The energy bias was confirmed
to be within 3% across the entire range from 10 to 100 TeV. Furthermore,
simulations demonstrated that at around 10 TeV, selecting only events
whose shower core hits the area covered by the underground muon
detectors improves the signal-to-noise ratio for background rejection
through muon cuts, even though it results in a reduction of the total
statistics.
In this presentation, we report on the details of these simulation
results and discuss the feasibility of observing cosmic-ray electrons
with the Tibet AS$\gamma$ experiment.
