Limits to the energy resolution of a single Air Cherenkov Telescope at low energies

TL;DR

This study investigates the fundamental limits of energy resolution in low-energy Cherenkov telescope observations, highlighting the impact of detector parameters, fluctuations, and primary particle type on measurement accuracy.

Contribution

The paper provides a detailed Monte Carlo simulation analysis of Cherenkov photon density fluctuations at low energies, establishing fundamental resolution limits for single telescopes.

Findings

Relative density fluctuations are higher in proton showers.

Limited field of view increases fluctuations.

Energy resolution is not improved by larger mirror sizes.

Abstract

The photon density on the ground is a fundamental quantity in all experiments based on Cherenkov light measurements, e.g. in the Imaging Air Cherenkov Telescopes (IACT). IACT's are commonly and successfully used in order to search and study Very High Energy (VHE) gamma-ray sources. Difficulties with separating primary photons from primary hadrons (mostly protons) in Cherenkov experiments become larger at lower energies. I have calculated longitudinal and lateral density distributions and their fluctuations at low energies basing on Monte Carlo simulations (for vertical gamma cascades and protonic showers) to check the influence of the detector parameters on the possible measurement. Relative density fluctuations are significantly higher in proton than in photon induced showers. Taking into account the limited detector field of view (FOV) implies the changes of these calculated distributions for both types of primary particles and causes an enlargement in relative fluctuations. Absorption due to Rayleigh and Mie scattering has an impact on mean values but does not change relative fluctuations. The total number of Cherenkov photons is more sensitive to the observation height in gamma cascades than in proton showers at low primary energies. The relative fluctuations of the density do not depend on the reflector size in the investigated size range (from 240 m^2 up to 960 m^2). This implies that a single telescope with a mirror area larger than that of the MAGIC telescope cannot achieve better energy resolution than estimated and presented in this paper. The correlations between longitudinal and lateral distributions are much more pronounced for primary gamma-ray than for primary proton showers.