The supernova remnant population in the very-high-energy sky: prospects for CTA

TL;DR

This paper uses Monte-Carlo simulations to predict how the upcoming Cherenkov Telescope Array can improve understanding of supernova remnant populations and particle acceleration mechanisms in the very-high-energy gamma-ray range.

Contribution

It introduces a simulation-based approach to forecast CTA's capabilities in studying SNR populations and their particle acceleration properties.

Findings

CTA can constrain the particle spectral slope

CTA can determine the electron-to-proton ratio

Simulations match expected CTA observations

Abstract

The detection of very-high-energy gamma rays from supernova remnant shells testifies of the acceleration of particles at strong shocks. Many aspects of the particle acceleration remain however unclear. The study of individual objects is very helpful, but the study of the entire population of SNRs detected in this range and its characteristics can also bring valuable science. Using Monte-Carlo simulations, the population of shells bright in the TeV and multi-TeV range can be simulated. The results of these simulations aim at being compared with observations of in struments operating in these ranges, such as the Cherenkov Telescope Array (CTA). Our results suggest that CTA should be able to effectively constrain the slope of particles accelerated at SNRs and the electron-to-proton ratio.