Simulating Cherenkov Telescope Array observation of RX J1713.7-3946

TL;DR

This paper simulates Cherenkov Telescope Array observations of the supernova remnant RX J1713.7-3946 to assess CTA's ability to distinguish between leptonic and hadronic gamma-ray emission mechanisms.

Contribution

It provides the first detailed simulation-based evaluation of CTA's potential to resolve the gamma-ray emission origin in RX J1713.7-3946.

Findings

CTA can differentiate between leptonic and hadronic emission models.

Simulations show CTA's improved sensitivity will clarify the gamma-ray origin.

Results suggest CTA will significantly advance understanding of supernova remnant emissions.

Abstract

We perform simulations of Cherenkov Telescope Array (CTA) observations of a young supernova remnant RX J1713.7-3946. This target is not only one of the brightest sources ever discovered in very high-energy gamma rays but also well observed in other wavebands. In X-rays, the emission is dominated by synchrotron radiation, which links directly to the existence of high-energy electrons. Radio observations of CO and HI gas have revealed a highly inhomogeneous medium surrounding the SNR, such as clumpy molecular clouds. Therefore gamma rays from hadronic interactions are naturally expected. However, the spectrum in GeV energy range measured by Fermi/LAT indicates more typical of leptonic emission from accelerated electrons. Despite lots of multi-wavelength information, the competing interpretations have led to much uncertainty in the quest of unraveling the true origin of the gamma-ray emission from RX~J1713.7--3946. CTA will achieve highest performance ever in sensitivity, angular resolution, and energy resolution. We estimate CTA capability to examine the emission mechanisms of the gamma rays through simulated spatial distribution, spectra, and their time variation.