Evidence for TeV gamma-ray emission from the shell type SNR RXJ1713.7-3946

TL;DR

This paper reports the detection of TeV gamma-ray emission from the shell-type SNR RXJ1713.7-3946, supporting the presence of ultra-relativistic electrons and providing insights into the remnant's magnetic field and particle acceleration mechanisms.

Contribution

First detection of TeV gamma-ray emission from RXJ1713.7-3946, linking non-thermal X-ray and gamma-ray observations to shock-accelerated electrons.

Findings

Detected TeV gamma-ray emission with 5.6 sigma significance

Estimated gamma-ray flux of approximately 5.3 x 10^{-12} photons cm^{-2} s^{-1}

Inferred magnetic field strength of about 11 microgauss

Abstract

We report the results of TeV gamma-ray observations of the shell type SNR RXJ1713.7-3946 (G347.3-0.5). The discovery of strong non-thermal X-ray emission from the northwest part of the remnant strongly suggests the existence of electrons with energies up to 100 TeV in the remnant, making the SNR a good candidate TeV gamma-ray source. We observed RXJ1713.7-3946 from May to August 1998 with the CANGAROO 3.8m atmospheric imaging Cerenkov telescope and obtained evidence for TeV gamma-ray emission from the NW rim of the remnant with the significance of 5.6 sigma. The observed TeV gamma-ray flux from the NW rim region was estimated to be (5.3 +/- 0.9[statistical] +/- 1.6[systematic]) * 10^{-12} photons cm^{-2} s^{-1} at energies >= 1.8 +/- 0.9 TeV. The data indicate that the emitting region is much broader than the point spread function of our telescope. The extent of the emission is consistent with that of hard X-rays observed by ASCA. This TeV gamma-ray emission can be attributed to the Inverse Compton scattering of the Cosmic Microwave Background Radiation by shock accelerated ultra-relativistic electrons. Under this assumption, a rather low magnetic field of 11 micro gauss is deduced for the remnant from our observation.