Discovery of X-Ray Emission from a Radio Supernova Remnant G352.7-0.1

Abstract

We report on the first detection of X-rays from the radio supernova remnant (SNR) G352.7-0.1 with the ASCA Galactic Plane Survey Project. An X-ray image with a shell-like morphology similar to that of the radio band and a spectrum with prominent K-shell lines from highly ionized Si, S, and Ar are presented. These features provide convincing evidence that the X-rays are due to a shock-heated optically thin hot plasma. The spectra are represented by a non-equilibrium ionization (NEI) model with an electron temperature of kT ∼ 2.0 keV, an ionization parameter of $\tau\sim10^{11.0}$ cm−3 s, and an absorption of $N_\textrm H \sim 2.9 \times 10^{22}$ cm−2 . We report on evidence of overabundances of Si and S of ∼ 3.7 and ∼ 3.4, relative to the solar values, respectively. The large absorption indicates that G352.7–0.1 is near to the galactic center region and, after removing the absorption, the X-ray flux in the 1–10 keV band is estimated to be $F_\textrm X (1-10 \textrm {kev})\sim1.2\times10^{-11}\textrm {erg cm}^{-2} \textrm s^{-2}$ . Assuming the SNR to be in the Sedov phase and near to the galactic center (8.5 kpc), G352.7-0.1 is estimated to have a SN explosion energy and age of $E_\textrm {SN}\sim 2\times 10^{50}$erg and $t_{\textrm age}\sim 2200$ yr, respectively; hence, it is a middle-aged SNR.