Fe-rich ejecta in the supernova remnant G352.7-0.1 with Suzaku

TL;DR

This study analyzes Suzaku X-ray data of supernova remnant G352.7-0.1, revealing Fe-rich ejecta and supporting a Type Ia supernova origin through spectral modeling and elemental abundance analysis.

Contribution

First detection of Fe ejecta with a lower ionization time-scale in G352.7-0.1, indicating a Type Ia supernova origin.

Findings

Fe ejecta detected with strong Fe K-shell emission

Elemental abundances of Si, S, Ar, Ca, and Fe are significantly above solar values

Lower ionization time-scale of Fe ejecta supports Type Ia origin

Abstract

In this work, we present results from a $\sim$201.6 ks observation of G352.7$-$0.1 by using the X-ray Imaging Spectrometer onboard {\it Suzaku} X-ray Observatory. The X-ray emission from the remnant is well described by two-temperature thermal models of non-equilibrium ionization with variable abundances with a column density of $N_{\rm H}$ $\sim$ 3.3$\times$10$^{22}$ cm$^{-2}$. The soft component is characterized by an electron temperature of $kT_{\rm e}$ $\sim$ 0.6 keV, an ionization time-scale of $\tau$ $\sim$ 3.4$\times$10$^{11}$ cm$^{-3}$ s, and enhanced Si, S, Ar, and Ca abundances. The hard component has $kT_{\rm e}$ $\sim$ 4.3 keV, $\tau$ $\sim$ 8.8$\times$10$^{9}$ cm$^{-3}$ s, and enhanced Fe abundance. The elemental abundances of Si, S, Ar, Ca, and Fe are found to be significantly higher than the solar values that confirm the presence of ejecta. We detected strong Fe K-shell emission and determined its origin to be the ejecta for the first time. The detection of Fe ejecta with a lower ionization time-scale favor Type Ia origin for this remnant.