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

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 $N_{\mathrm{H}}$ $\sim$ 3.3$\times$10${}^{22}$ cm${}^{-2}$. The soft component is characterized by an electron temperature of $k{T}_{\mathrm{e}}$ $\sim$ 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 $k{T}_{\mathrm{e}}$ $\sim$ 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.

5 pages, 2 figures and 2 tables, Accepted for publication in The Astrophysical Journal

References in corpus (1)

• Limits on GRB Prompt Radio Emission Using the LWA1

Cited by in corpus (3)

• The gas-to-extinction ratio and the gas distribution in the Galaxy
• Molecular environment of the thermal composite supernova remnant G352.7$-$0.1
• Typing supernova remnant G352.7$-$0.1 using XMM-Newton X-ray observations