Fe-RICH EJECTA IN THE SUPERNOVA REMNANT G352.7-0.1 WITH SUZAKU

In this work, we present results from a similar to 201.6 ks observation of G352.7-0.1 using the X-ray Imaging Spectrometer on board 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-H similar to 3.3 x 10(22) cm(-2). The soft component is characterized by an electron temperature of kT(e) similar to 0.6 keV, an ionization timescale of tau similar to 3.4 x 10(11) cm(-3) s, and enhanced Si, S, Ar, and Ca abundances. The hard component has kT(e) similar to 4.3 keV, tau similar to 8.8 x 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 timescale favors a Type Ia origin for this remnant.