A. Sezer¹ and F. Gök²

¹TÜBİTAK Space Technologies Research Institute, ODTU Campus, Ankara, 06531, Turkey
²Akdeniz University, Faculty of Education, Department of Secondary Science and Mathematics Education, Antalya, 07058, Turkey

In this work, we present results from a ~201.6 ks observation of G352.7–0.1 using the X-ray Imaging Spectrometer on board SuzakuX-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 ~ 3.3 × 10²² cm^-2. The soft component is characterized by an electron temperature of kT_e ~ 0.6 keV, an ionization timescale of τ ~ 3.4 × 10¹¹ cm^-3 s, and enhanced Si, S, Ar, and Ca abundances. The hard component has kT_e ~ 4.3 keV, τ ~ 8.8 × 10⁹ 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.

Reference
Sezer A and Gök F (2014) Fe-rich Ejecta in the Supernova Remnant G352.7–0.1 with Suzaku. The Astrophysical Journal 790:81.
[doi:10.1088/0004-637X/790/1/81]

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