Abundances in the ejecta of core-collapse supernova remnants G350.1−0.3 and G349.7+0.2

We present Suzaku results of the two Galactic supernova remnants (SNRs) G350.1−0.3 and G349.7+0.2. We find Al and Ni Kα lines from both the SNRs for the first time, in addition to previously detected K-shell lines of Mg, Si, S, Ar, Ca, and Fe. The spectra are well described by two optically thin thermal plasmas: a low-temperature (low-kT) plasma in collisional ionization equilibrium and a high-temperature (high-kT) plasma in non-equilibrium ionization. Since the low-kT plasma has solar metal abundances, it is thought to be of interstellar medium origin. The high-kT plasma has super-solar abundances, hence it is likely to be of ejecta origin. The abundance patterns of the ejecta components are similar to those of core-collapse supernovae with progenitor masses of ∼ 15–25 M ⊙ for G350.1−0.3 and ∼ 35–40 M ⊙ for G349.7+0.2. We find extremely high abundances of Ni compared to Fe (Z Ni/Z Fe ∼ 8). Based on the measured column densities between the SNRs and the near sky background, we propose that G350.1−0.3 and G349.7+0.2 are located at distances of 9 ± 3 kpc and 12 ± 5 kpc, respectively. Then the ejecta masses are estimated to be ∼ 13 M ⊙ and ∼ 24 M ⊙ for G350−0.3 and G349.7+0.2, respectively. These values are consistent with the progenitor masses of ∼ 15–25 M ⊙ and ∼ 35–40 M ⊙ for G350.1−0.3 and G349.7+0.2, respectively.