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In this paper, we investigated the Fe K-shell lines in the supernova remnantW51C and hard X-ray sources in the proximity. We measured the intensities of FeI K$\alpha$ and Fe XXV He$\alpha$ lines at 6.40 keV and 6.68 keV, respectively,and found that the intensity of the 6.68 keV line is consistent with thebackground level expected from previous studies, while that of the 6.40 keVline is higher at the significance level of 2.0${\sigma}$. Given the presenceof gamma-ray emission and high ionization rate point spatially coincident withthe remnant, we conclude that the enhanced 6.40 keV line most likely originatesfrom the interaction between low-energy cosmic rays and molecular clouds. Also,we discovered an enhanced 6.68 keV line emission from the compact H II regionG49.0-0.3 at the significance level of 3.4${\sigma}$. Spectral analysisrevealed that the temperature and abundance of the thermal plasma with the 6.68keV line is $kT = 3.0^{+0.8}_{-0.7}$ keV and $Z = 0.5 \pm 0.2$ solar,respectively. These values are explained by the thermal plasma generated by thestellar winds of O stars.

Suzaku Observations of Fe K-shell Lines in the Supernova Remnant W51C and Hard X-ray Sources in the Proximity