Notes. (1) Time intervals where the Fe K emission is measured by fitting a Gaussian. (i), (ii), and (iii) are intervals during the main flare indicated in Fig. 4, and the 94–98 ks interval is where the sharp rise in line core flux occurs, as examined in Sect. 3.3.3. (2) Gaussian centroid energy in keV, measured in the rest frame. (3) Line width represented by Gaussian dispersion in keV. (4) Line intensity in units of 10^-5 phcm^-2s^-1. (5) Line equivalent width in keV. The narrow line in interval (i) was investigated using the spectrum with a 200-eV resolution.