2025MNRAS.543.3981X

We have conducted a systematic broad-band X-ray timing and spectral analysis of the soft X-ray excess in the narrow-line Seyfert 1 galaxy, Mrk 382, using data from XMM-Newton and NuSTAR observations between 2011 and 2019. A significant soft X-ray excess was detected. Two primary models were employed to fit the broad-band spectra. The warm corona model provided a good fit except in the 3-8 keV band, where residuals are observed in the low-flux state spectrum. Conversely, the relativistically smeared reflection model effectively fitted the entire energy range, including the 3-8 keV hump, which is attributed to relativistically broadened iron K ${\alpha }$ emission. This is confirmed through simulated-spectral analysis. The variability in the spectral features between high- and low-flux states may result from variations in the hot corona's height relative to the black hole and accretion disc. We conclude that the relativistic reflection model provides the most satisfactory explanation for the X-ray production mechanism in Mrk 382.