  This study presents the detection of a high-frequency Quasi-Periodic
Oscillation (QPO) in the Seyfert galaxy NGC 1365, based on observational data
obtained by the XMM-Newton in January 2004. Utilizing the Weighted Wavelet
Z-transform (WWZ) and Lomb-Scargle Periodogram (LSP) methods, a QPO signal was
identified at a frequency of 2.19 * 10^-4 Hz (4566 s), with a confidence level
of 3.6 sigma. The signal was notably absent in the lower 0.2-1.0 keV energy
band, with the primary contribution emerging from the 2.0-10.0 keV band, where
the confidence level reached 3.9 sigma. Spectral analysis shows that there are
multiple absorption and emission lines in the high-energy band (> 6 keV). The
correlation between the QPO frequency (f_QPO) and the mass of NGC 1365 central
black hole (M_BH) aligns with the established logarithmic trend observed across
black holes, indicating the QPO is of high frequency. This discovery provides
new clues for studying the generation mechanism of QPO in Seyfert galaxies,
which helps us understand the accretion process around supermassive black holes
and the characteristics of strong gravitational fields in active galactic
nuclei.
