  We present a spectral and temporal analysis of XMM-Newton data from a sample
of six galaxies (NGC 3783, Mrk 279, Mrk 766, NGC 3227, NGC 7314, and NGC 3516).
Using the hardness-ratio curves, we identify time-intervals in which clouds are
eclipsing the central X-ray source in five of the six sources. We detect three
occultations in NGC 3227 and one occultation in NGC 3783, NGC 7314, and NGC
3516, together with the well-known occultations in Mrk 766. We estimate the
physical properties of the eclipsing clouds. The derived physical size of the
X-ray sources ($\sim$(3-28)$\times$10$^{13}$ cm) is less than that of the
eclipsing clouds with column densities of $\sim$10$^{22}$-10$^{23}$ cm$^{-2}$,
thus a single cloud may block the X-ray source, leading to notorious temporal
variability of the X-ray flux. The eclipsing clouds in Mrk 766, NGC 3227, NGC
7314, and NGC 3516 with distances from the X-ray source of
$\sim$(0.3-3.6)$\times$10$^4$ $R_g$ are moving at Keplerian velocities $>$1122
km s$^{-1}$, typical parameters of broad-line region clouds, while the
eclipsing cloud in NGC 3783 is likely located in the dusty torus. We also find
a good anti-correlation with a slope of -187$\pm$62 between the known masses of
the supermassive black hole in the center of the galaxies with the equivalent
width (EW) of the 6.4 keV Fe line for the five Seyfert 1 galaxies of our
sample, while the Seyfert 2 galaxy NGC 7314 shows an average EW value of
100$\pm$11 eV inconsistent with the above anti-correlation.
