  In this work, we present the results of a detailed X-ray spectral analysis of
the brightest AGNs detected in the XMM-Newton 1.75 Ms Ultra Narrow Deep Field.
We analyzed 23 AGNs that have a luminosity range of $\sim 10^{42} - 10^{46}\,
\rm{erg}\, \rm{s}^{-1}$ in the $2 - 10\, \rm{keV}$ energy band, redshifts up to
2.66, and $\sim 10,000$ X-ray photon counts in the $0.3 - 10\, \rm{keV}$ energy
band. Our analysis confirms the Iwasawa-Taniguchi effect, an anti-correlation
between the X-ray luminosity ($L_x$) and the Fe-k$\alpha$ Equivalent Width
($EW_{Fe}$) possibly associated with the decreasing of the torus covering
factor as the AGN luminosity increases. We investigated the relationship among
black hole mass ($M_{BH}$), $L_x$, and X-ray variability, quantified by the
Normalized Excess Variance ($\sigma^2_{rms}$). Our analysis suggest an
anti-correlation in both $M_{BH} - \sigma^2_{rms}$ and $L_x- \sigma^2_{rms}$
relations. The first is described as $\sigma^2_{rms} \propto M^{-0.26 \pm
0.05}_{BH}$, while the second presents a similar trend with $\sigma^2_{rms}
\propto L_{x}^{-0.31 \pm 0.04}$. These results support the idea that the
luminosity-variability anti-correlation is a byproduct of an intrinsic
relationship between the BH mass and the X-ray variability, through the size of
the emitting region. Finally, we found a strong correlation among the Eddington
ratio ($\lambda_{Edd}$), the hard X-ray photon index ($\Gamma$), and the
illumination factor $\log(A)$, which is related to the ratio between the number
of Compton scattered photons and the number of seed photons. The
$\log(\lambda_{Edd})-\Gamma-\log(A)$ plane could arise naturally from the
connection between the accretion flow and the hot corona.
