  The X-ray narrow emission line region (NELR) of the archetypal Seyfert 1
galaxy NGC\,5548 has been interpreted as a single-phase photoionized plasma
that is absorbed by some of the warm absorber components. This scenario
requires those overlaying warm absorber components to have larger distance (to
the central engine) than the X-ray NELR, which is not fully consistent with the
distance estimates found in the literature. Therefore, we reanalyze the
high-resolution spectra obtained in 2013--2014 with the Reflection Grating
Spectrometer (RGS) aboard \textit{XMM}-Newton to provide an alternative
interpretation of the X-ray narrow emission features. We find that the X-ray
narrow emission features in NGC\,5548 can be described by a two-phase
photoionized plasma with different ionization parameters ($\log \xi=1.3$ and
$0.1$) and kinematics ($v_{\rm out}=-50$ and $-400~{\rm km~s^{-1}}$), and no
further absorption by the warm absorber components. The X-ray and optical NELR
might be the same multi-phase photoionized plasma. Both X-ray and optical NELR
have comparable distances, asymmetric line profiles, and the underlying
photoionized plasma is turbulent and compact in size. The X-ray NELR is not the
counterpart of the UV/X-ray absorber outside the line of sight because their
distances and kinematics are not consistent. In addition, X-ray broad emission
features that we find in the spectrum can be accounted for by a third
photoionized emission component. The RGS spectrum obtained in 2016 is analyzed
as well, where the luminosity of most prominent emission lines (the
\ion{O}{vii} forbidden line and \ion{O}{viii} Ly$\alpha$ line) are the same (at
a 1 $\sigma$ confidence level) as in 2013--2014.
