  We have extensively studied the broadband X-ray spectra of the source
ESO~141--G055 using all available \xmm{} and \nustar{} observations. We detect
a prominent soft excess below 2 keV, a narrow Fe line and a Compton hump (>10
keV). The origin of the soft excess is still debated. We used two models to
describe the soft excess: the blurred reflection from the ionized accretion
disk and the intrinsic thermal Comptonisation model. We find that both of these
models explain the soft excess equally well. We confirm that we do not detect
any broad Fe line in the X-ray spectra of this source, although both the
physical models prefer a maximally spinning black hole scenario (a$>$0.96).
This may mean that either the broad Fe line is absent or blurred beyond
detection. The Eddington rate of the source is estimated to be $\lambda_{Edd}
\sim 0.31$. In the reflection model, the Compton hump has a contribution from
both ionized and neutral reflection components. The neutral reflector which
simultaneously describes the narrow Fe K$\alpha$ and the Compton hump has a
column density of $\rm N_{H} \geq 7\times 10^{24} \rm cm^{-2} $. In addition,
we detect a partially covering ionized absorption with ionization parameter
$\log \xi/\rm erg cm s^{-1}$ = $0.1^{+0.1}_{-0.1}$ and column density $\rm
N_{H} =20.6^{+1.0}_{-1.0}\times 10^{22} \rm cm^{-2}$ with a covering factor of
$0.21^{+0.01}_{-0.01}$.
