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We have extensively studied the broadband X-ray spectra of the sourceESO~141--G055 using all available \xmm{} and \nustar{} observations. We detecta prominent soft excess below 2 keV, a narrow Fe line and a Compton hump (>10keV). The origin of the soft excess is still debated. We used two models todescribe the soft excess: the blurred reflection from the ionized accretiondisk and the intrinsic thermal Comptonisation model. We find that both of thesemodels explain the soft excess equally well. We confirm that we do not detectany broad Fe line in the X-ray spectra of this source, although both thephysical models prefer a maximally spinning black hole scenario (a$>$0.96).This may mean that either the broad Fe line is absent or blurred beyonddetection. 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 fromboth ionized and neutral reflection components. The neutral reflector whichsimultaneously describes the narrow Fe K$\alpha$ and the Compton hump has acolumn 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 $\rmN_{H} =20.6^{+1.0}_{-1.0}\times 10^{22} \rm cm^{-2}$ with a covering factor of$0.21^{+0.01}_{-0.01}$.

A broadband X-ray spectral study of the Seyfert 1 galaxy ESO 141--G055 with XMM-Newton and NuSTAR