  We present the results from a coordinated XMM-Newton $+$ NuSTAR observation
of the Seyfert 1 Galaxy ESO 511$-$G030. With this joint monitoring programme,
we conduct a detailed variability and spectral analysis. The source remained in
a low flux and very stable state throughout the observation period, although
there are slight fluctuations of flux over long timescales. The broadband
(0.3-78~keV) spectrum shows the presence of a power-law continuum with a soft
excess below 2~keV, a relatively narrow iron K$\alpha$ emission
($\sim$6.4~keV), and an obvious cutoff at high energies. We find that the soft
excess can be modeled by two different possible scenarios: a warm ($kT_{\rm e}
\sim$ 0.19~keV) and optically thick ($\tau - 18\sim25$) Comptonizing corona or
a relativistic reflection from a high-density ($\log [n_{\rm e}/{\rm
cm}^{-3}]=17.1 \sim 18.5$) inner disc. All models require a low temperature
($kT_{\rm e} \sim$ 13~keV) for the hot corona.
