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We present a detailed spectral analysis of the joint XMM-Newton and NuSTARobservations of the active galactic nuclei (AGN) in the Seyfert 1.5 Galaxy ESO362-G18. The broadband ($0.3\mbox{--}79$ keV) spectrum shows the presence of apower-law continuum with a soft excess below $2$ keV, iron K$\alpha$ emission($\sim 6.4$ keV), and a Compton hump (peaking at $\sim 20$ keV). We find thatthe soft excess can be modeled by two different possible scenarios: a warm($kT_\mathrm{e}\sim0.2$ keV) and optically thick ($\tau\sim34$) Comptonizingcorona; or with relativistically-blurred reflection off a high-density($\log{[n_\mathrm{e}/\mathrm{cm}^{-3}]}>18.3$) inner disk. These two modelscannot be easily distinguished solely from their fit statistics. However, thelow temperature ($kT_\mathrm{e}\sim20$ keV) and the thick optical depth($\tau\sim5$) of the hot corona required by the warm corona scenario areuncommon for AGNs. We also fit a 'hybrid' model, which includes both diskreflection and a warm corona. Unsurprisingly, as this is the most complex ofthe models considered, this provides the best fit, and more reasonable coronalparameters. In this case, the majority of the soft excess flux arises in thewarm corona component. However, based on recent simulations of warm coronae, itis not clear whether such a structure can really exist at the low accretionrates relevant for ESO 362-G18 ($\dot{m}\sim0.015$). This may therefore arguein favor of a scenario in which the soft excess is instead dominated by therelativistic reflection. Based on this model, we find that the data wouldrequire a compact hot corona ($h\sim3\,R_\mathrm{Horizon}$) around a highlyspinning ($a_\star>0.927$) black hole.

The Nature of Soft Excess in ESO 362-G18 Revealed by XMM-Newton and NuSTAR Spectroscopy