Porquet, D and Reeves, JN and Matt, G and Marinucci, A and Nardini, E and Braito, V and Lobban, AP and Ballantyne, DR and Boggs, SE and Christensen, FE and Dauser, T and Farrah, D and Garcia, J and Hailey, CJ and Harrison, F and Stern, D and Tortosa, A and Ursini, F and Zhang, WW (2018) A deep X-ray view of the bare AGN Ark120. IV. XMM-Newton and NuSTAR spectra dominated by two temperature (warm, hot) Comptonization processes. Astronomy & Astrophysics, 609. A42 -?. ISSN 0004-6361

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We perform an X-ray spectral analysis of the brightest and cleanest bare AGN known so far, Ark 120, in order to determine the process(es) at work in the vicinity of the SMBH. We present spectral analysis of data from an extensive campaign observing Ark 120 in X-rays with XMM-Newton (4$\times$120 ks, 2014 March 18-24), and NuSTAR (65.5 ks, 2014 March 22). During this very deep X-ray campaign, the source was caught in a high flux state similar to the earlier 2003 XMM-Newton observation, and about twice as bright as the lower-flux observation in 2013. The spectral analysis confirms the "softer when brighter" behaviour of Ark 120. The four XMM-Newton/pn spectra are characterized by the presence of a prominent soft X-ray excess and a significant FeK$\alpha$ complex. The continuum is very similar above about 3 keV, while significant variability is present for the soft X-ray excess. We find that relativistic reflection from a constant-density, flat accretion disk cannot simultaneously produce the soft excess, broad FeK$\alpha$ complex, and hard X-ray excess. Instead, Comptonization reproduces the broadband (0.3-79 keV) continuum well, together with a contribution from a mildly relativistic disk reflection spectrum. During this 2014 observational campaign, the soft X-ray spectrum of Ark 120 below $\sim$0.5 keV was found to be dominated by Comptonization of seed photons from the disk by a warm ($kT_{\rm e}$$\sim0.5 keV), optically-thick corona (\tau$$\sim$9). Above this energy, the X-ray spectrum becomes dominated by Comptonization from electrons in a hot optically thin corona, while the broad FeK$\alpha$ line and the mild Compton hump result from reflection off the disk at several tens of gravitational radii.