Matzeu, G. A.G. A.MatzeuNARDINI, EMANUELEEMANUELENARDINIParker, M. L.M. L.ParkerReeves, J. N.J. N.ReevesBRAITO, ValentinaValentinaBRAITOPorquet, D.D.PorquetMiddei, R.R.MiddeiKammoun, E.E.KammounLusso, E.E.LussoAlston, W. N.W. N.AlstonGiustini, M.M.GiustiniLobban, A. P.A. P.LobbanJoyce, A. M.A. M.JoyceIgo, Z.Z.IgoEbrero, J.J.EbreroBallo, L.L.BalloSantos-Lleó, M.M.Santos-LleóSchartel, N.N.Schartel2022-06-172022-06-1720200035-8711http://hdl.handle.net/20.500.12386/32401We present joint XMM-Newton and NuSTAR observations of the 'bare' narrow-line Seyfert 1 Ton S180 (z = 0.062), carried out in 2016 and providing the first hard X-ray view of this luminous galaxy. We find that the 0.4-30 keV band cannot be self-consistently reproduced by relativistic reflection models, which fail to account simultaneously for the soft and hard X-ray emission. The smooth soft excess prefers extreme blurring parameters, confirmed by the nearly featureless nature of the Reflection Grating Spectrometer (RGS) spectrum, while the moderately broad Fe K line and the modest hard excess above 10 keV appear to arise in a milder gravity regime. By allowing a different origin of the soft excess, the broad-band X-ray spectrum and overall spectral energy distribution (SED) are well explained by a combination of (a) direct thermal emission from the accretion disc, dominating from the optical to the far/extreme UV; (b) Comptonization of seed disc photons by a warm (kT<SUB>e</SUB> ~ 0.3 keV) and optically thick (τ ~ 10) corona, mostly contributing to the soft X-rays; (c) Comptonization by a standard hot ($kT_{\rm \mathrm{ e}}\gtrsim 100$ keV) and optically thin (τ < 0.5) corona, responsible for the primary X-ray continuum; and (d) reflection from the mid/outer part of the disc. The two coronae are suggested to be rather compact, with $R_{\rm hot}\lesssim R_{\rm warm}\lesssim 10\, r_{\rm g}$. Our SED analysis implies that Ton S180 accretes at super-Eddington rates. This is a key condition for the launch of a wind, marginal (i.e. 3.1σ significance) evidence of which is indeed found in the RGS spectrum.STAMPAenArticle10.1093/mnras/staa20762-s2.0-85092892112https://academic.oup.com/mnras/article/497/2/2352/5871831http://arxiv.org/abs/2007.06575v12020MNRAS.497.2352MFIS/05 - ASTRONOMIA E ASTROFISICA