Examinando por Autor "Schartel, N."

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The first broad-band X-ray view of the narrow-line Seyfert 1 Ton S180
(Oxford Academics: Oxford University Press, 2020-07-15) Matzeu, G. A.; Nardini, E.; Parker, M. L.; Reeves, J. N.; Braito, V.; Porquet, D.; Middei, R.; Kammoun, E.; Lusso, E.; Alston, W. N.; Giustini, M.; Lobban, A. P.; Joyce, A. M.; Igo, Z.; Ebrero, J.; Ballo, L.; Santos Lleó, M.; Schartel, N.; European Research Council (ERC); European Commission (EC); Agenzia Spaziale Italiana (ASI); Istituto Nazionale di Astrofisica (INAF); Comunidad de Madrid; National Aeronautics and Space Administration (NASA); Giustini, M. [0000-0002-1329-658X]; Kammoun, E. [0000-0002-0273-218X]; Braito, V. [0000-0002-2629-4989]; Matzeu, G. [0000-0003-1994-5322]; Parker, M. [0000-0002-8466-7317]; Lobban, A. [0000-0002-6433-1357]; Santos Lleo, M. [0000-0001-5948-8360]; Middei, R. [0000-0001-9815-9092]; Igo, Z. [0000-0001-9274-1145]; Alston, W. [0000-0003-2658-6559]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We 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 hardX-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(e) similar to 0.3 keV) and optically thick (tau similar to 10) corona, mostly contributing to the soft X-rays; (c) Comptonization by a standard hot (kT(e) greater than or similar to 100 keV) and optically thin (tau < 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-hot less than or similar to R-warm less than or similar to 10 r(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. 3.1 sigma significance) evidence of which is indeed found in the RGS spectrum.