Marinucci, A.A.MarinucciBIANCHI, SIMONESIMONEBIANCHIBRAITO, ValentinaValentinaBRAITODe Marco, B.B.De MarcoMatt, G.G.MattMiddei, R.R.MiddeiNARDINI, EMANUELEEMANUELENARDINIReeves, J. N.J. N.Reeves2022-06-172022-06-1720200035-8711http://hdl.handle.net/20.500.12386/32400We report on one of the brightest flux levels of the Seyfert 2 galaxy NGC 2992 ever observed in X-rays, on 2019 May. The source has been monitored every few days from 2019 March 26 to 2019 December 14 by Swift-X-Ray Telescope (XRT), and simultaneous XMM-Newton (250 ks) and NuSTAR (120 ks) observations were triggered on 2019 May 6. The high count rate of the source (its 2-10 keV flux ranged between 0.7 and 1.0 × 10<SUP>-10</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>) allows us to perform a time-resolved spectroscopy, probing spatial scales of tens of gravitational radii from the central black hole. By constructing a map of the excess emission over the primary continuum, we find several emission structures in the 5.0-7.2 keV energy band. From fitting the 50 European Photon Imaging Camera (EPIC)-pn spectral slices of ∼5 ks duration, we interpret them as a constant narrow iron Kα line and three variable components in the iron K complex. When a self-consistent model accounting for the accretion disc emission is considered (KYNRLINE), two of these features (in the 5.0-5.8 and 6.8-7.2 keV bands) can be ascribed to a flaring region of the accretion disc located at r<SUB>in</SUB> ≃ 15-40r<SUB>g</SUB> from the black hole. The third one (6.5-6.8 keV) is likely produced at much larger radii (r<SUB>in</SUB> > 50r<SUB>g</SUB>). The inner radius and the azimuthal extension retrieved from the co-added spectra of the flaring states are r<SUB>in</SUB> = 15 ± 3r<SUB>g</SUB> and ϕ = 165°-330°, suggesting that the emitting region responsible for the broad iron K component is a relatively compact annular sector within the disc. Our findings support a physical scenario in which the accretion disc in NGC 2992 becomes more active at high accretion rates ( $L_{\rm bol}/L_{\rm Edd}\ge 4$ per cent).STAMPAenArticle10.1093/mnras/staa1683https://academic.oup.com/mnras/article/496/3/3412/5857190?login=truehttp://arxiv.org/abs/2006.05280v12020MNRAS.496.3412MFIS/05 - ASTRONOMIA E ASTROFISICA