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http://hdl.handle.net/20.500.12386/32400
Titolo: | The lively accretion disc in NGC 2992 - I. Transient iron K emission lines in the high-flux state | Autori: | Marinucci, A. BIANCHI, SIMONE BRAITO, Valentina De Marco, B. Matt, G. Middei, R. NARDINI, EMANUELE Reeves, J. N. |
Data pubblicazione: | 2020 | Rivista: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Numero: | 496 | Fascicolo: | 3 | Da pagina:: | 3412 | Abstract: | We 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). | URI: | http://hdl.handle.net/20.500.12386/32400 | URL: | https://academic.oup.com/mnras/article/496/3/3412/5857190?login=true http://arxiv.org/abs/2006.05280v1 |
ISSN: | 0035-8711 | DOI: | 10.1093/mnras/staa1683 | Bibcode ADS: | 2020MNRAS.496.3412M | Fulltext: | open |
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