We report on one of the brightest flux levels of the Seyfert 2 galaxy NGC 2992 ever observed in X-rays , on May 2019 .
The source has been monitored every few days from March 26 , 2019 to December 14 , 2019 by Swift -XRT , and simultaneous XMM- Newton ( 250 ks ) and NuSTAR ( 120 ks ) observations were triggered on May 6 , 2019 .
The high count rate of the source ( its 2-10 keV flux ranged between 0.7 and 1.0 \times 10 ^ { -10 } erg cm ^ { -2 } s ^ { -1 } ) 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 EPIC pn spectral slices of \sim 5 ks duration , we interpret them as a constant narrow iron K \alpha line and three variable components in the iron K complex .
When a self-consistent model accounting for the accretion disk emission is considered ( KYNrline ) , two of these features ( in the 5.0-5.8 keV and 6.8-7.2 keV bands ) can be ascribed to a flaring region of the accretion disk located at { r _ { in } } \simeq 15 -40 r _ { g } from the black hole .
The third one ( 6.5-6.8 keV ) is likely produced at much larger radii ( r _ { in } > 50 r _ { g } ) .
The inner radius and the azimuthal extension retrieved from the coadded spectra of the flaring states are { r _ { in } } = 15 \pm 3 r _ { g } and \phi = 165 ^ { \circ } -330 ^ { \circ } , suggesting that the emitting region responsible for the broad iron K component is a relatively compact annular sector within the disk .
Our findings support a physical scenario in which the accretion disk in NGC 2992 becomes more active at high accretion rates ( L _ { bol } / L _ { Edd } \geq 4 \% ) .