[5] The source of activity in the AGNs is a supermassive black hole (SMBH) lying at the centre of the galaxy.

The 2-10 keV spectrum of NGC 7213 resembles the spectrum of Seyfert I galaxies, but also contains significant emission lines from FeXXV and FeXXVI, which are observed in LINERs and are not present in most classical Seyfert galaxies.

Also, the soft X-ray spectrum of NGC 7213 features collisionally ionized thermal plasma, one more characteristic of LINERs.

This flare showed a fast-rise-exponential-decay pattern and has been suggested to be caused by the tidal disruption of a main sequence star by the black hole at the centre of NGC 7213.

[11] Surrounding the nucleus is a ring of starforming regions, lying at a radius of circa 20 arcseconds.

[6] Although NGC 7213 appears undisturbed in visible light, it shows signs of having undergone a collision or merger when viewed at longer wavelengths, with disturbed patterns of ionized hydrogen including a filament of gas around 64,000 light-years long, itself being part of a larger HI tidal tail southwest of the nucleus.