Seyfert galaxies are spiral or irregular galaxies containing an extremely bright nucleus, most likely caused by a supermassive black hole, that can sometimes outshine the surrounding galaxy. The light from the central nucleus varies in less than a year, which
implies that the emitting region must be less than one light year across. They are named after the astronomer Carl Seyfert, who studied them extensively in the 1940s. They are a subclass of active galactic nuclei.
Seyfert galaxies are characterized by extremely bright nuclei, and spectra which have very bright emission lines of hydrogen, helium, nitrogen, and oxygen. These emission lines exhibit strong Doppler broadening, which implies velocities from 500 to 4000 km/s, and are believed to originate near an accretion disk surrounding the central black hole.
These emission lines may come from the surface of the accretion disk itself, or may come from clouds of gas illuminated
by the central engine in an ionization cone. The exact geometry of the emitting region is difficult to determine due to poor
resolution. However, each part of the accretion disk has a different velocity relative to our line of sight, and the faster
the gas is rotating around the black hole, the broader the line will be. Similarly, an illuminated disk wind also has a position-dependent velocity.
The narrow lines are believed to originate from the outer part of the AGN where velocities are lower, while the broad lines
originate closer to the black hole. This is confirmed by the fact that the narrow lines do not vary detectably, which implies
that the emitting region is large, contrary to the broad lines which can vary on relatively short timescales. Reverberation
mapping is a technique which uses this variability to try to determine the location and morphology of the emitting region.
Seyfert galaxies also show strong emission in the radio, infrared, ultraviolet, and X-ray parts of the spectrum. The radio emission is believed to be synchrotron emission from the jet. The infrared emission is due to radiation in other bands being reprocessed by dust near the nucleus.
The highest energy photons are believed to be created by inverse compton scattering by a high temperature corona near the black hole.
Seyferts were first classified as Type 1 or 2, depending upon whether the spectra show both narrow and broad emission lines,
or only narrow lines. They are now given a fractional classification depending upon the relative strengths of the narrow and
broad components (e.g. Type 1.5 or Type 1.9). The narrow and broad components are believed to both originate from the accretion
disk, but in Type 2 Seyferts it is believed that the broad component is obscured by dust and/or by our viewing angle on the
galaxy. In some Type 2 Seyfert galaxies, the broad component can be observed in polarized light; it is believed that light from the broad-line region is scattered by a hot, gaseous halo surrounding the nucleus, allowing us to view it indirectly. This effect was first discovered by Antonucci and Miller in the
Type 2 Seyfert NGC 1068.