Gaseous Filaments around the Galaxy Mrk 6
Using various techniques of optical observations at the 6-m Russian telescope (direct images, long-slit and 3D spectroscopy), we have studied distribution and motions of the ionized gas in the galaxy Mrk 6 having an active (Seyfert) nucleus. This lenticular galaxy is located at a distance of about 80 Mpc from us. The active galactic nuclei phenomenon is usually associated with capture of the matter by a supermassive black hole in the galactic centre. During this process, a considerable amount of energy is released in the whole range of the electromagnetic spectrum. Due to the specific spatial distribution of the gas and dust matter, the ionizing emission from the nucleus usually is collimated in two broad cones («ionization cones»).
The active nucleus of Mrk 6 is a traditional target of studies of variability
in various spectral ranges;
Images obtained with the 6-m telescope using the
The observed velocity distribution can be explained by suggesting that the gas in the extended filaments rotate on the circular orbits almost orthogonal to the galaxy stellar disc. The study of the spectra of the filament radiation shows that the filaments gas is ionized by the active nucleus similar to that in the inner regions. The whole complex of the obtained data can be explained on the hypothesis that we observe the gas captured by Mrk 6 from the environment and illuminated by the hard radiation of the active nucleus. In this case, the active nucleus is a kind of a «searchlight» allowing the part of a considerably more extended structure of cold gas to be observed; the origin of this external cold gas is still unclear. Deep images obtained with the upgraded 1-m Schmidt telescope of the Byurakan Astrophysical Observatory of the National Academy of Sciences of Armenia demonstrate the absence of any stellar structures (tidal tails, destroyed satellites) associated with the gaseous filaments.
Contact person: Aleksandrina Smirnova
Studies are supported by the RSF grant № 17-12-01335 «Ionized gas in galactic disks and beyond the optical radius».
The upper row shows the direct images in the broadband filters and in the [OIII] and Hα emission lines of the ionized gas.
The lower row shows the observation results obtained with the scanning Fabry-Perot interferometer in the Hα line: the brightness distribution (on the left), the line-of-sight velocity field (in the centre), and velocity distribution after subtracting the circular rotation model in the plane of the galaxy's disc.