There are different Seyfert flavors depending on the presence and intensity of narrow emission lines in their spectra. What is the nature of this distinction is still a subject of discussions and controversies. In this article we concentrate on the sequence, Sy1.0:Sy1.2:Sy1.5 along which the broad component decreases while the narrow component increases. Our sample is composed of 4000 galaxies with redshifts z < 0.40, and optical spectra extracted from SDSS DR7, from which we deduced the physical characteristics of the Sy1 subgroups. We compared this information with the morphology of the hosts and levels of star formation. Along the sequence we found that: 1.- the luminosity of the AGN decreases, the power law flatters and the mass of the black hole (BH) decreases, 2.- the redshift decreases, the morphology changes from early to late-type spirals and star formation increases, 3.- we also found evidence that the AGN winds are ubiquitous and were radiatively launched. These results suggest that the subgroups of Sy1s reflects the star formation histories (SFHs) of their host galaxies, due to different formation processes: while the Sy1.0s formed their stars rapidly building massive bulges and BHs, the Sy1.2s and Sy1.5s built their stars more slowly, leaving most of the gas in their disk. Since more gas went towards the center of the Sy1.0s, their NLRs are relatively depleted in gas, explaining the spectral differences. The fact that there is no difference in AGN winds suggests they did not influenced the SFHs of the galaxies.
Enviado por jp.torrespapaqui@ugto.mx, 2019 Oct