BH mass versus stellar velocity dispersion (σ_⋆) relation for our simulated dwarfs, which are indicated as coloured squares. The velocity dispersion of the stellar component has been measured inside 0.5 R_eff for each galaxy. Observations from Xiao et al. (2011) are marked by grey points with error bars, with a 0.2 dex scatter as a grey-shaded area. Observations from Baldassare et al. (2020) are marked by black crosses. The green line shows the Martín-Navarro & Mezcua (2018) observational relation obtained for low-mass Seyfert 1 galaxies. All of our simulated galaxies follow fairly well current existing observational relations between the mass of the central SMBH and the velocity dispersion of the galaxy’s stellar component.