ИСТИНА

There are two channels of SMBH growth: accretion of infalling material and galaxy mergers leading to the mergers of central black holes. The latter way of growth leads to scaling relations between central black hole mass and intrinsic properties of the host galaxy (e.g. bulge stellar mass, velocity dispersion of stars in a bulge). Our goal is to populate these relations at the low-mass end (<1M MSun including intermediate-mass black holes <200k MSun). We study the environment and internal properties of host galaxies for a sample of 305 IMBH candidates identified by Chilingarian et al. (2018) complemented with slightly more massive black holes. Low-mass BHs tend to reside in low density environments. We followed up over 40 galaxies using the MagE spectrograph (R=6000) and the FourStar NIR imager at the 6.5-m Magellan telescope. We obtained stellar velocity dispersions by using full spectrum fitting and the total bulge stellar masses from the 2D photometric decomposition. Our results demonstrate that host galaxies of AGN powered by low-mass BHs follow scaling relations set by more massive SMBHs for both velocity dispersion and stellar mass. This supports the scenario of BH and host galaxy co-evolution in the low-mass regime.