Black Hole Mass Scaling Relations of 10 Pseudo-Bulge Galaxies

Abstract

We present stellar and gas kinematics of 10 pseudo-bulge galaxies, in order to investigate the correlation between black hole mass (MBH) and galaxy properties, i.e., the MBH-σ∗ relation (where σ∗ is stellar velocity dispersion) using high quality spatially resolved spectra. We observed 9 galaxies with the Faint Object Camera and Spectrograph (FOCAS) at the Subaru telescope, and the other with the Inamori Magellan Areal Camera and Spectrograph (IMACS) at the Magellan telescope. For all galaxies, we obtained spatially resolved data along the major axis and we measured the radial velocity and velocity dispersion from stellar continuum and gas emission lines. We do not find a significant evidence that pseudo-bulge galaxies offset from the MBH-σ∗ relation based on the spatially resolved measurements. To investigate the inclination effects on the effective sigma (σe), which defines the MBH-σ∗ relation, we calculated inclinationcorrected σ∗. We suggest to use rotation-free σ∗ especially for galaxies with a rotation dominant bulge, i.e., pseudo-bulges. Additionally, we obtained velocity and velocity dispersion profiles of [OIII] and Hβ emission lines to investigate specific properties of pseudo-bulge galaxies. Gas kinematics are generally following stellar kinematics, which can be well explained by the gravitational potential of the host galaxies.