CALIBRATING STELLAR VELOCITY DISPERSIONS BASED ON SPATIALLY RESOLVED H-BAND SPECTRA FOR IMPROVING THE M-BH-sigma(*) RELATION

To calibrate stellar velocity dispersion measurements from optical and near-IR stellar lines, and to improve the black hole mass (M-BH)-stellar velocity dispersion (sigma(*)) relation, we measure sigma(*) based on high-quality H-band spectra for a sample of 31 nearby galaxies, for which dynamical M-BH is available in the literature. By comparing velocity dispersions measured from stellar lines in the H-band with those measured from optical stellar lines, we find no significant difference, suggesting that optical and near-IR stellar lines represent the same kinematics and that dust effect is negligible for early-type galaxies. Based on the spatially resolved rotation and velocity dispersion measurements along the major axis of each galaxy, we find that a rotating stellar disk is present for 80% of galaxies in the sample. For galaxies with a rotation component, sigma(*) measured from a single aperture spectrum can vary by up to similar to 20%, depending on the size of the adopted extraction aperture. To correct for the rotational broadening, we derive luminosity-weighted sigma(*) within the effective radius of each galaxy, providing uniformly measured velocity dispersions to improve the M-BH-sigma(*) relation.Astronomy & AstrophysicsSCI(E)12ARTICLE1null76