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Different massive black hole mass - host galaxy scaling relations suggestthat the growth of massive black holes is entangled with the evolution of theirhost galaxies. The number of measured black hole masses is still limited, andadditional measurements are necessary to understand the underlying physics ofthis apparent co-evolution. We add six new black hole mass (MBH) measurementsof nearby fast rotating early-type galaxies to the known black hole masssample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281 and NGC 7049.Our target galaxies have effective velocity dispersions ({\sigma}e) between 170and 245 km s^(-1), and thus this work provides additional insight into theblack hole properties of intermediate-mass early-type galaxies. We combinehigh-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS andSAURON data from ATLAS3D to derive two-dimensional stellar kinematics maps. Wethen build both Jeans Anisotropic Models and axisymmetric Schwarzschild modelsto measure the central black hole masses. Our Schwarzschild models provideblack hole masses which are consistent with recent MBH-{\sigma}e scalingrelations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constantvelocity dispersion in the center, but we can clearly constrain their lowerblack hole mass limit. We conclude our analysis with a test on NGC 4570 takinginto account a variable mass-to-light ratio (M/L) when constructing dynamicalmodels. When considering M/L variations linked mostly to radial changes in thestellar metallicity, we find that the dynamically determined black hole massfrom NGC 4570 decreases by 30%. Further investigations are needed in the futureto account for the impact of radial M/L gradients on dynamical modeling.

Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations