A Black Hole Mass Determination for the Compact Galaxy Mrk 1216
Jonelle L. Walsh (1), Remco C.E. van den Bosch (2), Karl Gebhardt (3),, Ak{\i}n Y{\i}ld{\i}r{\i}m (2,4), Kayhan G\"ultekin (5), Bernd Husemann (2,6),, Douglas O. Richstone (5) ((1) Texas A, M University, (2) Max Planck, Institute for Astronomy

TL;DR
This study measures the supermassive black hole in galaxy Mrk 1216 using high-resolution spectroscopy and dynamical modeling, revealing an over-massive black hole consistent with local velocity dispersion relations but larger than expected from luminosity and mass correlations.
Contribution
First detailed black hole mass measurement in Mrk 1216 using integral-field spectroscopy and orbit-based dynamical models, highlighting its over-massiveness relative to bulge properties.
Findings
Black hole mass of (4.9±1.7)×10^9 M_sun
Consistent with local M-sigma relation
Over-massive compared to M-L and M-M relations
Abstract
Mrk 1216 is a nearby, early-type galaxy with a small effective radius of 2.8 kpc and a large stellar velocity dispersion of 308 km/s for its K-band luminosity of 1.4x10^11 L_sun. Using integral-field spectroscopy assisted by adaptive optics from Gemini North, we measure spatially resolved stellar kinematics within ~450 pc of the galaxy nucleus. The galaxy exhibits regular rotation with velocities of \pm 180 km/s and a sharply peaked velocity dispersion profile that reaches 425 km/s at the center. We fit axisymmetric, orbit-based dynamical models to the combination of these high angular resolution kinematics, large-scale kinematics extending to roughly three effective radii, and Hubble Space Telescope imaging, resulting in a constraint of the mass of the central black hole in Mrk 1216. After exploring several possible sources of systematics that commonly affect stellar-dynamical black…
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