  We present a new constraint on the mass of the black hole in the active S0
galaxy NGC 5273. Due to the proximity of the galaxy at $16.6 \pm 2.1$ Mpc, we
were able to resolve and extract the bulk motions of stars near the central
black hole using AO-assisted observations with Gemini NIFS, as well as
constrain the large-scale kinematics using re-reduced archival SAURON
spectroscopy. High resolution HST imaging allowed us to generate a surface
brightness decomposition, determine approximate mass-to-light ratios for the
bulge and disk, and obtain an estimate for the disk inclination. We constructed
an extensive library of dynamical models using the Schwarzschild
orbit-superposition code FORSTAND, exploring a range of disk and bulge shapes,
halo masses, etc. We determined a black hole mass of $M_{\bullet} = [0.5 - 2]
\times 10^{7}$ $M_{\odot}$, where the low side of the range is in agreement
with the reverberation mapping measurement of $M_{\bullet} = [4.7 \pm 1.6]
\times 10^{6}$ $M_{\odot}$. NGC 5273 is one of only a small number of nearby
galaxies hosting broad-lined AGN, allowing crucial comparison of the black hole
masses derived from different mass measurement techniques.
