  Supermassive black hole (SMBH) masses can be measured by resolving the
dynamical influences of the SMBHs on spatially-resolved tracers of the central
potentials. Modern long-baseline interferometers have enabled the use of
molecular gas as such a tracer. We present here Atacama Large
Millimeter/submillimeter Array observations of the elliptical galaxy NGC 7052
at 0.11 arcseconds (37 pc) resolution in the 12CO(2-1) line and 1.3mm continuum
emission. This resolution is sufficient to resolve the region in which the
potential is dominated by the SMBH. We forward model these observations, using
a multi-Gaussian expansion of a Hubble Space Telescope F814W image and
spatially-constant mass-to-light ratio to model the stellar mass distribution.
We infer a SMBH mass of $2.5\pm0.3\times10^9\,\mathrm{M_\odot}$ and a stellar
I-band mass-to-light ratio of $4.6\pm 0.2\,\mathrm{M_\odot/L_{\odot,I}}$
($3\sigma$ confidence intervals). This SMBH mass is significantly larger than
that derived using ionised gas kinematics, which however appear significantly
more kinematically disturbed than the molecular gas. We also show that a
central molecular gas deficit is likely to be the result of tidal disruption of
molecular gas clouds due to the strong gradient in the central gravitational
potential.
