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We present stellar-dynamical measurements of the central supermassive blackhole (SMBH) in the S0 galaxy NGC 307, using adaptive-optics IFU data fromVLT-SINFONI. We investigate the effects of including dark-matter haloes as wellas multiple stellar components with different mass-to-light (M/L) ratios in thedynamical modeling. Models with no halo and a single stellar component yield arelatively poor fit with a low value for the SMBH mass ($7.0 \pm 1.0 \times10^{7} M_{\odot}$) and a high stellar M/L ratio (K-band M/L = $1.3 \pm 0.1$).Adding a halo produces a much better fit, with a significantly larger SMBH mass($2.0 \pm 0.5 \times 10^{8} M_{\odot}$) and a lower M/L ratio ($1.1 \pm 0.1$).A model with no halo but with separate bulge and disc components produces asimilarly good fit, with a slightly larger SMBH mass ($3.0 \pm 0.5 \times10^{8} M_{\odot}$) and an identical M/L ratio for the bulge component, thoughthe disc M/L ratio is biased high (disc M/L $ = 1.9 \pm 0.1$). Adding a halo tothe two-stellar-component model results in a much more plausible disc M/L ratioof $1.0 \pm 0.1$, but has only a modest effect on the SMBH mass ($2.2 \pm 0.6\times 10^{8} M_{\odot}$) and leaves the bulge M/L ratio unchanged. Thissuggests that measuring SMBH masses in disc galaxies using just a singlestellar component and no halo has the same drawbacks as it does for ellipticalgalaxies, but also that reasonably accurate SMBH masses and bulge M/L ratioscan be recovered (without the added computational expense of modeling haloes)by using separate bulge and disc components.

NGC 307 and the Effects of Dark-Matter Haloes on Measuring Supermassive Black Holes in Disc Galaxies