The inner mass distribution of late-type spiral galaxies from SAURON
  stellar kinematic maps
  We infer the central mass distributions within 0.4-1.2 disc scale lengths of
18 late-type spiral galaxies using two different dynamical modelling approaches
- the Asymmetric Drift Correction (ADC) and axisymmetric Jeans Anisotropic
Multi-gaussian expansion (JAM) model. ADC adopts a thin disc assumption,
whereas JAM does a full line-of-sight velocity integration. We use stellar
kinematics maps obtained with the integral-field spectrograph SAURON to derive
the corresponding circular velocity curves from the two models. To find their
best-fit values, we apply Markov Chain Monte Carlo (MCMC) method. ADC and JAM
modelling approaches are consistent within 5% uncertainty when the ordered
motions are significant comparable to the random motions, i.e,
$\overline{v_{\phi}}/\sigma_R$ is locally greater than 1.5. Below this value,
the ratio $v_\mathrm{c,JAM}/v_\mathrm{c,ADC}$ gradually increases with
decreasing $\overline{v_{\phi}}/\sigma_R$, reaching $v_\mathrm{c,JAM}\approx 2
\times v_\mathrm{c,ADC}$. Such conditions indicate that the stellar masses of
the galaxies in our sample are not confined to their disk planes and likely
have a non-negligible contribution from their bulges and thick disks.
