Self-consistent bulge/disk/halo galaxy dynamical modeling using integral
  field kinematics
  We introduce a method for modeling disk galaxies designed to take full
advantage of data from integral field spectroscopy (IFS). The method fits
equilibrium models to simultaneously reproduce the surface brightness, rotation
and velocity dispersion profiles of a galaxy. The models are fully
self-consistent 6D distribution functions for a galaxy with a Sersic-profile
stellar bulge, exponential disk and parametric dark matter halo, generated by
an updated version of GalactICS. By creating realistic flux-weighted maps of
the kinematic moments (flux, mean velocity and dispersion), we simultaneously
fit photometric and spectroscopic data using both maximum-likelihood and
Bayesian (MCMC) techniques. We apply the method to a GAMA spiral galaxy
(G79635) with kinematics from the SAMI Galaxy Survey and deep $g$- and $r$-band
photometry from the VST-KiDS survey, comparing parameter constraints with those
from traditional 2D bulge-disk decomposition. Our method returns broadly
consistent results for shared parameters, while constraining the mass-to-light
ratios of stellar components and reproducing the HI-inferred circular velocity
well beyond the limits of the SAMI data. While the method is tailored for
fitting integral field kinematic data, it can use other dynamical constraints
like central fibre dispersions and \HI circular velocities, and is well-suited
for modelling galaxies with a combination of deep imaging and HI and/or optical
spectra (resolved or otherwise). Our implementation (MagRite) is
computationally efficient and can generate well-resolved models and kinematic
maps in under a minute on modern processors.
