Photometric and kinematic DiskFit models of four nearby spiral galaxies
  We present optical $\textit{BVRI}$ photometry, H$\alpha$ IFU velocity fields,
and H$\alpha$ long-slit rotation curves for a sample of four nearby spiral
galaxies having a range of morphologies and inclinations. We show that the
$\texttt{DiskFit}$ code can be used to model the photometric and kinematic data
of these four galaxies and explore how well the photometric data can be
decomposed into structures like bars and bulges and to look for non-circular
motions in the kinematic data. In general, we find good agreement between our
photometric and kinematic models for most parameters. We find the best
consistency between our photometric and kinematic models for NGC 6674, a
relatively face-on spiral with clear and distinct bulge and bar components. We
also find excellent consistency for NGC 2841, and find a bar $\sim$10$^{\circ}$
south of the disc major axis in the inner 20''. Due to geometric effects caused
by its high inclination, we find the kinematic model for NGC 2654 to be less
accurate than its photometry. We find the bar in NGC 2654 to be roughly
parallel to the major axis of the galaxy. We are unable to photometrically
model our most highly inclined galaxy, NGC 5746, with $\texttt{DiskFit}$ and
instead use the galaxy isophotes to determine that the system contains a bar
$\sim$5$^{\circ}$ to $\sim$10$^{\circ}$ east of the disc major axis. The high
inclination and extinction in this galaxy also prevent our kinematic model from
accurately determining parameters about the bar, though the data are better
modeled when a bar is included.
