Orbital decomposition of CALIFA spiral galaxies
  Schwarzschild orbit-based dynamical models are widely used to uncover the
internal dynamics of early-type galaxies and globular clusters. Here we present
for the first time the Schwarzschild models of late-type galaxies: an SBb
galaxy NGC 4210 and an S0 galaxy NGC 6278 from the CALIFA survey. The mass
profiles within $2\,R_e$ are constrained well with $1\sigma$ statistical error
of $\sim 10\%$. The luminous and dark mass can be disentangled with
uncertainties of $\sim 20\%$ and $\sim 50\%$ respectively. From $R_e$ to
$2\,R_e$, the dark matter fraction increases from $14\pm10\%$ to $18\pm10\%$
for NGC 4210 and from $15\pm10\%$ to $30\pm20\%$ for NGC 6278. The velocity
anisotropy profiles of both $\sigma_r/\sigma_t$ and $\sigma_z/\sigma_R$ are
well constrained. The inferred internal orbital distributions reveal clear
substructures. The orbits are naturally separated into three components: a cold
component with near circular orbits, a hot component with near radial orbits,
and a warm component in between. The photometrically-identified exponential
disks are predominantly made up of cold orbits only beyond $\sim 1\,R_e$, while
they are constructed mainly with the warm orbits inside. Our dynamical hot
components are concentrated in the inner regions, similar to the
photometrically-identified bulges. The reliability of the results, especially
the orbit distribution, are verified by applying the model to mock data.
