  We present a relativistic disk reflection model based on the geometry
calculated using analytical formulae for super-Eddington accretion flows. This
model features a slim disk geometry where the inner disk thickness is
proportional to radius, becoming thicker as the mass accretion rate increases.
The slim disk profile reduces the brightness of the blue horn in the Fe K
emission line for a fixed emissivity and significantly changes the intensity
profile for a lamppost geometry. The model is constructed assuming a
spherically symmetric spacetime. It can be used for any kind of sources showing
fluorescent reflection features and predicted to have slim accretion disks,
like slow rotating black holes in X-ray binaries, active galactic nuclei, tidal
disruption events, and neutron star X-ray binaries. To show the capability of
the model, we use the 2017 \textit{NICER} and \textit{NuSTAR} data of the
ultraluminous X-ray transient Swift~J0243.6+6124.
