  With the advent of direct imaging spectroscopy, the number of spectra from
brown dwarfs and extrasolar gas giants is growing rapidly. Many brown dwarfs
and extrasolar gas giants exhibit spectroscopic and photometric variability,
which is likely the result of weather patterns. However, for the foreseeable
future, point-source observations will be the only viable method to extract
brown dwarf and exoplanet spectra. Models have been able to reproduce the
observed variability, but ground truth observations are required to verify
their results. To that end, we provide visual and near-infrared spectra of
Jupiter and Saturn obtained from the \emph{Cassini} VIMS instrument. We
disk-integrate the VIMS spectral cubes to simulate the spectra of Jupiter and
Saturn as if they were directly imaged exoplanets or brown dwarfs. We present
six empirical disk-integrated spectra for both Jupiter and Saturn with phase
coverage of $1.7^\circ$ to $133.5^\circ$ and $39.6^\circ$ to $110.2^\circ$,
respectively. To understand the constituents of these disk-integrated spectra,
we also provide end member (single feature) spectra for permutations of
illumination and cloud density, as well as for Saturn's rings. In tandem, these
disk-integrated and end member spectra provide the ground truth needed to
analyze point source spectra from extrasolar gas giants and brown dwarfs.
Lastly, we discuss the impact that icy rings, such as Saturn's, have on
disk-integrated spectra and consider the feasibility of inferring the presence
of rings from direct imaging spectra.
