  With more than 15 years since the the first radial velocity discovery of a
planet orbiting a Sun-like star, the time baseline for radial velocity surveys
is now extending out beyond the orbit of Jupiter analogs. The sensitivity to
exoplanet orbital periods beyond that of Saturn orbital radii however is still
beyond our reach such that very few clues regarding the prevalence of ice
giants orbiting solar analogs are available to us. Here we simulate the radial
velocity, transit, and photometric phase amplitude signatures of the solar
system giant planets, in particular Uranus and Neptune, and assess their
detectability. We scale these results for application to monitoring low-mass
stars and compare the relative detection prospects with other potential
methods, such as astrometry and imaging. These results quantitatively show how
many of the existing techniques are suitable for the detection of ice giants
beyond the snow line for late-type stars and the challenges that lie ahead for
the detection true Uranus/Neptune analogues around solar-type stars.
