  The study of cosmic ray anisotropy in the TeV-PeV energy range could provide
clues about the origin and propagation of cosmic rays in our galactic
neighborhood. Because the observed anisotropy is very small, below the
per-mille level, large event volumes are needed in order to characterize it in
sufficient detail. Over the last six years, the IceCube Observatory has
collected 150 billion cosmic ray induced muon events. This large data sample
made it possible to detect anisotropies in the southern hemisphere, down to the
10$^{-5}$ level, at primary energies in excess of 10 TeV. The observed
anisotropy is not a simple dipole, but it can be described as composed of
multipole components of the spherical harmonic expansion, to about
10$^{\circ}$. A change in topological structure of the cosmic ray arrival
distribution is observed above 100 TeV. Data collected with the air shower
array IceTop above 300 TeV confirm the observations up to the PeV energy scale.
Moreover, the addition of data collected with the AMANDA neutrino telescope,
which operated between 2000 and 2007, has enabled us to search for time
variability in the observed TeV anisotropy.
