  After two years of operation, the High-Altitude Water Cherenkov (HAWC)
Observatory has analyzed the TeV cosmic-ray sky over an energy range between
$2.0$ and $72.8$ TeV. The HAWC detector is a ground-based air-shower array
located at high altitude in the state of Puebla, Mexico. Using 300 light-tight
water tanks, it collects the Cherenkov light from the particles of extensive
air showers from primary gamma rays and cosmic rays. This detection method
allows for uninterrupted observation of the entire overhead sky (2~sr
instantaneous, 8.5~sr integrated) in the energy range from a few TeV to
hundreds of TeV. Like other detectors in the northern and southern hemisphere,
HAWC observes an energy-dependent anisotropy in the arrival direction
distribution of cosmic rays. The observed cosmic-ray anisotropy is dominated by
a dipole moment with phase $\alpha\approx40^{\circ}$ and amplitude that slowly
rises in relative intensity from $8\times10^{-4}$ at 2 TeV to $14\times10^{-4}$
around 30.3 TeV, above which the dipole decreases in strength. A significant
large-scale ($>60^{\circ}$ in angular extent) signal is also observed in the
quadrupole and octupole moments, and significant small-scale features are also
present, with locations and shapes consistent with previous observations.
Compared to previous measurements in this energy range, the HAWC cosmic-ray sky
maps improve on the energy resolution and fit precision of the anisotropy.
These data can be used in an effort to better constrain local cosmic-ray
accelerators and the intervening magnetic fields.
