  Relativistic jets are the most energetic manifestation of the active galactic
nucleus (AGN) phenomenon. AGN jets are observed from the radio through
gamma-rays and carry copious amounts of matter and energy from the sub-parsec
central regions out to the kiloparsec and often megaparsec scale galaxy and
cluster environs. While most spatially resolved jets are seen in the radio, an
increasing number have been discovered to emit in the optical/near-IR and/or
X-ray bands. Here we discuss a spectacular example of this class, the 3C 111
jet, housed in one of the nearest, double-lobed FR II radio galaxies known. We
discuss new, deep Chandra and HST observations that reveal both near-IR and
X-ray emission from several components of the 3C 111 jet, as well as both the
northern and southern hotspots. Important differences are seen between the
morphologies in the radio, X-ray and near-IR bands. The long (over 100 kpc on
each side), straight nature of this jet makes it an excellent prototype for
future, deep observations, as it is one of the longest such features seen in
the radio, near-IR/optical and X-ray bands. Several independent lines of
evidence, including the X-ray and broadband spectral shape as well as the
implied velocity of the approaching hotspot, lead us to strongly disfavor the
EC/CMB model and instead favor a two-component synchrotron model to explain the
observed X-ray emission for several jet components. Future observations with
NuSTAR, HST, and Chandra will allow us to further constrain the emission
mechanisms.
