  We present an intriguing, serendipitously-detected system consisting of an
S0/a galaxy, which we refer to as the "Kite", and a highly-collimated tail of
gas and stars that extends over 380 kpc and contains pockets of star formation.
In its length, narrowness, and linearity the Kite's tail is an extreme example
relative to known tails. The Kite (PGC 1000273) has a companion galaxy, Mrk
0926 (PGC 070409), which together comprise a binary galaxy system in which both
galaxies host active galactic nuclei. Despite this systems being previously
searched for signs of tidal interactions, the tail had not been discovered
prior to our identification as part of the validation process of the SMUDGes
survey for low surface brightness galaxies. We confirm the kinematic
association between various H$\alpha$ knots along the tail, a small galaxy, and
the Kite galaxy using optical spectroscopy obtained with the Magellan telescope
and measure a velocity gradient along the tail. The Kite shares characteristics
common to those formed via ram pressure stripping ("jellyfish" galaxies) and
formed via tidal interactions. However, both scenarios face significant
challenges that we discuss, leaving open the question of how such an extreme
tail formed. We propose that the tail resulted from a three-body interaction
from which the lowest-mass galaxy was ejected at high velocity.
