  As part of a wider search for radio emission from nearby systems known or
suspected to contain extrasolar planets $\epsilon$ Eridani was observed by the
Jansky Very Large Array (VLA) in the 2-4 GHz and 4-8 GHz frequency bands. In
addition, as part of a separate survey of thermal emission from solar-like
stars, $\epsilon$ Eri was observed in the 8-12 GHz and the 12-18 GHz bands of
the VLA. Quasi-steady continuum radio emission from $\epsilon$ Eri was detected
in the three high-frequency bands at levels ranging from 67-83 $\mu$Jy. No
significant variability is seen in the quasi-steady emission. The emission in
the 2-4 GHz emission, however, is shown to be the result of a circularly
polarized (up to 50\%) radio pulse or flare of a few minutes duration that
occurred at the beginning of the observation. We consider the astrometric
position of the radio source in each frequency band relative to the expected
position of the K2V star and the purported planet. The quasi-steady radio
emission at frequencies $\ge \!8$ GHz is consistent with a stellar origin. The
quality of the 4-8 GHz astrometry provides no meaningful constraint on the
origin of the emission. The location of the 2-4 GHz radio pulse is $>2.5\sigma$
from the star yet, based on the ephemeris of Benedict et al. (2006), it is not
consistent with the expected location of the planet either. If the radio pulse
has a planetary origin, then either the planetary ephemeris is incorrect or the
emission originates from another planet.
