Detection of 2$-$4 GHz Continuum Emission from $\epsilon$ Eridani
  The nearby star $\rm \epsilon \ Eridani$ has been a frequent target of radio
surveys for stellar emission and extraterrestial intelligence. Using deep $\rm
2-4 \ GHz$ observations with the Very Large Array, we have uncovered a $29 \
\mu {\rm Jy}$ compact, steady continuum radio source coincident with $\rm
\epsilon \ Eridani$ to within 0.06 arcseconds ($\lesssim 2\sigma$; 0.2 au at
the distance of the star). Combining our data with previous high frequency
continuum detections of $\rm \epsilon \ Eridani$, our observations reveal a
spectral turnover at $\rm 6 \ GHz$. We ascribe the $\rm 2-6 \ GHz$ emission to
optically thick, thermal gyroresonance radiation from the stellar corona, with
thermal free-free opacity likely becoming relevant at frequencies below $\rm 1
\ GHz$. The steep spectral index ($\alpha \simeq 2$) of the $\rm 2-6 \ GHz$
spectrum strongly disfavors its interpretation as stellar wind-associated
thermal bremsstrahlung ($\alpha \simeq 0.6$). Attributing the entire observed
$\rm 2-4 \ GHz$ flux density to thermal free-free wind emission, we thus,
derive a stringent upper limit of $3 \times 10^{-11} \ M_{\odot} \ {\rm
yr}^{-1}$ on the mass loss rate from $\rm \epsilon \ Eridani$. Finally, we
report the non-detection of flares in our data above a $5\sigma$ threshold of
$\rm 95 \ \mu Jy$. Together with the optical non-detection of the most recent
stellar maximum expected in 2019, our observations postulate a likely evolution
of the internal dynamo of $\rm \epsilon \ Eridani$.
