  Stellar coronal mass ejections remain experimentally unconstrained, unlike
their stellar flare counterparts which are observed ubiquitously across the
electromagnetic spectrum. Low frequency radio bursts in the form of a type II
burst offer the best means of identifying and constraining the rate and
properties of stellar CMEs. CME properties can be further improved through the
use of proposed solar-stellar scaling relations and multi-wavelength
observations of CMEs through the use of type II bursts and the associated flare
expected to occur occur alongside. We report on 20 hours of observation of the
nearby, magnetically active, and well characterized M dwarf star EQ Peg. The
observations are simultaneously observed with the Jansky Very Large Array at
their P-band (230-470 MHz) and at the Apache Point observatory in the SDSS u'
filter ($\lambda$ = 3557 \AA). Dynamic spectra of the P band data, constructed
to search for signals in the frequency-time domains, did not reveal evidence
for drifting radio bursts that could be ascribed to type II bursts. Given the
sensitivity of our observations, we are able to place limits on the brightness
temperature and source size of any bursts which may have occurred. Using solar
scaling rations on four observed stellar flares, we predict CME parameters.
Given the constraints on coronal density and photospheric field strength, our
models suggest that the observed flares would have been insufficient to produce
detectable type II bursts at our observed frequencies. We consider the
implications of these results, and other recent findings, on stellar mass loss.
