  We present spectropolarimetric imaging observations of the solar corona at
low frequencies (80 - 240 MHz) using the Murchison Widefield Array (MWA). These
images are the first of their kind, and we introduce an algorithm to mitigate
an instrumental artefact by which the total intensity signal contaminates the
polarimetric images due to calibration errors. We then survey the range of
circular polarization (Stokes V) features detected in over 100 observing runs
near solar maximum during quiescent periods. First, we detect around 700
compact polarized sources across our dataset with polarization fractions
ranging from less than 0.5% to nearly 100%. These sources exhibit a positive
correlation between polarization fraction and total intensity, and we interpret
them as a continuum of plasma emission noise storm (Type I burst) continua
sources associated with active regions. Second, we report a characteristic
"bullseye" structure observed for many low-latitude coronal holes in which a
central polarized component is surrounded by a ring of the opposite sense. The
central component does not match the sign expected from thermal bremsstrahlung
emission, and we speculate that propagation effects or an alternative emission
mechanism may be responsible. Third, we show that the large-scale polarimetric
structure at our lowest frequencies is reasonably well-correlated with the
line-of-sight (LOS) magnetic field component inferred from a global potential
field source surface (PFSS) model. The boundaries between opposite circular
polarization signs are generally aligned with polarity inversion lines in the
model at a height roughly corresponding to that of the radio limb. This is not
true at our highest frequencies, however, where the LOS magnetic field
direction and polarization sign are often not straightforwardly correlated.
