  A new instrument was designed to take visible-light (VL) polarized brightness
($pB$) observations of the solar corona during the 14 December 2020 total solar
eclipse. The instrument, called the Coronal Imaging Polarizer (CIP), consisted
of a 16 MP CMOS detector, a linear polarizer housed within a piezoelectric
rotation mount, and an f-5.6, 200 mm DSLR lens. Observations were successfully
obtained, despite poor weather conditions, for five different exposure times
(0.001 s, 0.01 s, 0.1 s, 1 s, and 3 s) at six different orientation angles of
the linear polarizer (0\de, 30\de, 60\de, 90\de, 120\de, and 150\de). The
images were manually aligned using the drift of background stars in the sky and
images of different exposure times were combined using a simple signal-to-noise
ratio cut. The polarization and brightness of the local sky is also estimated
and the observations were subsequently corrected. The $pB$ of the K-corona was
determined using least squares fitting and radiometric calibration was done
relative to the Mauna Loa Solar Observatory (MLSO) K-Cor $pB$ observations from
the day of the eclipse. The $pB$ data was then inverted to acquire the coronal
electron density, $n_e$, for an equatorial streamer and a polar coronal hole,
which agreed very well with previous studies. The effect of changing the number
of polarizer angles used to compute the $pB$ is also discussed and it is found
that the results vary by up to $\sim$ 13\% when using all six polarizer angles
versus only a select three angles.
