  The circumgalactic medium (CGM) plays a vital role in the formation and
evolution of galaxies, acting as a lifeline between galaxies and the
surrounding intergalactic medium (IGM). In this study we leverage a unique
sample of quasar pairs to investigate the properties of the CGM with absorption
line tomography. We present a new sample of medium resolution Keck/ESI,
Magellan/MagE, and VLT/XSHOOTER spectra of 29 quasar pairs at redshift $2 < z <
3$. We supplement the sample with additional spectra of 32 pairs from the
literature, creating a catalog of 61 quasar pairs with angular separations
between 1.7" and 132.9" and projected physical separations ($r_\perp$) between
14 kpc and 887 kpc. We construct a catalog of 906 metal-line absorption
doublets of C IV ($\lambda\lambda 1548, 1550$) with equivalent widths ranging
from 6 m{\AA} $\leq W_{r, 1550} \leq 2053$ m{\AA}. The best fit linear model to
the log-space equivalent width frequency distribution ($\log f(W_r) =
m\log(W_{r}) + b$) of the sample yields coefficients of $m=-1.44\pm0.16$ and
$b=-0.43\pm0.16$. To constrain the projected extent of C IV, we calculate the
transverse autocorrelation function. The flattening of the autocorrelation
function at low $r_\perp$ provides a lower limit for the coherence length of
the metal enriched CGM - on the order of 200 $h^{-1}$ comoving kpc. This
physical size constraint allows us to refine our understanding of the metals in
the CGM, where the extent of C IV in the CGM depends on gas flows, feedback,
timescale of metal injection and mixing, and the mass of the host galaxies.
