  We present an analysis of \textit{HST}/COS/G160M observations of CIV in the
inner circumgalactic medium (CGM) of a novel sample of eight z$\sim$0,
L$\approx$L$^{\star}$ galaxies, paired with UV-bright QSOs at impact parameters
($R_\mathrm{proj}$) between 25-130 kpc. The galaxies in this
stellar-mass-controlled sample (log$_{10}$M$_{\star}$/M$_{\odot}$ $\sim$
10.2-10.9 M$_{\odot}$) host super-massive black holes (SMBHs) with
dynamically-measured masses spanning log$_{10}$M$_\mathrm{BH}$/M$_{\odot}$
$\sim$ 6.8-8.4; this allows us to compare our results with models of galaxy
formation where the integrated feedback history from the SMBH alters the CGM
over long timescales. We find that the \ion{C}{IV} column density measurements
(N$_{\rm C IV}$) (average log$_{10}$N$_{\rm C IV, CH}$ = 13.94$\pm$0.09
cm$^{-2}$) are largely consistent with existing measurements from other surveys
of N$_{\rm C IV}$ in the CGM (average log$_{10}$N$_{\rm C IV, Lit}$ =
13.90$\pm$0.08 cm$^{-2}$), but do not show obvious variation as a function of
the SMBH mass. In contrast, specific star-formation rate (sSFR) is highly
correlated with the ionized content of the CGM. We find a large spread in sSFR
for galaxies with log$_{10}$M$_\mathrm{BH}$/M$_{\odot}$ $>$ 7.0, where the CGM
\ion{C}{IV} content shows clear dependence on galaxy sSFR but not
M$_\mathrm{BH}$. Our results do not indicate an obvious causal link between CGM
CIV and the mass of the galaxy's SMBH; however through comparisons to the
EAGLE, Romulus25, $\&$ IllustrisTNG simulations, we find that our sample is
likely too small to constrain such causality.
