  Using standard 1D-LTE model atmosphere analysis, we provide an in-depth
investigation of iron abundance as derived from neutral and singly ionization
iron lines (Fe {\scriptsize{I, II}}) in nearby star clusters. Specifically, we
replicate the discrepancy regarding $\Delta$[Fe/H], wherein the difference of
Fe {\scriptsize{II}} - Fe {\scriptsize{I}} increases for stars of the same
cluster with decreasing $T_\mathrm{eff}$, reaching an astonishing 1.0 dex at
$T_\mathrm{eff}$ $\thicksim$ 4000 K. Previous studies have investigated this
anomaly in the Pleiades and Hyades clusters with no concrete solution. In this
analysis, we probe two samples: 63 wide binary field stars where the primary
star is of sun-like temperatures and the secondary is a K-dwarf, ranging from
4231 K $\leq$ $T_\mathrm{eff}$ $\leq$ 6453 K, and 33 Hyades stars of
temperatures 4268 K $\leq$ $T_\mathrm{eff}$ $\leq$ 6072 K. Previous studies
have found discrepancies on the order of 1.0 dex. However, we find that these
studies have neglected line-blending effects of certain Fe {\scriptsize{II}}
lines, namely $\lambda$ = \{4508.29 \AA, 4993.34 \AA, 5197.58 \AA, 5325.55 \AA,
5425.26 \AA, 6456.38 \AA\}. When these lines are removed from the line-list, we
find $\Delta$[Fe/H] decreases to $\thicksim$ 0.6 dex in the field binaries and
$\thicksim$ 0.3 dex in the Hyades. The reason for this remaining trend is
investigated by probing NLTE effects, as well as age and activity
considerations using Ca {\scriptsize{II}} H+K emission and Li absorption, but
these results appear to be small to negligible.
