  A handful of well-studied Weak-Line Radio Galaxies (WLRGs) have been
traditionally classified as Low Ionization Nuclear Emission-line Regions
(LINERs), suggesting that these two groups of AGNs might be related. In this
paper, we present new optical emission-line measurements for twenty Weak-Line
Radio Galaxies which we supplement with measurements for an additional four
from the literature. Classifying these objects by their emission-line ratios,
we find that 50% of the objects are robustly classified as LINERs while an
additional 25% are likely to be LINERs. Photoionization calculations show that
the Spectral Energy Distribution of the well-studied WLRG 3C 270 (NGC 4261) is
able to produce the observed emission-line ratios, but only if the UV emission
seen by the narrow emission-line gas is significantly higher than that
observed, implying A_V = 2.5-4.2 magnitudes along our line of sight to the
nucleus. From the photoionization calculations, we find that the emission-line
gas must have an ionization parameter between 10^-3.5 and 10^-4.0 and a wide
range in hydrogen density (10^2-10^6 cm^-3) to reproduce the measured
emission-line ratios, similar to the properties inferred for the emission-line
gas in LINERs. Thus, we find that properties of the emission-line gas as well
as the underlying excitation mechanism are indeed similar in LINERs and WLRGs.
By extension, the central engines of accretion-powered LINERs and WLRGs, which
do host an accreting black hole, may be qualitatively similar.
