  We present ultraviolet spectroscopy covering the Ly$\alpha$ + N V complex of
six candidate low-redshift ($0.9 < z < 1.5$) weak emission-line quasars (WLQs)
based on observations with the Hubble Space Telescope. The original systematic
searches for these puzzling Type 1 quasars with intrinsically weak broad
emission lines revealed an $N \approx 100$ WLQ population from optical
spectroscopy of high-redshift ($z > 3$) quasars, defined by a Ly$\alpha$ + N V
rest-frame equivalent width (EW) threshold $< 15.4$ \r{A}. Identification of
lower-redshift ($z < 3$) WLQ candidates, however, has relied primarily on
optical spectroscopy of weak broad emission lines at longer rest-frame
wavelengths. With these new observations expanding existing optical coverage
into the ultraviolet, we explore unifying the low- and high-$z$ WLQ populations
via EW[Ly$\alpha$+NV]. Two objects in the sample unify with high-$z$ WLQs,
three others appear consistent with the intermediate portion of the population
connecting WLQs and normal quasars, and the final object is consistent with
typical quasars. The expanded wavelength coverage improves the number of
available line diagnostics for our individual targets, allowing a better
understanding of the shapes of their ionizing continua. The ratio of
EW[Ly$\alpha$+NV] to EW[MgII] in our sample is generally small but varied,
favoring a soft ionizing continuum scenario for WLQs, and we find a lack of
correlation between EW[Ly$\alpha$+NV] and the X-ray properties of our targets,
consistent with a "slim-disk" shielding gas model. We also find indications
that weak absorption may be a more significant contaminant in low-$z$ WLQ
populations than previously thought.
