We investigate the potential for the emission lines OV] $lambdalambda$1213.8,1218.3 and HeII $lambda$1215.1 to contaminate flux measurements of Ly$alpha$ $lambda$1215.7 in the extended nebulae of quasars. We have computed a grid of photoionization models with a substantial range in the slope of the ionizing powerlaw (-1.5 $<$ $alpha$ $<$ -0.5), gas metallicity (0.01 $<$ $Z/Z_{odot}$ $<$ 3.0), gas density (1 $<$ $n_H$ $<$ 10$^4$ cm$^{-3}$), and ionization parameter (10$^{-5}$ $<$ U $<$ 1.0). We find the contribution from HeII $lambda$1215.1 to be negligible, i.e., $<$ 0.1 of Ly$alpha$ flux, across our entire model grid. The contribution from OV] $lambdalambda$1213.8,1218.3 is generally negligible when U is low (<10$^{-3}$) and/or when the gas metallicity is low ($Z/Z_{odot}$ < 0.1). However, at higher values of U and Z we find that OV] can significantly contaminate Ly$alpha$, in some circumstances accounting for more than half the total flux of the Ly$alpha$+HeII+OV] blend. We also provide means to estimate the fluxes of OV] $lambdalambda$1213.8,1218.3 and HeII $lambda$1215.1 by extrapolating from other lines. We estimate the fluxes of OV] and HeII for a sample of 107 Type 2 active galaxies at z$>$2, and find evidence for significant (>10%) contamination of Ly$alpha$ fluxes in the majority of cases (84%). We also discuss prospects for using OV] $lambdalambda$1213.8,1218.3 as a diagnostic for the presence of AGN activity in high-z Ly$alpha$ emitters, and caution that the presence of significant OV] emission could impact the apparent kinematics of Ly$alpha$, potentially mimicking the presence of high-velocity gas outflows.
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