If the emission is the first peak of the [\[O[ii]{}\]]{} doublet at $\lambda_{\rm rest}=3726$Å, we would have detected the second peak (at $\lambda_{\rm rest}=3729$Å) at 2–10$\sigma$ significance at wavelengths clear of sky lines. On the other hand, if the emission is the second peak of the doublet, the centroid of the first peak would be behind the sky line located blueward of the detected line. To examine these possibilities, we performed simulations in which we inserted mock lines representing either the first or second peak of the [\[O[ii]{}\]]{} doublet at the expected positions in the 2D spectrum. The spatial and spectral line profile of the mock line was assumed to be the same as that of the observed emission, and the flux was assigned based on the most unfavorable flux ratio that is physically allowed (i.e., the weakest line possible; 0.35 $<$ $f$([\[O[ii]{}\]]{}$\lambda$3729)/$f$([\[O[ii]{}\]]{}$\lambda$3726) $<$ 1.5; @pradhan06). Our simulation results indicate that due to its low flux and broad line profile, we would not be able to completely rule out the existence of the other line of the doublet based solely on our 2D spectrum. If the detected emission is indeed one of the [\[O[ii]{}\]]{} doublet, the broad line width of 