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We investigate the properties of $z$=2.23 H$\alpha$ and [OIII]$\lambda$5007emitters using the narrow-band-selected samples obtained from the High-$z$Emission Line Survey (HiZELS: Sobral et al. 2013). We construct two samples ofthe H$\alpha$ and [OIII] emitters and compare their integrated physicalproperties. We find that the distribution of stellar masses, dust extinction,star formation rates (SFRs), and specific SFRs, is not statistically differentbetween the two samples. When we separate the full galaxy sample into threesubsamples according to the detections of the H$\alpha$ and/or [OIII] emissionlines, most of the sources detected with both H$\alpha$ and [OIII] show ${\rmlog(sSFR_{UV})}$$\gtrsim$-9.5. The comparison of the three subsamples suggeststhat sources with strong [OIII] line emission tend to have the higheststar-forming activity out all galaxies that we study. We argue that the [OIII]emission line can be used as a tracer of star-forming galaxies at highredshift, and that it is especially useful to investigate star-forming galaxiesat $z$$>$3, for which H$\alpha$ emission is no longer observable from theground.

[OIII] emission line as a tracer of star-forming galaxies at high redshifts: Comparison between H$\alpha$ and [OIII] emitters at $z$=2.23 in HiZELS