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A study of [S III]$\lambda\lambda9096,9532$ emitters at $z$ = 1.34 and 1.23is presented using our deep narrow-band $H_2S1$ (centered at 2.13 $\mu$m)imaging survey of the Extended Chandra Deep Field South (ECDFS). We combine ourdata with multi-wavelength data of ECDFS to build up spectral energydistributions (SEDs) from the $U$ to the $K_{s}$-band for emitter candidatesselected with strong excess in $H_2S1 - K_{s}$ and derive photometricredshifts, line luminosities, stellar masses and extinction. A sample of 14 [SIII] emitters are identified with $H_2S1<22.8$ and $K_{\rm s}<24.8$ (AB) over381 arcmin$^{2}$ area, having [S III] line luminosity $L_{[SIII]}= \sim10^{41.5-42.6}$erg s$^{-1}$. None of the [S III] emitters is found to haveX-ray counterpart in the deepest Chandra 4 Ms observation, suggesting that theyare unlikely powered by AGN. HST/ACS F606W and HST/WFC3 F160W images show theirrest-frame UV and optical morphologies. About half of the [S III] emitters aremergers and at least one third are disk-type galaxies. Nearly all [S III]emitters exhibit a prominent Balmer break in their SEDs, indicating thepresence of a significant post-starburst component. Taken together, our resultsimply that both shock heating in post-starburst and photoionization caused byyoung massive stars are likely to excite strong [S III] emission lines. Weconclude that the emitters in our sample are dominated by star-forming galaxieswith stellar mass $8.7<\log (M/M_{sun})<9.9$.

The nature of [S III]{\lambda}{\lambda}9096, 9532 emitters at z = 1.34 and 1.23