The nature of [S III]λλ9096, 9532 emitters at z = 1.34 and 1.23

Abstract

A study of [S III]$\lambda \lambda 9096,9532$ emitters at $z$ = 1.34 and 1.23 is presented using our deep narrow-band $H_{2}S1$ (centered at 2.13 $\mu$m) imaging survey of the Extended Chandra Deep Field South (ECDFS). We combine our data with multi-wavelength data of ECDFS to build up spectral energy distributions (SEDs) from the $U$ to the $K_s$-band for emitter candidates selected with strong excess in $H_{2}S1-K_s$ and derive photometric redshifts, line luminosities, stellar masses and extinction. A sample of 14 [S III] emitters are identified with $H_{2}S1<22.8$ and $K_{\mathrm{s}}<24.8$ (AB) over 381 arcmin${}^2$ area, having [S III] line luminosity $L_{[SIII]}=\sim 10^{41.5-42.6}$erg s${}^{-1}$. None of the [S III] emitters is found to have X-ray counterpart in the deepest Chandra 4 Ms observation, suggesting that they are unlikely powered by AGN. HST/ACS F606W and HST/WFC3 F160W images show their rest-frame UV and optical morphologies. About half of the [S III] emitters are mergers and at least one third are disk-type galaxies. Nearly all [S III] emitters exhibit a prominent Balmer break in their SEDs, indicating the presence of a significant post-starburst component. Taken together, our results imply that both shock heating in post-starburst and photoionization caused by young massive stars are likely to excite strong [S III] emission lines. We conclude that the emitters in our sample are dominated by star-forming galaxies with stellar mass $8.7<\log (M/M_{sun})<9.9$.

9 pages, 3 figures, 4 tables, published in SCIENCE CHINA Physics, Mechanics & Astronomy

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