2014/02/14 by F. X. An, X. Z. Zheng, Y. Z. Meng +3 · 1 citation
Physics and Astronomy · #astro-ph.GA #astro-ph.CO
paper · pdf · doi:10.1007/s11433-013-5331-y
published as SCIENCE CHINA Physics, Mechanics & Astronomy, 2013, 56(11): 2226-2235 · 9 pages, 3 figures, 4 tables, published in SCIENCE CHINA Physics, Mechanics & Astronomy
arxiv created 2014/02/14 · arxiv updated 2014/02/18
A study of [S III]λλ9096,9532 emitters at z = 1.34 and 1.23 is presented using our deep narrow-band H2S1 (centered at 2.13 μm) 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 Ks-band for emitter candidates selected with strong excess in H2S1 - Ks and derive photometric redshifts, line luminosities, stellar masses and extinction. A sample of 14 [S III] emitters are identified with H2S1<22.8 and K\rm s<24.8 (AB) over 381 arcmin2 area, having [S III] line luminosity L[SIII]= ∼ 1041.5-42.6erg 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/Msun)<9.9.