Lyman-alpha spectroscopy of extreme [OIII] emitting galaxies at : Implications for Ly visibility and LyC leakage at
arXiv:2012.04697 · doi:10.1093/mnras/stab705
Abstract
Spectroscopic observations of massive galaxies selected to have extremely large [OIII]+H equivalent width (EW Å) have recently revealed large Ly detection rates, in contrast to the weak emission seen in the general population. Why these systems are uniquely visible in Ly at redshifts where the IGM is likely significantly neutral is not clear. With the goal of better understanding these results, we have begun a campaign with MMT and Magellan to measure Ly in galaxies with similar [OIII]+H EWs at . At these redshifts, the IGM is highly ionized, allowing us to clearly disentangle how the Ly properties depend on the [OIII]+H EW. Here we present Ly EWs of galaxies at with intense [OIII]+H line emission (EW Å). Our results demonstrate that strong Ly emission (EW Å) becomes more common in galaxies with larger [OIII]+H EW, reflecting a combination of increasingly efficient ionizing photon production and enhanced transmission of Ly. Among the galaxies with the most extreme [OIII]+H emission (EW Å), we find that strong Ly emission is not ubiquitous, with only per cent of our population showing Ly EW Å. Our data suggest that the range of Ly strengths is related to the observed ellipticity, with those systems that appear edge-on or elongated having weaker Ly emission. We use these results to interpret the anomalous Ly properties seen in galaxies with extreme [OIII]+H emission and discuss implications for the escape of ionizing radiation from these extreme line emitting galaxies.
arXiv comment13 pages, 8 figure, accepted by MNRAS
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