2017MNRAS.472..772M

We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs) at z = 5.7-6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of both sources. These sources have luminosities L_Ly α_ ≃ 3 x 10⁴³ erg s^–1, very high rest-frame equivalent widths of EW₀ >= 200 Å and narrow Ly α lines (200-340 km s^–1). VR7 is the most UV-luminous LAE at z > 6.5, with M₁₅₀₀ = -22.5, even brighter in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α line widths increase with Ly α luminosity at z = 5.7, while there are indications that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization. We find a large spread of up to 3 dex in UV luminosity for >L^* LAEs, but find that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity at z = 6.6. Under basic assumptions, we find that several LAEs at z ≃ 6-7 have Ly α escape fractions >= 100 per cent, indicating bursty star formation histories, alternative Ly α production mechanisms, or dust attenuating Ly α emission differently than UV emission. Finally, we present a method to compute ξ_ion, the production efficiency of ionizing photons, and find that LAEs at z ≃ 6-7 have high values of log₁₀(ξ_ion/Hz erg^–1) ≃ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum escape fractions required for reionization.