Astrophys. J., 859, 91-91 (2018/June-1)
Complex Lyα profiles in redshift 6.6 ultraluminous Lyα emitters.
SONGAILA A., HU E.M., BARGER A.J., COWIE L.L., HASINGER G., ROSENWASSER B. and WATERS C.
Abstract (from CDS):
We report on a search for ultraluminous Lyα-emitting galaxies (LAEs) at z = 6.6 using the NB921 filter on the Hyper Suprime-Cam on the Subaru telescope. We searched a 30 deg2 area around the north ecliptic pole, which we observed in broadband g', r', i', z', and y' and narrowband NB816 and NB921, for sources with NB921 < 23.5 and z'-NB921 > 1.3. This corresponds to a selection of log L(Lyα) > 43.5 erg s–1. We followed up seven candidate LAEs (out of 13) with the Keck DEIMOS spectrograph and confirmed five z = 6.6 LAEs, one z = 6.6 AGN with a broad Lyα line and a strong red continuum, and one low-redshift ([O III] 5007) galaxy. The five ultraluminous LAEs have wider line profiles than lower-luminosity LAEs, and one source, NEPLA4, has a complex line profile similar to that of COLA1. In combination with previous results, we show that the line profiles of the z = 6.6 ultraluminous LAEs are systematically different from those of lower-luminosity LAEs at this redshift. This result suggests that ultraluminous LAEs generate highly ionized regions of the intergalactic medium in their vicinity that allow the full Lyα profile of the galaxy-including any blue wings-to be visible. If this interpretation is correct, then ultraluminous LAEs offer a unique opportunity to determine the properties of the ionized zones around them, which will help in understanding the ionization of the z ∼ 7 intergalactic medium. A simple calculation gives a very rough estimate of 0.015 for the escape fraction of ionizing photons, but more sophisticated calculations are needed to fully characterize the uncertainties.
© 2018. The American Astronomical Society. All rights reserved.
cosmology: observations - galaxies: distances and redshifts - galaxies: evolution - galaxies: starburst
Table 1: [SHB2018] NEPLAN (Nos NEPLA1-NEPLA5), [SHB2018] NEPAGN N=1, [SHB2018] OIII N=1.
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