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5AF8F89E-9C18-419B-B178-4F3035965251

Nature and Nurture? Comparing Lyα Detections in UV Bright and Fainter [O III]+Hβ Emitters at z8 With Keck/MOSFIRE

Guido Roberts-Borsani, Tommaso Treu, Charlotte Mason, Richard S. Ellis, Nicolas Laporte, Thomas Schmidt, Maruša Bradač, Adriano Fontana, Takahiro Morishita, Paola Santini
arXiv:2207.01629

Submitted on 4 July 2022

Abstract

The 100% detection rate of Lyα in a sample of four luminous z8 galaxies with red Spitzer/IRAC colors suggested objects with unusual ionizing capabilities and the presence of early (re)ionized bubbles in a neutral era. Whether such bubbles are a reflection of enhanced ionizing properties (nature) or an overdense environment (nurture), however, remains an open question. Here we aim to distinguish between these hypotheses with a spectroscopic search for Lyα in five fainter galaxies from the CANDELS-GOODS fields with Keck/MOSFIRE, selected on a similar IRAC excess and UV magnitudes that reflect reduced clustering effects. We detect >4σ line emission in only two targets, placing them at redshifts of zLyα=7.1081 and zLyα=7.9622, with rest-frame EWs of 16-17 A that are 1.5× weaker than those of their bright counterparts. Comparing line detections we find a reduced rate of Lyα emission of 0.400.25+0.30 in the faint sample compared to 1.000.44+0.00 for the bright sample. The lower rate of the faint sample is well-matched by the predicted number of detections derived from simulations of a mostly neutral IGM and an intrinsic EW0,Lyα distribution from z6 galaxies. However, even with an extreme EW model, it is challenging to match the detection rate of the luminous objects. SED-fitting of the faint galaxies indicates generally young, metal- and dust-poor systems, albeit with reduced star-forming properties compared to their luminous counterparts. We argue the enhanced detection rate in UV bright galaxies is likely a byproduct of both extreme ionizing properties as well as environment, where nature and nurture both play an important role. Ultimately, UV emission lines and direct measurements of clustering with JWST are required to resolve the physical nature of this puzzling population.

Preprint

Comment: 14 pages, 4 figures, 2 tables. Submitted to ApJ

Subject: Astrophysics - Astrophysics of Galaxies

URL: https://arxiv.org/abs/2207.01629