Journal article
Theoretical study of an LAE-C IV absorption pair at z = 5.7
LA García, E Tescari, EV Ryan-Weber, JSB Wyithe
Monthly Notices of the Royal Astronomical Society Letters | OXFORD UNIV PRESS | Published : 2017
Abstract
We present a theoretical model to predict the properties of an observed z=5.72Lyman a emitter galaxy-C IV absorption pair separated by 1384 comoving kpc h-1. We use the separation of the pair and an outflow velocity/time travelling argument to demonstrate that the observed galaxy cannot be the source of metals for the C IV absorber. We find a plausible explanation for the metal enrichment in the context of our simulations: a dwarf galaxy with M∗= 1.87 × 109M⊙located 119 comoving kpc h-1away with a wind velocity of ~100 km s-1launched at z ~ 7. Such a dwarf (MUV= -20.5) is fainter than the detection limit of the observed example. In a general analysis of galaxy-C IV absorbers, we find galaxie..
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Funding Acknowledgements
Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. This work was supported by the Flagship Allocation Scheme of the NCI National Facility at the ANU. The authors acknowledge CAASTRO for funding and allocating time for the project Diagnosing Hydrogen Reionization with metal absorption line ratios (fy6) during 2015 and 2016. We also thank the anonymous referee for their insightful comments. EVR-W acknowledges ARC DP 1095600.