ner_tags: B-Survey I-Survey I-Survey I-Survey B-Survey B-Citation I-Citation I-Citation O B-Dataset I-Dataset I-Dataset I-Dataset O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Dataset I-Dataset I-Dataset I-Dataset O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject B-Citation I-Citation I-Citation O O O O O O O O O
tokens: Evolution of 21-cm Structure (EOS; Mesinger etal. 2016 ) 9 2016 data release. These semi-numerical reionization simulations are 1.6Gpc on a side with a 1024 3 grid and include state-of-the-art subgrid prescriptions for inhomogeneous recombinations and photo-heating suppression of star formation. The 2016 EOS data release corresponds to two simulation runs, with the efficiency of supernovae feedback adjusted to approximately bracket the expected EoR contribution from faint galaxies. The two runs are: Faint galaxies the EoR is driven by galaxies residing in haloes with masses of 10 8 M h / M 10 9 , and is characterized by numerous small cosmic H ii regions. Hereafter we will refer to the EoR morphologies resulting from this simulation as S mall H ii . Bright galaxies the EoR is instead driven by galaxies residing in haloes with masses of M h 10 10 M , and is characterized by spatially more extended H ii structures. We refer to these simulated EoR morphologies as L arge H ii . We note that the L arge H ii ionization fields have a factor of few10times more power on large scales during the EoR, compared to the S mall H ii ionization fields. Although these are two opposite extremes in terms of H ii region sizes, the S mall H ii EoR morphology is likely more realistic (see the discussion in Mesinger etal. 2016 ), and so we use this simulation as our fiducial model. Nevertheless, we include both extremes to explore the dependence of our results on EoR morphology. We construct samples of sightlines through our simulations which are terminated on one end at a halo, and then extended in a random direction through the simulation volume for a distance of 200 comoving Mpc. Along each sightline, we sum the contributions from all encountered H i patches to construct a composite optical depth for the damping wing (e.g. Miralda-Escud 1998 ). We purposefully exclude the H i contribution from pixels 16 comoving Mpc (2 physical Mpc) from the QSO host halo.This corresponds to the minimum possible radius of the H ii region around ULAS1120 inferred from measurements of its near zone (Mortlock etal. 2011 ). We do not explicitly include the flux from the QSO in our reionization maps. Doing so would require assumptions about the QSO lifetime and ionizing luminosity. Neglecting the QSO ionizing contribution implies that the surrounding H ii region could be larger than predicted by our EoR models. For a given a larger surrounding H ii region implies a smaller integrated damping wing optical depth. Thus if the QSO contributes in growing the surrounding H ii region, our modelled optical depths should be associated with even higher values of , shifting the probability distribution functions (PDFs) we present below towards larger . At z 7.1, we select 10 4 identified haloes in the mass range 6 10 11 M h /M 3 10 12 , consistent with the inferred dynamical mass of the host halo of ULASJ1120 (Venemans etal. 2012 ). Importantly, these higher host halo masses, made possible