@article{bd6ecb51601b487d8c0e7822956143bf,
title = "The role of galaxies and AGN in reionizing the IGM - III. IGM-galaxy cross-correlations at z ~ 6 from eight quasar fields with DEIMOS and MUSE",
abstract = "We present improved results of the measurement of the correlation between galaxies and the intergalactic medium transmission at the end of reionization. We have gathered a sample of 13 spectroscopically confirmed Lyman-break galaxies (LBGs) and 21 Lyman-α emitters (LAEs) at angular separations 20 arcsec ≤ θ ≤ 10 arcmin (~0.1-4 pMpc at z ~ 6) from the sightlines to eight background z ≥ 6 quasars. We report for the first time the detection of an excess of Lyman-α transmission spikes at ~10-60 cMpc from LAEs (3.2σ) and LBGs (1.9σ).We interpret the datawith an improvedmodel of the galaxy-Lyman-α transmission and two-point cross-correlations, which includes the enhanced photoionization due to clustered faint sources, enhanced gas densities around the central bright objects and spatial variations of the mean free path. The observed LAE(LBG)-Lyman-α transmission spike two-point cross-correlation function (2PCCF) constrains the luminosity-averaged escape fraction of all galaxies contributing to reionization to (fesc)MUV<-12 = 0.14+0.28-0.05 (0.23+0.46 -0.12). We investigate if the 2PCCF measurement can determine whether bright or faint galaxies are the dominant contributors to reionization. Our results show that a contribution from faint galaxies (MUV > -20 (2σ)) is necessary to reproduce the observed 2PCCF and that reionizationmight be driven by different sub-populations around LBGs and LAEs at z ~ 6.",
keywords = "Dark ages, First stars, Galaxies: evolution, Galaxies: high-redshift, Intergalactic medium, Quasars: absorption lines, Reionization",
author = "Meyer, {Romain A.} and Koki Kakiichi and Bosman, {Sarah E.I.} and Ellis, {Richard S.} and Nicolas Laporte and Robertson, {Brant E.} and Ryan-Weber, {Emma V.} and Ken Mawatari and Adi Zitrin",
note = "Funding Information: Some of the data used in this work were taken with the W. M. Keck Observatory on Maunakea, Hawaii, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. This observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Funding Information: The authors thank the anonymous referee for useful comments that improved the manuscript. RAM, SEIB, KK, RSE, and NL acknowledge funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 669253). NL also acknowledges support from the Kavli Foundation. BER acknowledges NASA program HST-GO-14747, contract NNG16PJ25C, and grant 17- ATP17-0034, andNSF award 1828315.ERWacknowledges support from the Australian Research Council Centre of Excellence for All- Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. RAM thanks A. Font-Ribeira and F. Davies for useful discussions. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes ID 060.A-9321(A), 094.B-0893(A), 095.A-0714(A), 097.A-5054(A), 099.A-0682(A), and 0103.A-0140(A). This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. Some of the data used in this work were taken with the W. M. Keck Observatory on Maunakea, Hawaii, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. This observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit ofMaunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST- 0071048. The authors acknowledge the use of the UCL Myriad High Performance Computing Facility (Myriad@UCL), and associated support services, in the completion of this work. The authors acknowledge the use of the following communitydeveloped packages NUMPY (van der Walt, Colbert & Varoquaux 2011), SCIPY (Virtanen et al. 2019), ASTROPY (The Astropy Collaboration 2013, 2018), MATPLOTLIB (Hunter 2007), EMCEE (Foreman- Mackey et al. 2013), and CHAINCONSUMER (Hinton&Hinton 2016). Funding Information: The authors thank the anonymous referee for useful comments that improved the manuscript. RAM, SEIB, KK, RSE, and NL acknowledge funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant agreement No 669253). NL also acknowledges support from the Kavli Foundation. BER acknowledges NASA program HST-GO-14747, contract NNG16PJ25C, and grant 17-ATP17-0034, and NSF award 1828315. ERW acknowledges support from the Australian Research Council Centre of Excellence for All-Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. RAM thanks A. Font-Ribeira and F. Davies for useful discussions. Funding Information: Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes ID 060.A-9321(A), 094.B-0893(A), 095.A-0714(A), 097.A-5054(A), 099.A-0682(A), and 0103.A-0140(A). This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. Funding Information: The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. Publisher Copyright: {\textcopyright} 2020 The Author(s).",
year = "2020",
doi = "10.1093/MNRAS/STAA746",
language = "English (US)",
volume = "494",
pages = "1560--1578",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",
}