Galaxy clustering measurements out to redshift z$\sim$8 from Hubble Legacy Fields

Abstract

We present a novel approach for measuring the two-point correlation function of galaxies in narrow pencil beam surveys with varying depths. Our methodology is utilized to expand high-redshift galaxy clustering investigations up to $z\sim 8$ by analyzing a comprehensive sample consisting of $N_g=160$ Lyman break galaxy candidates obtained through optical and near-infrared photometric data within the CANDELS GOODS datasets from the Hubble Space Telescope Legacy Fields. For bright sources with $M_{UV}<-19.8$, we determine a galaxy bias of $b=9.33\pm 4.90$ at $\overline{z}=7.7$ and a correlation length of $r_0=10.74\pm 7.06$ $h^{-1}Mpc$. We obtain similar results for the XDF, with a galaxy bias measurement of $b=8.26\pm 3.41$ at the same redshift for a slightly fainter sample with a median luminosity of $M_{UV}=-18.4$. By comparing with dark-matter halo bias and employing abundance matching, we deduce a characteristic halo mass of $M_h\sim 10^{11.5}{M}_{\odot }$ and a duty cycle close to unity. To validate our approach for variable-depth datasets, we replicate the analysis in a region with near-uniform depth using a standard two-point correlation function estimator, yielding consistent outcomes. Our study not only provides a valuable tool for future utilization in JWST datasets but also suggests that the clustering of early galaxies continues to increase with redshift beyond $z\gtrsim 8$, potentially contributing to the existence of protocluster structures observed in early JWST imaging and spectroscopic surveys at $z\gtrsim 8$.

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