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We investigate the dependence of galaxy clustering at $z \sim 4 - 7$ onUV-luminosity and stellar mass. Our sample consists of $\sim$ 10,000Lyman-break galaxies (LBGs) in the XDF and CANDELS fields. As part of ouranalysis, the $M_\star - M_{\rm UV}$ relation is estimated for the sample,which is found to have a nearly linear slope of $d\log_{10} M_\star / d M_{\rmUV} \sim 0.44$. We subsequently measure the angular correlation function andbias in different stellar mass and luminosity bins. We focus on comparing theclustering dependence on these two properties. While UV-luminosity is onlyrelated to recent starbursts of a galaxy, stellar mass reflects the integratedbuild-up of the whole star formation history, which should make it more tightlycorrelated with halo mass. Hence, the clustering segregation with stellar massis expected to be larger than with luminosity. However, our measurementssuggest that the segregation with luminosity is larger with $\simeq 90\%$confidence (neglecting contributions from systematic errors). We compare thisunexpected result with predictions from the \textsc{Meraxes} semi-analyticgalaxy formation model. Interestingly, the model reproduces the observedangular correlation functions, and also suggests stronger clusteringsegregation with luminosity. The comparison between our observations and themodel provides evidence of multiple halo occupation in the small scaleclustering.

Dependence of galaxy clustering on UV-luminosity and stellar mass at $z \sim 4 - 7$