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One of the biggest puzzles regarding the circumgalactic medium (CGM) is thestructure of its cool ($T\sim10^4$ K) gas phase. While the kinematics of quasarabsorption systems suggests the CGM is composed of a population of differentclouds, constraining the clouds' extent and spatial distribution has provenchallenging, both from the theoretical and observational points of view. Inthis work we study the spatial structure of the $z\sim 1$ CGM withunprecedented detail via resolved spectroscopy of giant gravitational arcs. Weput together a sample of Mg II$\lambda\lambda 2796,2803$ detections obtainedwith VLT/MUSE in 91 spatially independent and contiguous sight-lines toward 3arcs, each probing an isolated star-forming galaxy believed to be detected inabsorption. We constrain the coherence scale of this gas ($C_{\rm{length}}$),which represents the spatial scale over which the Mg II equivalent width (EW)remains constant, by comparing EW variations measured across all sight-lineswith empirical models. We find $1.4 <C_{\rm{length}}/\rm{kpc} <7.8$ (95%confidence). This measurement, of unprecedented accuracy, represents the scaleover which the cool gas tends to cluster in separate structures. We argue that,if $C_{\rm{length}}$ is a universal property of the CGM, it needs to bereproduced by current and future theoretical models in order to understand theexact role of this medium in galaxy evolution.

Directly constraining the spatial coherence of the $z\sim1$ circumgalactic medium