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The connection between galaxies and dark matter halos is often quantifiedusing the stellar mass-halo mass (SMHM) relation. Optical and near-infraredimaging surveys have led to a broadly consistent picture of the evolving SMHMrelation based on measurements of galaxy abundances and angular correlationfunctions. Spectroscopic surveys at $z \gtrsim 2$ can also constrain the SMHMrelation via the galaxy autocorrelation function and through thecross-correlation between galaxies and Ly$\alpha$ absorption measured intransverse sightlines; however, such studies are very few and have producedsome unexpected or inconclusive results. We use $\sim$3000 spectra of$z\sim2.5$ galaxies from the Lyman-alpha Tomography IMACS Survey (LATIS) tomeasure the galaxy-galaxy and galaxy-Ly$\alpha$ correlation functions in fourbins of stellar mass spanning $10^{9.2} \lesssim M_* / M_{\odot} \lesssim10^{10.5}$. Parallel analyses of the MultiDark N-body and ASTRID hydrodynamiccosmological simulations allow us to model the correlation functions, estimatecovariance matrices, and infer halo masses. We find that results of the twomethods are mutually consistent and are broadly in accord with standard SMHMrelations. This consistency demonstrates that we are able to accurately measureand model Ly$\alpha$ transmission fluctuations $\delta_F$ in LATIS. We alsoshow that the galaxy-Ly$\alpha$ cross-correlation, a free byproduct of opticalspectroscopic galaxy surveys at these redshifts, can constrain halo masses withsimilar precision to galaxy-galaxy clustering.

LATIS: Constraints on the Galaxy-halo Connection at $z \sim 2.5$ from Galaxy-galaxy and Galaxy-Ly$\alpha$ Clustering