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We examine the statistics of the low-redshift Ly-alpha forest in an adaptivemesh refinement hydrodynamic cosmological simulation of sufficient volume toinclude distinct large-scale environments. We compare our HI column densitydistribution of absorbers both with recent work and between two highly-refinedregions of our simulation: a large-scale overdensity and a large-scaleunderdensity (on scales of approximately 20 Mpc). We recover the averageresults presented in Kollmeier et al. (2014) using different simulationmethods. We further break down these results as a function of environment toexamine the detailed dependence of absorber statistics on large-scale density.We find that the slope of the HI column density distribution in the 10$^{12.5}$$\le$ N$_{HI}$/cm$^{-2}$ $\le$ 10$^{14.5}$ range depends on environment suchthat the slope becomes steeper for higher environmental density, and thisdifference reflects distinct physical conditions of the intergalactic medium onthese scales. We track this difference to the different temperature structuresof filaments in varying environments. Specifically, filaments in theoverdensity are hotter and, correspondingly, are composed of gas with lower HIfractions than those in underdense environments. Our results highlight that inorder to understand the physics driving the HI CDD, we need not only improvedaccounting of the sources of ionizing UV photons, but also of the physicalconditions of the IGM and how this may vary as a function of large-scaleenvironment.

Probing the Dependence of the Intergalactic Medium on Large Scale Environment Using the Low Redshift Lyman Alpha Forest