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The z > 2 Lyman-alpha (Lya) forest traces the underlying dark-matterdistribution on large scales and, given sufficient sightlines, can be used tocreate 3D maps of large-scale structure. We examine the observationalrequirements to construct such maps and estimate the signal-to-noise as afunction of exposure time and sightline density. Sightline densities at z =2.25 are n_los = [360, 1200,3300] deg^{-2} at limiting magnitudes of g =[24.0,24.5,25.0], resulting in transverse sightline separations of d_perp = [3.6,1.9, 1.2] h^{-1} Mpc, which roughly sets the reconstruction scale. We simulatethese reconstructions using mock spectra with realistic noise properties, andfind that spectra with S/N = 4 per angstrom can be used to generate maps thatclearly trace the underlying dark-matter at overdensities of rho/<rho> ~ 1. Forthe VLT/VIMOS spectrograph, exposure times t_exp = [4, 6, 10] hrs aresufficient for maps with spatial resolution epsilon_3d = [5.0, 3.2, 2.3] h^{-1}Mpc. Assuming ~ 250 h^{-1} Mpc is probed along the line-of-sight, 1 deg^2 ofsurvey area would cover a comoving volume of ~ 10^6 h^{-3} Mpc^3 at <z>=2.3,enabling efficient mapping of large volumes with 8-10m telescopes. These mapscould be used to study galaxy environments, detect proto-clusters, and studythe topology of large-scale structure at high-z.

Observational Requirements for Lyman-alpha Forest Tomographic Mapping of Large-Scale Structure at z ~ 2