We analyze a new large-scale (100 h-1 Mpc) numerical hydrodynamic simulation of the popular ΛCDM cosmological model, including in our treatment dark matter, gas, and star formation, on the basis of standard physical processes. The method, applied with a numerical resolution of 200 h-1 kpc (which is still quite coarse for following individual galaxies, especially in dense regions), attempts to estimate where and when galaxies form. We then compare the smoothed galaxy distribution with the smoothed mass distribution to determine the "bias," defined as b ≡ (δM/M)gal/(δM/M)total, on scales that are large compared to the code numerical resolution (on the basis of resolution tests given in the Appendix of this paper). We find that (holding all variables constant except the quoted one) bias increases with decreasing scale, with increasing galactic age or metallicity, and with increasing redshift of observations. At the 8 h-1 Mpc fiducial comoving scale, bias (for bright regions) is 1.35 at z = 0, reaching to 3.6 at z = 3, both numbers being consistent with extant observations. We also find that (10-20) h-1 Mpc voids in the distribution of luminous objects are as observed (i.e., observed voids are not an argument against cold dark matter [CDM]-like models), and finally that the younger systems should show a colder Hubble flow than do the early-type galaxies (a testable proposition). Surprisingly, little evolution is found in the amplitude of the smoothed galaxy-galaxy correlation function (as a function of comoving separation). Testing this prediction against observations will allow a comparison between this work and that of Kauffmann et al., which is based on a different physical modeling method.
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