DO GALACTIC SYSTEMS FORM TOO LATE IN COLD PLUS HOT DARK-MATTER MODELS

The abundance of galactic systems at high redshifts can impose a strong constraint on the cold + dark matter (CDM + HDM) models. The hot component reduces the excessive small-scale power in the COBE-normalized CDM model but also delays the epoch of galaxy formation. We present results from the first numerical simulations that have enough dynamic range to address accurately the issue of high-redshift halo abundances in CDM + HDM models. Equivalent high-resolution particle-particle/particle-mesh N-body simulations are performed for spatially flat models with Omega(v) = 0.3 and 0.2 (with H-O = 50 km s(-1) Mpc(-1) and Omega(b) = 0.05). We study the constraints placed on the models by the high-redshift quasar space density and by the mass fraction in neutral dense gas associated with damped Ly alpha systems. We find that even with optimistic assumptions, the much-studied Omega(v) = 0.3 model does not produce enough massive halos to account for the observed abundance of quasars at z > 4. The model passes this test if Omega(v) is decreased to 0.2. Both models do not produce enough high column density halos to account for the amount of gas in damped Ly alpha systems at z greater than or similar to 3: the Omega(v) = 0.3 model falls short by a factor of similar to 80; the Omega(v) = 0.2 model by a factor similar to 3. We conclude that only CDM + HDM models with Omega(v) less than or similar to 0.2 can match observations at high redshift, implying an upper bound of 4.7 eV on the most massive light neutrino (presumably the tau).