High-Redshift Clumpy Disks & Bulges in Cosmological Simulations

We analyze the first cosmological simulations that recover the fragmentation of high-redshift galactic discs driven by cold streams. The fragmentation is recovered owing to an AMR resolution better than 70 pc with cooling below 10K. We study three typical star-forming galaxies in haloes of ∼ 5 × 10M⊙ at z ≃ 2.3, when they were not undergoing a major merger. The steady gas supply by cold streams leads to gravitationally unstable, turbulent discs, which fragment into giant clumps and transient features on a dynamical timescale. The disc clumps are not associated with dark-matter haloes. The clumpy discs are self-regulated by gravity in a marginaly unstable state. Clump migration and angular-momentum transfer on an orbital timescale help the growth of a central bulge with a mass comparable to the disc. The continuous gas input keeps the system of clumpy disc and bulge in a near steady state for several Gyr. The average star-formation rate, much of which occurs in the clumps, follows the gas accretion rate of ∼ 45M⊙ yr. The simulated galaxies resemble in many ways the observed star-forming galaxies at high redshift. Their properties are consistent with the simple theoretical framework presented in Dekel, Sari & Ceverino (2009, DSC). In particular, a two-component analysis reveals that the simulated discs are indeed marginally unstable, and the time evolution confirms the robustness of the clumpy configuration in a cosmological steady state. By z ∼ 1, the simulated systems are stabilized by a dominant stellar spheroid, demonstrating the process of “morphological quenching” of star formation (Martig et al. 2009). We demonstrate that the disc fragmentation is not a numerical artifact once the Jeans length is kept larger than ∼ 7 resolution elements, i.e. beyond the standard Truelove criterion.