Statistics – Computation
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994phdt........10f&link_type=abstract
PhD Dissertation, Texas Univ. Austin, TX United States
Statistics
Computation
2
Dwarf Galaxies, Maxwell-Boltzmann Density Function, Dark Matter, Galactic Clusters, Galactic Evolution, Baryons, Boundary Conditions, Cosmology, Extraterrestrial Matter, Many Body Problem, Simulation, Stellar Mass, Velocity Distribution
Scientific paper
Formation and evolution of Dwarf Galaxies and their clustering is studied in a cold dark matter dominated universe, using cosmological N-body simulations. Our model assumes a spatially flat universe with a baryon density parameter omegab = 0.09 and dark matter density parameter omegadark = 0.91. We produce the initial conditions of the cold dark matter spectrum at relatively small scales, so that the size of our computational box is 5.253 Mpc3 in present units. We assume periodic boundary conditions, using a P3M code to carry out the simulations. We model a two component system consisting of collisional gas and collisionless dark matter. The experiments have been conducted on a 643 grid with 323 gas and 3 x 323 dark matter particles. The gas is isothermal with maxwellian distribution of particle velocities. 25 gas particles correspond to have a mass of 109 m(solar mass). We present the results of five experiments. The last experiment is conducted with initial power spectrum of P(k) = Ak-1 and gives a remarkable agreement with the observed correlation function, although no discrete objects like galaxies are seen to have formed till the end of the experiment in this case. With CDM power spectrum, discrete objects having masses corresponding to those of dwarf galaxies are formed throughout the computational box giving a galaxy-galaxy correlation function xigg(r) directly proportional to r-1.2 for galaxies containing 29 particles or more. The galaxy-galaxy correlation function is strongly dependent upon the masses of the galaxies, more massive galaxies being more strongly clustered. The main conclusion is that this relatively conservative gas model provides physical justification for the formation of dwarf galaxy sized objects in the absence of large scale power in a CDM model.
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