Cosmological Simulations with Scale-Free Initial Conditions I: Adiabatic Hydrodynamics

Details Cosmological Simulations with Scale-Free Initial Conditions I: Adiabatic Hydrodynamics Cosmological Simulations with Scale-Free Initial Conditions I: Adiabatic Hydrodynamics

1997-05-14

arxiv.org/abs/astro-ph/9705109v2

Astrophys.J. 503 (1998) 16

Astronomy and Astrophysics

Astrophysics

40 pages, 16 embedded postscript figures, uses AASTEX 4.0 style. Minor wording changes, to appear in ApJ. Abridged abstract

Scientific paper

10.1086/305957

We analyze hierarchical structure formation based on scale-free initial conditions in an Einstein-de Sitter universe, including a baryonic component. We present three independent, smoothed particle hydrodynamics (SPH) simulations, performed with two different SPH codes (TreeSPH and P3MSPH) at two resolutions. Each simulation is based upon identical initial conditions, which consist of Gaussian distributed initial density fluctuations that have an n=-1 power spectrum. The baryonic material is modeled as an ideal gas subject only to shock heating and adiabatic heating and cooling. The evolution is expected to be self-similar in time, and under certain restrictions we identify the expected scalings for many properties of the distribution of collapsed objects in all three realizations. The distributions of dark matter masses, baryon masses, and mass and emission weighted temperatures scale quite reliably. However, the density estimates in the central regions of these structures are determined by the degree of numerical resolution. As a result, mean gas densities and luminosities obey the expected scalings only when calculated within a limited dynamic range in density contrast. The temperatures and luminosities of the groups show tight correlations with the baryon masses, which can be well-represented by power-laws. The Press-Schechter (PS) approximation predicts the distribution of group dark matter and baryon masses fairly well, though it tends to overestimate the baryon masses. Combining the PS mass distribution with the measured relations for T(M) and L(M) predicts the temperature and luminosity distributions reasonably, though there are some discrepancies at high temperatures/luminosities. The three simulations agree well for the properties of groups that are resolved by 32 or more particles.

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