Clustering of galaxy clusters in cold dark matter universes
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Discussion
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Implication
Cosmological simulation analysis demonstrates mass-dependent clustering of galaxy clusters in cold dark matter models, indicating strong agreement with analytic predictions across cosmic scales.
Key Points
- Predict the two-point correlation functions and power spectra of mass-limited galaxy cluster samples in critical-density and low-density cold dark matter cosmologies.
- Simulated mass distributions using cosmological N-body simulations with 10^9 particles in cubic volumes of side 2 h^-1 Gpc (tCDM) and 3 h^-1 Gpc (LCDM) at a force resolution exceeding 10^-4 of the cube side.
- Measured correlation lengths and power spectra across varying cluster mass limits and abundances, comparing results to the Sheth, Mo & Tormen model and observational APM cluster data.
- Correlation length increased with mean cluster separation, shifting from r_0 = 12–13 h^-1 Mpc at d_c = 30 h^-1 Mpc to r_0 = 22–27 h^-1 Mpc at d_c = 100 h^-1 Mpc, with lower bounds in tCDM and higher bounds in LCDM.
- The Sheth, Mo & Tormen model predicted correlation lengths and power spectrum biases to within 10% accuracy without adjustable parameters.
- Observed APM richness-dependent correlation lengths matched the LCDM model closely, though observed cluster power spectrum amplitudes at d_c ≈ 31 h^-1 Mpc exceeded predictions for both models.
Cite This Study
Colberg et al. (2002) studied this question.