Dependence of the non-linear mass power spectrum on the equation of state of dark energy

作者：McDonald P^*; Trac H; Contaldi C

来源：Monthly Notices of the Royal Astronomical Society, 2006, 366(2): 547-556.

DOI：10.1111/j.1365-2966.2005.09881.x

• equation of state
• methods : N-body simulations
• cosmological parameters
• cosmology : theory
• dark matter
• large-scale structure of Universe

We present N-body simulation calculations of the dependence of the power spectrum of non-linear cosmological mass density fluctuations on the equation of state of the dark energy, w=p/rho. At fixed linear theory power, increasing w leads to an increase in non-linear power, with the effect increasing with k. By k= 10 h Mpc(-1), a model with w=-0.75 has similar to 12 per cent more power than a standard cosmological constant model (w=-1), while a model with w=-0.5 has similar to 33 per cent extra power (at z= 0). The size of the effect increases with increasing dark energy fraction, and to a lesser extent increasing power spectrum normalization, but is insensitive to the power spectrum shape (the numbers above are for Omega(m)= 0.281 and sigma(8)= 0.897). A code quantifying the non-linear effect of varying w, as a function of k, z and other cosmological parameters, which should be accurate to a few per cent for k less than or similar to 10 h Mpc(-1) for models that fit the current observations, is available at http://www.cita.utoronto.ca/similar to pmcdonal/code.html. This paper also serves as an example of a detailed exploration of the numerical convergence properties of ratios of power spectra for different models, which can be useful because some kinds of numerical error cancel in a ratio. When precision calculations based on numerical simulations are needed for many different models, efficiency may be gained by breaking the problem into a calculation of the absolute prediction at a central point, and calculations of the relative change in the prediction with model parameters.

• 出版日期2006-2-21