MODERN COSMOLOGY
Methods 427 Table 15.1.Approximations of the power spectra. 0 bar hP 2 P 3 P 4 P 5 P 6 0.3 0.035 0.60 −1.7550E+00 6.0379E+01 ...
428 Numerical simulations in cosmology Figure 15.1. An example of the construction of mass refinement in real space (top) and in ...
Methods 429 then 1024^3 particles. We simply do not have enough computer memory to store the information for all the harmonics. ...
430 Numerical simulations in cosmology Figure 15.2. Another example of construction of mass refinement in phase space. For the h ...
Methods 431 Figure 15.3. Distribution of particles of different masses in a thin slice going through the centre of halo A 1 at r ...
432 Numerical simulations in cosmology (Couchman 1991). With modification the code is as fast as the TREE code even for heavily ...
Methods 433 different resolutions covering the regions of interest. The refinement is done cell-by-cell (individual cells can be ...
434 Numerical simulations in cosmology Figure 15.4.An example of a refinement structure constructed by the (hydro)ART code for s ...
Methods 435 Table 15.2.Parameters of the numerical simulations. Softening Steps Simulation (h−^1 kpc) Dyn. range (min–max) Nstep ...
436 Numerical simulations in cosmology Figure 15.6.Density profiles of four largest halos in simulations of Knebeet al(1999). No ...
Methods 437 resolutions, time steps and numerical techniques used for the simulations, the convergence is observed at a scale mu ...
438 Numerical simulations in cosmology actually was found very often in real halos when we compared the contents of halos at dif ...
Spatial and velocity biases 439 procedure is quite complicated. First, the density field is constructed. Second, the density (wi ...
440 Numerical simulations in cosmology DirectN-body simulations can be used for studies of the biases only if they have very hig ...
Spatial and velocity biases 441 There are some processes which we know create and affect the bias. At high redshifts there is st ...
442 Numerical simulations in cosmology (ii) Linear and nonlinear bias. If inξh(r)=b^2 ξdm(r)the biasbdoes not depend onξdm, it i ...
Spatial and velocity biases 443 Figure 15.7. Evolution of the correlation function of the dark matter and halos. The correlation ...
444 Numerical simulations in cosmology Figure 15.8. The correlation function and the power spectrum of halos with different limi ...
Spatial and velocity biases 445 Figure 15.9.Top panel: The evolution of bias at comoving scale of 0. 54 h−^1 Mpc for halos with ...
446 Numerical simulations in cosmology Figure 15.10. Overdensity of halosδhversus the overdensity of the dark matterδdm. The ove ...
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