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The effect of non-linear evolution on the baryonic features

The effect of non-linear evolution on the oscillations in the power
spectrum. The solid line shows the ratio of the linear power spectrum for
a model with &Omega_{0} = 0.4, &Omega_{&Lambda} = 0.6,
H_{0} = 65 km s^{-1} Mpc^{-1},
&Omega_{b} h^{2} = 0.03 and n = 1.030 to a BBKS model.
The BBKS transfer function has &Gamma^{*} = 0.198, and the model
is *COBE* normalised. The dashed line shows the ratio including 2nd
order corrections. The small arrow near k = 0.2 h Mpc^{-1} indicates
where &Delta^{2}(k) = 1.
The open squares are the results from *N*-body simulations with the
Cold Dark Matter spectrum in real space, solid squares the results in
redshift space. Note that the oscillations for k > 0.1 h Mpc^{-1}
are washed out. (From Meiksin & White 1999, MNRAS, 304, 851.)

Return to baryonic P(k) features