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We study some effects the inclusion of the radiation energy component in theuniverse, Omega_r, can have on several quantities of interest for thelarge-scale structure of the universe in a LCDM cosmological simulation;started at a very high redshift (z=500). In particular we compute the powerspectrum density, the halo mass function, and the concentration-mass relationfor haloes. We find that Omega_r has an important contribution in the long-termnonlinear evolution of structures in the universe. For instance, a lower matterdensity power, by approx 50%, in all scales is obtained when compared with asimulation without the radiation term. Also, haloes formed with the Omega_rtaken into account are approx 20% less concentrated than when not included inthe Hubble function.

The radiation energy component of the Hubble function and a LCDM cosmological simulation