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The dataset consists of the matter power spectra at four redshifts (z=80,50,15,0) generated by simulating Lambda-Cold Dark Matter cosmology within the cosmic screening approach as described in the associated paper. Outputs of six distinct runs are available for boxes with L= 280, 560, 1680, 4480, 5120, 5632 Mpc/h comoving sizes, each with 2 Mpc/h resolution.

One of the main objectives of modern cosmology is to explain the origin and evolution of cosmic structures at different scales. The principal force responsible for the formation of such structures is gravity. In a general relativistic framework, we have shown that matter density contrasts do not grow over time at scales exceeding the cosmic screening length, which corresponds to a cosmological scale of the order of two to three gigaparsecs at the present time, at which gravitational interactions exhibit an exponential cut-off. This is a purely relativistic effect. To demonstrate the suppression of density growth, we have performed N-body simulations in a box with a comoving size of 5.632 Gpc/h and obtained the power spectrum of the mass density contrast. We have shown that it becomes independent of time for scales beyond the cosmic screening length as a clear manifestation of the cosmic screening effect.

Gravitational clustering of cold dark matter, as predicted by concordance cosmology, is often studied via N-body simulations based on Newtonian dynamics. Though efficient in tracking nonlinear growth of fluctuations at small scales, outcomes of such simulations cannot be linked to observables immediately, and a certain effort is required to obtain relativistic interpretations of variables by employing convenient gauges and dictionaries. Based on a weak-field expansion of general relativity, a fully-relativistic N-body code has been introduced in the past decade (Adamek, J., Daverio, D., Durrer, R., Kunz, M., JCAP 07, 053 (2016)), capable of evolving all metric variables in the Poisson gauge which is the conventional choice in formulating cosmological perturbations. However, spatial and temporal derivates are assigned different orders of smallness and field equations, containing admixtures of higher-order terms, acquire a rather complex form. In this talk we will explore an alternative formulation of perturbations, still based on a weak-field expansion, and expressed in the Poisson gauge, which however treats all derivates on equal footing and hence a clear distinction exists between first and second order contributions in the expansion (Eingorn, M., ApJ 825, 84 (2016), Canay, E., Eingorn, M., PDU 29, 100565 (2020), arXiv:2206.13495 [gr-qc]). We will show that it is possible to obtain analytical solutions for the scalar and vector potentials in this scheme and that they hint at some exciting characteristics of gravitational interactions at large-enough cosmological scales.

Gravitational clustering of cold dark matter, as predicted by concordance cosmology, is often studied via N-body simulations based on Newtonian dynamics. Though efficient in tracking nonlinear growth of fluctuations at small scales, outcomes of such simulations cannot be linked to observables immediately, and a certain effort is required to obtain relativistic interpretations of variables by employing convenient gauges and dictionaries. Based on a weak-field expansion of general relativity, a fully-relativistic N-body code has been introduced in the past decade (Adamek, J., Daverio, D., Durrer, R., Kunz, M., JCAP 07, 053 (2016)), capable of evolving all metric variables in the Poisson gauge which is the conventional choice in formulating cosmological perturbations. However, spatial and temporal derivates are assigned different orders of smallness and field equations, containing admixtures of higher-order terms, acquire a rather complex form. In this talk we will explore an alternative formulation of perturbations, still based on a weak-field expansion, and expressed in the Poisson gauge, which however treats all derivates on equal footing and hence a clear distinction exists between first and second order contributions in the expansion (Eingorn, M., ApJ 825, 84 (2016), Canay, E., Eingorn, M., PDU 29, 100565 (2020), arXiv:2206.13495 [gr-qc]). We will show that it is possible to obtain analytical solutions for the scalar and vector potentials in this scheme and that they hint at some exciting characteristics of gravitational interactions at large-enough cosmological scales.

The dataset consists of matter power spectra at four redshifts (z=80,50,15,0) generated by simulating Lambda-Cold Dark Matter cosmology with respect to two distinct weak-field expansion schemes (one relevant to the energy density and the other relevant to the mass density of matter) as described in the associated paper. Additionally, it contains the power spectrum of the gravitational potential at the same redshift values, based on the expansion scheme of the screening approach only.

The dataset consists of matter power spectra at four redshifts (z=80,50,15,0) generated by simulating Lambda-Cold Dark Matter cosmology within the cosmic screening approach as described in the associated paper.