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  1. N-body simulations for CDM cosmology starting from back-scaled initial conditions can be self-consistently embedded in a relativistic space-time with rst-order metric potentials cal-culated using a linear Boltzmann code. This space-time coincides with a simple \N-body gauge" for z<50 for all observable modes.
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  3. Initial conditions for (Newtonian) cosmological N-body simulations are usually set by re-scaling the present-day power spectrum obtained from linear (relativistic) Boltzmann codes to the desired initial redshift of the simulation. This back-scaling method can account for the effect of inhomogeneous residual thermal radiation at early times, which is absent in the Newtonian simulations. We ...
    Author:Christian Fidler, Thomas Tram, Thomas Tram, Cornelius Rampf, Cornelius Rampf, Robert Crittenden, Kaz...Published:2017
  4. We find that N-body simulations for ΛCDM cosmology starting from back-scaled initial conditions can be self-consistently embedded in a relativistic space-time with first-order metric potentials calculated using a linear Boltzmann code. This space-time coincides with a simple ''N-body gauge'' for z < 50 for all observable modes.
  5. researchportal.port.ac.uk

    We find that N-body simulations for ΛCDM cosmology starting from back-scaled initial conditions can be self-consistently embedded in a relativistic space-time with first-order metric potentials calculated using a linear Boltzmann code. This space-time coincides with a simple "N-body gauge" for z < 50 for all observable modes.
  6. inspirehep.net

    We find that N-body simulations for ΛCDM cosmology starting from back-scaled initial conditions can be self-consistently embedded in a relativistic space-time with first-order metric potentials calculated using a linear Boltzmann code. This space-time coincides with a simple ``N-body gauge'' for z < 50 for all observable modes.
  7. iopscience.iop.org

    We find that N-body simulations for ΛCDM cosmology starting from back-scaled initial conditions can be self-consistently embedded in a relativistic space-time with first-order metric potentials calculated using a linear Boltzmann code. This space-time coincides with a simple ``N-body gauge'' for z < 50 for all observable modes. Care must be ...
  8. semanticscholar.org

    Initial conditions for (Newtonian) cosmological N-body simulations are usually set by re-scaling the present-day power spectrum obtained from linear (relativistic) Boltzmann codes to the desired initial redshift of the simulation. This back-scaling method can account for the effect of inhomogeneous residual thermal radiation at early times, which is absent in the Newtonian simulations.
  9. link.aps.org

    The initial conditions for Newtonian N-body simulations are usually generated by applying the Zel'dovich approximation to the initial displacements of the particles using an initial power spectrum of density fluctuations generated by an Einstein-Boltzmann solver.We show that in most gauges the initial displacements generated in this way receive a first-order relativistic correction.
  10. researchgate.net

    Initial conditions for (Newtonian) cosmological N-body simulations are usually set by re-scaling the present-day power spectrum obtained from linear (relativistic) Boltzmann codes to the desired ...
  11. link.aps.org

    Some recent work has focused on the effects of incorporating relativistic corrections into N-body simulations [6- 9], or interpreting Newtonian simulations in terms of General Relativity [10, 11]. Since gravity is nonlinear, the simulations are extremely sensitive to the initial conditions used. So far, the initial conditions have been ...

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