The cosmological parameters used for the EAGLE simulations: Ωm, |$\Omega _\Lambda$|, and Ωb are the average densities of matter, dark energy, and baryonic matter in units of the critical density at redshift zero; H0 is the Hubble parameter, σ8 is the square root of the linear variance of the matter distribution when smoothed with a top-hat filter of radius 8h−1 cMpc, ns is the scalar power-law index of the power spectrum of primordial adiabatic perturbations, and Y is the primordial abundance of helium.
| Cosmological parameter . | Value . |
|---|---|
| Ωm | 0.307 |
| |$\Omega _\Lambda$| | 0.693 |
| Ωb | 0.048 25 |
| h ≡ H0/(100 km s−1 Mpc−1) | 0.6777 |
| σ8 | 0.8288 |
| ns | 0.9611 |
| Y | 0.248 |
| Cosmological parameter . | Value . |
|---|---|
| Ωm | 0.307 |
| |$\Omega _\Lambda$| | 0.693 |
| Ωb | 0.048 25 |
| h ≡ H0/(100 km s−1 Mpc−1) | 0.6777 |
| σ8 | 0.8288 |
| ns | 0.9611 |
| Y | 0.248 |
The cosmological parameters used for the EAGLE simulations: Ωm, |$\Omega _\Lambda$|, and Ωb are the average densities of matter, dark energy, and baryonic matter in units of the critical density at redshift zero; H0 is the Hubble parameter, σ8 is the square root of the linear variance of the matter distribution when smoothed with a top-hat filter of radius 8h−1 cMpc, ns is the scalar power-law index of the power spectrum of primordial adiabatic perturbations, and Y is the primordial abundance of helium.
| Cosmological parameter . | Value . |
|---|---|
| Ωm | 0.307 |
| |$\Omega _\Lambda$| | 0.693 |
| Ωb | 0.048 25 |
| h ≡ H0/(100 km s−1 Mpc−1) | 0.6777 |
| σ8 | 0.8288 |
| ns | 0.9611 |
| Y | 0.248 |
| Cosmological parameter . | Value . |
|---|---|
| Ωm | 0.307 |
| |$\Omega _\Lambda$| | 0.693 |
| Ωb | 0.048 25 |
| h ≡ H0/(100 km s−1 Mpc−1) | 0.6777 |
| σ8 | 0.8288 |
| ns | 0.9611 |
| Y | 0.248 |
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