Table of contents


Back to the main page 1. Compute Background Evolution 2. Compute Recombination History 3. Compute Perturbations 4. Compute Powerspectrum


Compute Background Evolution


Here you can select the cosmologically parameters and numerically compute the background evolution in $\Lambda$CDM and make some plots (dark energy density set from the stuff below as $\Omega_\Lambda = 1 - \sum_i \Omega_i$ and to use a pure cosmological constant as dark energy use $w_0 = -1$ and $w_a = 0$). We also show a comparison of the luminosity distance to supernova data (taken from Betoule et al. 2014). If you don't include neutrinos just put $N_{\rm eff} = 0.0$. The results using the fiducial parameters below can also be found here.

Background parameters

Hubble parameter ($H_0\equiv 100 h{\rm km/s/ Mpc}$):
$h$:
Baryon density:
$\Omega_b$:
CDM density:
$\Omega_{\rm CDM}$:
Curvature density ($\Omega_k \equiv -k/H_0^2$):
$\Omega_k$:
Temperature of the CMB today ($\Omega_\gamma \propto T_{\rm CMB}^4 / h^2$):
$T_{\rm CMB}$ (K):
Effective number of neutrinos ($\Omega_\nu \equiv N_{\rm eff}\frac{7}{8}\left(\frac{4}{11}\right)^{4/3}\Omega_\gamma$):
$N_{\rm eff}$:
Dark energy equation of state (CPL parametrisation) $w = w_0 + w_a(1-a)$:
$w_0$:
$w_a$:
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