pyccl.massfunction module

pyccl.massfunction.halo_bias(cosmo, halo_mass, a, overdensity=200)[source]

Tinker et al. (2010) halo bias

Parameters:
  • cosmo (Cosmology) – Cosmological parameters.
  • halo_mass (float or array_like) – Halo masses; Msun.
  • a (float) – Scale factor.
  • overdensity (float) – Overdensity parameter (default: 200).
Returns:

Halo bias.

Return type:

float or array_like

pyccl.massfunction.massfunc(cosmo, halo_mass, a, overdensity=200)[source]

Tinker et al. (2010) halo mass function, dn/dlog10M.

Parameters:
  • cosmo (Cosmology) – Cosmological parameters.
  • halo_mass (float or array_like) – Halo masses; Msun.
  • a (float) – scale factor.
  • overdensity (float) – overdensity parameter (default: 200)
Returns:

Halo mass function; dn/dlog10M.

Return type:

float or array_like

pyccl.massfunction.massfunc_m2r(cosmo, halo_mass)[source]

Converts smoothing halo mass into smoothing halo radius.

Note

This is R=(3M/(4*pi*rho_m))^(1/3), where rho_m is the mean matter density.

Parameters:
  • cosmo (Cosmology) – Cosmological parameters.
  • halo_mass (float or array_like) – Halo masses; Msun.
Returns:

Smoothing halo radius; Mpc.

Return type:

float or array_like

pyccl.massfunction.sigmaM(cosmo, halo_mass, a)[source]

Root mean squared variance for the given halo mass of the linear power spectrum; Msun.

Parameters:
  • cosmo (Cosmology) – Cosmological parameters.
  • halo_mass (float or array_like) – Halo masses; Msun.
  • a (float) – scale factor.
Returns:

RMS variance of halo mass.

Return type:

float or array_like