hmfast.halos.massfunc.T10HaloMassFunction
- class hmfast.halos.massfunc.T10HaloMassFunction[source]
Bases:
HaloMassFunctionHalo mass function from Tinker et al. (2010).
Calibrated for 200m mass definition.
Methods
dndlnm(cosmology, m, z[, mass_definition, ...])Compute the halo mass function \(dn/d\ln M\).
- dndlnm(cosmology, m, z, mass_definition=<hmfast.halos.massdef.MassDefinition object>, convert_masses=False)[source]
Compute the halo mass function \(dn/d\ln M\).
The halo mass function gives the comoving number density of halos per logarithmic mass interval:
\[\frac{dn}{d\ln M} = f(\sigma) \frac{\rho_{m,0}}{M} \left| \frac{d\ln \sigma^{-1}}{d\ln M} \right|\]\[f(\nu) = 0.5 \alpha \left[1 + (\beta^2 \nu)^{-\phi}\right] \nu^{\eta} \exp\left(-\frac{\gamma \nu}{2}\right) \sqrt{\nu},\]where \(\nu = \delta_c^2 / \sigma^2(M)\) with \(\delta_c = 1.686\), \(f(\nu)\) is the fitting function, \(\alpha\), \(\beta\), \(\gamma\), \(\eta\), and \(\phi\) are redshift-dependent fitting parameters, \(\rho_{m,0}\) is the present-day mean matter density, \(M\) is the halo mass, and \(\sigma(M)\) is the variance of the density field smoothed on mass scale \(M\).
- Parameters:
- cosmologyCosmology
Cosmology used to evaluate the halo mass function.
- marray-like
Halo mass grid in physical \(M_\odot\).
- zarray-like
Redshift grid.
- mass_definitionMassDefinition, optional
Halo mass definition at which to evaluate the halo mass function. Defaults to the native \(200\mathrm{m}\) calibration definition.
- convert_massesbool, optional
Mass conversions are applied if
convert_massesis set toTrue.
- Returns:
- dndlnMfloat or array-like
Halo mass function values \(dn/d\ln M\) in comoving \(\mathrm{Mpc}^{-3}\), with shape \((N_m, N_z)\), where singleton dimensions get squeezed before return.