halomod.bias.Seljak04Cosmo¶
- class halomod.bias.Seljak04Cosmo(nu: numpy.ndarray, delta_c: float = 1.686, m: Optional[numpy.ndarray] = None, mstar: Optional[float] = None, delta_halo: Optional[float] = 200, n: Optional[float] = 1, sigma_8: Optional[float] = 0.8, cosmo: astropy.cosmology.core.FLRW = FlatLambdaCDM(name="Planck15", H0=67.7 km / (Mpc s), Om0=0.307, Tcmb0=2.725 K, Neff=3.05, m_nu=[0. 0. 0.06] eV, Ob0=0.0486), n_eff: Optional[numpy.ndarray] = None, z: float = 0.0, **model_parameters)[source]¶
Empirical bias relation from Seljak & Warren (2004), with cosmological dependence.
See documentation for
Bias
for information on input parameters. This model has no free parameters.Notes
This the form from [1] with cosmological dependence – except we do not include the running of the spectral index. The form is
\[b_{\rm no cosmo} + \log_10(x) \left[a_1 (\Omega_{m,0} - 0.3 + n - 1) + a_2(\sigma_8 - 0.9 + h-0.7)\right]\]with \(x = m/m_\star\) (and \(m_{\star}\) the nonlinear mass – see
Bias
for details). The non-cosmologically-dependent bias is that given bySeljak04
.a1
anda2
are fitted, with values given in [1] as(a1,a2) = (0.4, 0.3)
.- Parameters
a (float, optional) – The fitted parameters for
Seljak04
.b (float, optional) – The fitted parameters for
Seljak04
.c (float, optional) – The fitted parameters for
Seljak04
.d (float, optional) – The fitted parameters for
Seljak04
.e (float, optional) – The fitted parameters for
Seljak04
.f (float, optional) – The fitted parameters for
Seljak04
.g (float, optional) – The fitted parameters for
Seljak04
.a1 (float, optional) – Fitted parameters for the cosmological dependence.
a2 (float, optional) – Fitted parameters for the cosmological dependence.
References
- 1(1,2)
Seljak, U. and Warren M. S., “Large-scale bias and stochasticity of haloes and dark matter”, https://ui.adsabs.harvard.edu/abs/2004MNRAS.355..129S, 2004.
Methods
__init__
(nu[, delta_c, m, mstar, …])Initialize self.
bias
()Calculate the first-order, linear, deterministic halo bias.
Get a dictionary of all implemented models for this component.
Attributes
The HMF model that pairs with this bias in the peak-background split