Class
NumCosmoClusterPseudoCounts
Description [src]
class NumCosmo.ClusterPseudoCounts : NumCosmoMath.Model
{
/* No available fields */
}Model for the pseudo number counts of galaxy clusters.
Functions
nc_cluster_pseudo_counts_clear
The reference count of cpc is decreased and the pointer is set to NULL.
Instance methods
nc_cluster_pseudo_counts_free
Atomically decreases the reference count of cpc by one. If the reference count drops to 0,
all memory allocated by cpc is released.
nc_cluster_pseudo_counts_mf_lognormal_integral
Numerically evaluate the integral of the mass function multiplied by the log-normal observable distribution for given SZ and lensing observed masses. This is used in assembling expected counts or likelihoods where a log-normal approximation is sufficient.
nc_cluster_pseudo_counts_ndet
Compute the expected number of detections integrating over mass and the configured redshift interval. The function integrates the selection-weighted halo mass function over the fiducial mass and redshift limits.
nc_cluster_pseudo_counts_ndet_no_z_integral
Compute the mass-only integral of the selection-weighted halo mass function at a fixed redshift. This integrates over the true-mass range and returns the expected number density contribution for that redshift.
nc_cluster_pseudo_counts_posterior_ndetone
Compute the posterior term contribution for a single detection (i-th term) assuming flat priors for the selection function and halo mass function. The routine uses the PL-CL cluster mass model to evaluate the likelihood term for the observed masses at given redshift.
nc_cluster_pseudo_counts_posterior_numerator
Compute the numerator of the posterior integrand for a single object given fixed spectroscopic redshift. The function integrates the product of the selection function, the halo mass function and the observable likelihood over true mass to yield the posterior numerator contribution.
nc_cluster_pseudo_counts_posterior_numerator_plcl
($M_0 = 5.7 \times 10^{14} \, h^{-1} M_\odot$) for the purpose of non-dimensionalizing observed masses. Future work may expose the pivot as a model property.
nc_cluster_pseudo_counts_selection_function
Compute the selection function S(lnM, z), i.e. the probability that a halo of true log-mass lnM at redshift z is included in the sample given the modelled survey selection parameters. The selection is 0 outside the configured redshift window and follows a smooth transition around the mass cut inside the interval.
nc_cluster_pseudo_counts_selection_function_lnMi
This function computes the lower mass threshold used in the resample function, namely, $l\ln M_i = lnM_{cut} - 6\sigma_{cut}$.
Properties
NumCosmo.ClusterPseudoCounts:Deltaz
Maximum redsift is $z_{max} = z_{min} + \Delta z$. Range: $\Delta z \in [0.1, 2.0]$.
NumCosmo.ClusterPseudoCounts:lnMCut
Logarithm base e of the lower mass cut-off, $\ln M_{CUT} \in [12.0 \ln(10), 16.0 \ln(10)]$.
NumCosmo.ClusterPseudoCounts:lnMCut-fit
Flag indicating whether the lower mass cut (lnMCut) is to be treated as a free/fitted parameter. The detailed parameter bounds and default behavior are defined in the registration call above.
Properties inherited from NcmModel (9)
NumCosmoMath.Model:implementation
NumCosmoMath.Model:name
NumCosmoMath.Model:nick
NumCosmoMath.Model:params-types
NumCosmoMath.Model:reparam
NumCosmoMath.Model:scalar-params-len
NumCosmoMath.Model:sparam-array
NumCosmoMath.Model:submodel-array
NumCosmoMath.Model:vector-params-len
Signals
Signals inherited from GObject (1)
GObject::notify
The notify signal is emitted on an object when one of its properties has its value set through g_object_set_property(), g_object_set(), et al.