NumCosmoClusterAbundance

Atomically decrements the reference count of cad by one. If the reference count drops to 0, all memory allocated by cad is released.

This function computes $ \int_{\ln M^{obs} - 7\sigma_{\ln M}}^{\ln M^{obs} + 7\sigma_{\ln M}} d\ln M \, \frac{d^2N}{dzdlnM} * P(\ln M^{obs}|\ln M) $. The integral limits were determined requiring a precision to five decimal places.

Atomically decrements the reference count of cad by one. If the reference count drops to 0, all memory allocated by cad is released.

Computes the integrated differential abundance over the specified observed mass and redshift bins.

Computes the bias-weighted integrated differential abundance over the specified bins.

Computes the interpolated differential abundance $d^2N/dzd\ln M$ at the given mass and redshift.

Computes the bias-weighted differential abundance for the given observed mass and redshift.

This function computes $ \int_{\ln M^{obs} - 7\sigma_{\ln M}}^{\ln M^{obs} + 7\sigma_{\ln M}} d\ln M \, \frac{d^2N}{dzdlnM} * P(\ln M^{obs}|\ln M) $. The integral limits were determined requiring a precision to five decimal places.

This function computes the total number of clusters within specific redshift and mass intervals, which are defined in clusterz and clusterm, respectively, and over a sky area.

This function prepares …

Prepares the cluster abundance object if the cosmology or cluster models have changed. This function checks if any of the models have been updated and calls nc_cluster_abundance_prepare() if necessary.

This function prepares a spline where the x array corresponds to the value of $\int_{\ln M_0} ^{\ln M_1} d^2N/dzd\ln M dM/ \int_lnMi^lnMf dN/dz dM$ given a redshift $z$ and the y array contains the values of logarithms base e of the mass. It is used to generate a sample of $\ln M$ values.

This function prepares a bidimensional spline…

Increases the reference count of cad by one.

Sets the sky area for the cluster abundance calculation.

This function computes the total number of “true” clusters, i.e., halos within redshift and mass intervals, and over a sky area.

This function computes $ \int_{z_{phot} - 10\sigma_{phot}}^{z_{phot} + 10\sigma_{phot}} dz \, \frac{d^2N}{dzdlnM} * P(z^{photo}|z) $. The integral limits were determined requiring a precision to five decimal places.

This function computes $ \int_0^\infty dz \int_{-\infty}^\infty d\ln M \frac{d^2N(\ln M, z)}{dzd\ln M} * P(z^{phot}|z) * P(\ln M^{obs}|\ln M, z) $. We studied the convergence of this integral to optimize this function. We verified that it converges to 5 decimal places at the redshift interval $ [z^{phot} - 10\sigma^{phot}, z^{phot} + 10\sigma^{phot}] $ and the mass interval $ [\ln M^{obs} - 7\sigma_{\ln M}, \ln M^{obs} + 7\sigma_{\ln M}] $.