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NcCorClusterCmbLensLimberNcCorClusterCmbLensLimber — Cluster and CMB lensing correlation using halo model and Limber approximation. |
NcCorClusterCmbLensLimber *
nc_cor_cluster_cmb_lens_limber_new (void);
This function allocates memory for a new NcCorClusterCmbLensLimber object.
gdouble nc_cor_cluster_cmb_lens_limber_oneh_int_mass (NcCorClusterCmbLensLimber *cccll,NcClusterAbundance *cad,NcClusterMass *clusterm,NcHICosmo *cosmo,NcHaloDensityProfile *dp,gdouble k,gdouble z,gdouble *lnM_obs,gdouble *lnM_obs_params);
This function computes the 1-halo integral on mass of the cluster and CMB lensing potential $\psi$, using Limber approximation.
gdouble nc_cor_cluster_cmb_lens_limber_oneh_term (NcCorClusterCmbLensLimber *cccll,NcClusterAbundance *cad,NcHICosmo *cosmo,NcDistance *dist,NcHaloDensityProfile *dp,gint l,gdouble *lnM_obs,gdouble *lnM_obs_params,gdouble *z_obs,gdouble *z_obs_params);
This function computes the 1-halo term of the cluster and CMB lensing potential $\psi$, using Limber approximation: \begin{equation} \left(C_l^{cl \psi} \right)_{1h} = -3 \frac{\Omega_{m0} H_0^2}{l^2} \int dz \frac{c}{H(z)} (1+z) \chi(z)^2 \frac{\left( \chi(z_\ast) - \chi(z) \right)}{\chi(z_\ast) \chi(z)} \int d\ln M S(\ln M, z) \frac{M}{\overline{\rho}(z)} \frac{dn(M, z)}{d\ln M} \tilde{u}^\ast (k = l/\chi(z) \vert M), \end{equation} where ...
gdouble nc_cor_cluster_cmb_lens_limber_twoh_int_mass1 (NcCorClusterCmbLensLimber *cccll,NcClusterAbundance *cad,NcClusterMass *clusterm,NcHICosmo *cosmo,gdouble z);
This function computes the first integral on mass of the 2-halo term of the cluster and CMB lensing potential $\psi$, using Limber approximation.
gdouble nc_cor_cluster_cmb_lens_limber_twoh_int_mm (NcCorClusterCmbLensLimber *cccll,NcClusterAbundance *cad,NcHICosmo *cosmo,NcHaloDensityProfile *dp,gdouble k,gdouble z);
This function computes the 2-halo term of the matter-matter power spectrum.
gdouble nc_cor_cluster_cmb_lens_limber_twoh_int_mass2 (NcCorClusterCmbLensLimber *cccll,NcClusterAbundance *cad,NcClusterMass *clusterm,NcHICosmo *cosmo,NcHaloDensityProfile *dp,gdouble k,gdouble z);
This function computes the second integral on mass of the 2-halo term of the cluster and CMB lensing potential $\psi$, using Limber approximation.
gdouble nc_cor_cluster_cmb_lens_limber_twoh_term (NcCorClusterCmbLensLimber *cccll,NcClusterAbundance *cad,NcHICosmo *cosmo,NcDistance *dist,NcHaloDensityProfile *dp,gint l,gdouble *z_obs,gdouble *z_obs_params);
This function computes the 2-halo term of the cluster and CMB lensing potential $\psi$, using Limber approximation: \begin{equation} \left(C_l^{cl \psi} \right)_{1h} = -3 \frac{\Omega_{m0} H_0^2}{l^2 c^2} \int dz \frac{c}{H(z)} (1+z) \chi(z)^2 \frac{\left( \chi(z_\ast) - \chi(z) \right)}{\chi(z_\ast) \chi(z)} P_{lin}(k = l/\chi, z) \int d\ln M S(\ln M, z) \frac{dn(M, z)}{d\ln M} b(M, z) \int dln M^{\prime} \frac{M^\prime}{\overline{\rho}(z)} \frac{dn(M^\prime, z)}{d\ln M} b(M^\prime, z) \tilde{u}^\ast (k = l/\chi(z) \vert M^\prime), \end{equation} where ...