NumCosmoWLSurfaceMassDensity

Atomically decrements the reference count of smd by one. If the reference count drops to 0, all memory allocated by smd is released. Set pointer to NULL.

Computes the reduced shear: $$ g(R) = \frac{\gamma(R)}{1 - \kappa(R)},$$ where $\gamma(R)$ is the shear [nc_wl_surface_mass_density_shear()] and $\kappa(R)$ is the convergence [nc_wl_surface_mass_density_convergence()], using the pre-computed critical surface density and surface mass density.

Variant of #nc_wl_surface_mass_density_reduced_shear_optzs_prep() that reuses a pre-computed lens-side context and pre-computed (r_s, rho_s). Only the per-R surface-mass-density profile evaluations are computed per call.

Computes and stores the surface mass density $\Sigma(R)$ and the mean surface mass density $\overline{\Sigma}(<R)$, see Eqs. $\eqref{eq:sigma}$ and $\eqref{eq:sigma_mean}$.

Computes the convergence $\kappa(R)$ at R, see Eq $\eqref{eq:convergence}$.

Computes the convergence $\kappa_\infty(R)$ at R, see Eq $\eqref{eq:convergence}$, and sources at infinite redshift.

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

Computes the reduced shear: $$ \mu(R) = \frac{1}{(1 - \kappa(R))^2 - \vert\gamma^2(R) \vert},$$ where $\gamma(R)$ is the shear [nc_wl_surface_mass_density_shear()] and $\kappa(R)$ is the convergence [nc_wl_surface_mass_density_convergence()].

Prepares the NcWLSurfaceMassDensity object smd for computation.

Prepares the NcWLSurfaceMassDensity object smd for computation if necessary.

Computes the reduced shear: $$ g(R) = \frac{\gamma(R)}{1 - \kappa(R)},$$ where $\gamma(R)$ is the shear [nc_wl_surface_mass_density_shear()] and $\kappa(R)$ is the convergence [nc_wl_surface_mass_density_convergence()].

Computes the reduced shear: $$ g(R) = \frac{\gamma(R)}{1 - \kappa(R)},$$ where $\gamma(R)$ is the shear [nc_wl_surface_mass_density_shear()] and $\kappa(R)$ is the convergence [nc_wl_surface_mass_density_convergence()].

Computes the reduced shear: $$ g(R) = \frac{\gamma(R)}{1 - \kappa(R)},$$ where $\gamma(R)$ is the shear [nc_wl_surface_mass_density_shear()] and $\kappa(R)$ is the convergence [nc_wl_surface_mass_density_convergence()].

Computes and stores the critical surface density.

Variant of #nc_wl_surface_mass_density_reduced_shear_crit_cache_prep() that reuses a pre-computed lens-side context. Only the source-side comoving distance and curvature transform are computed per call.

Computes the reduced shear assuming a lensed source at infinite redshift: $$ g(R) = \frac{\beta_s(zb)\gamma(R)}{1 - \beta_s(zb) \kappa(R)}, $$ where $\gamma(R)$ is the shear [nc_wl_surface_mass_density_shear()], $\kappa(R)$ is the convergence [nc_wl_surface_mass_density_convergence()], $z_b$ is the background-galaxy redshift and $$\beta_s = \frac{D_s}{D_l D_{ls}} \frac{D_\infty}{D_l D_{l\infty}}.$$ See Applegate (2014).

Computes the reduced shear: $$ g(R) = \frac{\gamma(R)}{1 - \kappa(R)},$$ where $\gamma(R)$ is the shear [nc_wl_surface_mass_density_shear()] and $\kappa(R)$ is the convergence [nc_wl_surface_mass_density_convergence()].

Computes the reduced shear: $$ g(R) = \frac{\gamma(R)}{1 - \kappa(R)},$$ where $\gamma(R)$ is the shear [nc_wl_surface_mass_density_shear()] and $\kappa(R)$ is the convergence [nc_wl_surface_mass_density_convergence()].

Increases the reference count of smd by one.

Computes the shear $\gamma(R)$ at R, see Eq $\eqref{eq:shear}$.

Computes the shear $\gamma_\infty (R)$ at R, see Eq $\eqref{eq:shear}$, and source at infinite redshift.

Computes the surface mass density at R, see Eq. $\eqref{eq:sigma}$.

Computes the surface mass density at R, see Eq. $\eqref{eq:sigma}$.

Computes the critical surface density, \begin{equation}\label{eq:def:SigmaC} \Sigma_c = \frac{c^2}{4\pi G} \frac{D_s}{D_l D_{ls}}, \end{equation} where $c^2$ is the speed of light squared [ncm_c_c2 ()], $G$ is the gravitational constant in units of $m^3/s^2 M_\odot^{-1}$ [ncm_c_G_mass_solar()], $D_s$ ($D_l$) is the angular diameter distance from the observer to the source (lens), and $D_{ls}$ is the angular diameter distance between the lens and the source.

Computes the critical surface density, \begin{equation}\label{eq:def:SigmaC} \Sigma_c = \frac{c^2}{4\pi G} \frac{D_\infty}{D_l D_{l\infty}}, \end{equation} where $c^2$ is the speed of light squared [ncm_c_c2 ()], $G$ is the gravitational constant in units of $m^3/s^2 M_\odot^{-1}$ [ncm_c_G_mass_solar()], $D_\infty$ ($D_l$) is the angular diameter distance from the observer to the source at infinite redshift (lens), and $D_{l\infty}$ is the angular diameter distance between the lens and the source.

Computes difference between the mean surface mass density inside the circle with radius R (Eq. $\eqref{eq:sigma_mean}$) and the surface mass density at R (Eq. $\eqref{eq:sigma}$).

Computes difference between the mean surface mass density inside the circle with radius R (Eq. $\eqref{eq:sigma_mean}$) and the surface mass density at R (Eq. $\eqref{eq:sigma}$).

Computes the mean surface mass density inside the circle with radius R, Eq. $\eqref{eq:sigma_mean}$.