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Surface Mass Density

A final, very central concept in lensing, is the convergence κ\kappa. This is the dimensionless, projected surface-mass density, which is related to ψ\psi through the Poisson equation. In our coordinates this gives

κ(θ)=12θψR\boxed{\kappa(\boldsymbol{\theta})= \frac12\nabla_\theta\psi^R}

Writing it out more explicitely, we find

κ(θ)=12(2ψRθ12+2ψRθ22)\kappa(\boldsymbol{\theta})= \frac12\left( \frac{\partial^2\psi^{\mathrm{R}}}{\partial\theta_1^2} + \frac{\partial^2\psi^{\mathrm{R}}}{\partial\theta_2^2} \right)

SIE (Singular isothermal ellipsoid)

The singular isothermal ellipsoid is a simple example of a non-spherical source.

The dimensionless projected surface-mass density κ\kappa is given as

κ(ξ1,ξ2)=fξ02ξ12+f2ξ22,\kappa(\xi_1,\xi_2)=\frac{\sqrt{f}\xi_0}{2\sqrt{\xi_1^2+f^2\xi_2^2}},

where the axis ratio ff obeys 0<f10\lt f\le1 and ξ0\xi_0 is a constant parameter related to the total mass (analogous to the Einstein radius RER_E).

Solving the Poisson equation, this gives, according to Kormann et al. (1994) the following.

ψξ0,f,θ,DLSIE(R)(θ,ϕ)=ξ0DL2f1f2θ([sin(ϕλL)]sin1(1f2sin(ϕλL))+[cos(ϕλL)]sinh1(1f2fcos(ϕλL))).\begin{aligned} \begin{split} \psi_{\xi_0,f,\theta,D_\mathrm{L}}^\textrm{SIE(R)}(\theta,\phi) = \frac{\xi_0}{D_\textrm{L}^2}\sqrt{\frac{f}{1-f^2}}\theta\cdot &\Bigg([\sin(\phi-\lambda_L)]\cdot\sin^{-1}\left(\sqrt{1-f^2}\cdot \sin{(\phi-\lambda_L)}\right) \\\\& +[\cos(\phi-\lambda_L)]\cdot\sinh^{-1}\left(\frac{\sqrt{1-f^2}}{f}\cos(\phi-\lambda_L)\right)\Bigg). \end{split} \end{aligned}

where (θ,ϕ)(\theta,\phi) are the polar coordinates in the lens plane, whereas λL\lambda_L is the orientation of the ellipse.

References
  1. Kormann, R., Schneider, P., & Bartelmann, M. (1994). Isothermal elliptical gravitational lens models. Astronomy and Astrophysics (ISSN 0004-6361), Vol. 284, No. 1, p. 285-299, 284, 285–299. https://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1994A&A...284..285K&classic=YES