The signatures of voids — I. Numerical model

In this paper, we describe the ray-tracing code used to calculate the signatures of quasi-linear voids in front of, and on, the last scattering surface. The spherically symmetric, general relativistic, Lagrangian fluid equations are integrated in time along with the geodesic equations. The voids are partially filled and are surrounded by either cold dark matter or interacting fluid with a small amount of pressure. In order to obtain accurate results using smaller arrays, a non-uniform grid is employed.