2002MNRAS.332..951W

The time-delay in gravitational lenses can be used to derive the Hubble constant in a relatively simple way. The results of this method are less dependent on astrophysical assumptions than in many other methods. For systems with accurately measured positions and time-delays, the most important uncertainty is related to the mass model used. Simple parametric models like isothermal ellipsoidal mass distributions seem to provide consistent results with a reasonably small scatter when applied to several lens systems. We discuss a family of models with a separable radial power law and an arbitrary angular dependence for the potential ψ=r^βF(θ). Isothermal potentials are a special case of these models with β =1. An additional external shear is used to take into account perturbations from other galaxies. Using a simple linear formalism for quadruple lenses, we can derive H₀ as a function of the observables and the shear. If the latter is fixed, the result depends on the assumed power-law exponent according to H₀∝(2-β)/β. The effect of external shear is quantified by introducing a `critical shear' γ_c as a measure for the amount of shear that changes the result significantly. The analysis shows that in the general case H₀ and γ_c do not depend on the position of the lens galaxy. Spherical lens models with images close to the Einstein radius with fitted external shear differ by a factor of β/2 from shearless models, leading to H₀∝2-β in this case. We discuss these results and compare them with numerical models for a number of real lens systems.