Determining the Hubble Constant from the Gravitational Lens PG 1115+080

Details Determining the Hubble Constant from the Gravitational Lens PG 1115+080 Determining the Hubble Constant from the Gravitational Lens PG 1115+080

1996-11-26

arxiv.org/abs/astro-ph/9611216v2

Astronomy and Astrophysics

Astrophysics

revised to use the updated time delays of Bar-Kana astro-ph/9701068; 30 pages, 7 Postscript figures, to appear in ApJ

Scientific paper

10.1086/304583

For the quadruple gravitational lens PG 1115+080, we combine recent measurements of the time delays with new lens models to determine the Hubble constant H_0. We explore the effects of systematic uncertainties in the lens models on the estimates of H_0, and we discuss how the uncertainties can be reduced by future observations. We find that the lens cannot be fit by an isolated lens galaxy, but that it can be well fit by including a perturbation from the nearby group of galaxies. To understand the full range of systematic uncertainties it is crucial to use an ellipsoidal galaxy and to let the group position vary. In this case, the existing constraints cannot break degeneracies in the models with respect to the profiles of the galaxy and group and to the position of the group. Combining the known time delays with a range of lens models incorporating most of the plausible systematic effects yields H_0 = 51_{-13}^{+14} km s^{-1} Mpc^{-1}. The constraints on the lens models, and hence on H_0, can be improved by reducing the standard errors in the lens galaxy position from 50 mas to \sim10 mas, reducing the uncertainties in the time delays to \sim0.5 days, and constraining the lens mass distribution using HST photometry and the fundamental plane. In particular, the time delay ratio r_{ABC} = \Delta\tau_{AC} / \Delta\tau_{BA} may provide the best constraint on the mass profile of the galaxy.

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