Where are the absorbers towards Q2302+029?

We present images and spectroscopy of objects close to the sightline of Q2302+029 in order to search for galaxies responsible for the remarkable z=0.7 high-ionization absorption line system found by Jannuzi et al (1996). This system shows `normal' narrow OVI, NV, and CIV lines superimposed on broader (3,000-5,000 km/s wide), unsaturated absorption troughs some 56,000 km/s away from the QSO emission redshift (z=1.052). Despite reaching sensitivities sufficient to detect 1/10 L* galaxies in the optical and 1/20 L* in the infra-red, we are unable to detect any obvious bright galaxies which might be responsible for the absorption beyond ~ 6 h-1 kpc of the sightline. This supports the hypotheses that the absorption is either intrinsic to the QSO, or arises in intracluster gas. Adopting either explanation is problematic: in the first case, `associated' absorption at such high ejection velocities is hard to understand, and challenges the conventional discrimination between intrinsic and intervening absorbers; in the second case, the gas must reside in a ~ 40 h-1 Mpc long filament aligned along the line of sight in order to reproduce the broad absorption. Spectroscopy of objects beyond the immediate vicinity of the QSO sightline reveals a galaxy cluster at z=0.59, which coincides with strong Lya and more narrow high ionization lines in the quasar spectrum. Here too, the lack of galaxies at distances comparable to those found for, e.g., Lya-absorbing galaxies, suggests that the absorption may arise from intracluster gas unassociated with any individual galaxies.