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Using long-slit optical spectroscopy obtained at the 10.4 m Gran TelescopioCanarias, we have examined the gaseous environment of the radio-loud quasar TXS1436+157 (z=2.54), previously known to be associated with a large Ly-alphanebula and a spatially extended Ly-alpha-absorbing structure. From the Ly-alphanebula we measure kinematic properties consistent with infall at a rate ofabout 10-100 M./yr - more than sufficient to power a quasar at the top of theluminosity function. The absorbing structure lies outside of the Ly-alphanebula, at a radius of >40 kpc from the quasar. Against the bright unresolvedcontinuum and line emission from the quasar, we detect in absorption the NV1239,1241, CIV 1548,1551 and SiIV 1394,1403 doublets, with no unambiguousdetection of absorption lines from any low-ionization species of metal. Themetal column densities, taken together with the HI column density measurementfrom the literature, indicate that the absorbing gas is predominantly ionizedby the quasar, has a mass of hydrogen of >1.6 x 10E11 M., a gas density of <18per cubic cm, a line of sight thickness of >18 pc, and a covering factorapproaching unity. While this absorbing structure is clearly not composed ofpristine gas, it has an extremely low metallicity, with ionization modelsproviding a 3-sigma limit of 12+log(O/H)<7.3. To explain these results, wediscuss a scenario involving starburst-driven super-bubbles and the creation ofinfalling filaments of cold gas which fuel/trigger the quasar. We also discussthe possibility of detecting large-scale absorbers such as this in emissionwhen illuminated by a powerful quasar.

A massive bubble of extremely metal poor gas around a collapsing Ly-alpha blob at z=2.54