  In an earlier paper, we presented the first evidence for a bow-shock nebula
surrounding the X-ray binary LMC X-1 on a scale of ~15 pc, which we argued was
powered by a jet associated with an accretion disk. We now present the first
evidence for an ionization cone extending from an X-ray binary, a phenomenon
only seen to date in active galactic nuclei (AGN). The ionization cone,
detected in the HeII4686/Hbeta and [OIII]5007/Hbeta line ratio maps, aligns
with the direction of the jet inferred from the bow-shock nebula. The cone has
an opening angle ~45 deg and radial extent ~3.8 pc. Since the HeII emission
cannot be explained by the companion O star, the gas in the ionization cone
must be exposed to the `naked' accretion disk, thereby allowing us to place
constraints on the unobservable ionizing spectrum. The energetics of the
ionization cone give unambiguous evidence for an "ultraviolet - soft X-ray"
(XUV) excess in LMC X-1. Any attempt to match the hard X-ray spectrum (>1keV)
with a conventional model of the accretion disk fails to account for this XUV
component. We propose two likely sources for the observed anisotropy: (1)
obscuration by a dusty torus, or (2) a jet-blown hole in a surrounding envelope
of circumstellar absorbing material. We discuss the implications of our
discovery in the context of the mass-scaling hypothesis for accretion onto
black holes and suggest avenues for future research.
