![Profile of a quasar accretion disk magnified by microlensing. The continuous curve corresponds to a relativistic model with innermost stable orbit at 3 Schwarzschild radii. Notice that one of the peaks is enhanced by relativistic beaming. The dashed curve Profile of a quasar accretion disk magnified by microlensing. The continuous curve corresponds to a relativistic model with innermost stable orbit at 3 Schwarzschild radii. Notice that one of the peaks is enhanced by relativistic beaming. The dashed curve](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/news/resultados157_173.jpg?itok=qF5k0VeM)
The one-way frontier around a black hole is the event horizon from which nothing can escape. Close to it, strong effects of gravity and exotic physics are expected. The most massive black holes are at the centre of distant quasars, which cannot be resolved by telescopes. Fortunately, in some quasars aligned with an intervening galaxy, gravitational microlensing can magnify very small regions within the quasar allowing horizon scale resolution. We have used three events of gravitational microlensing that scan the source of a lensed quasar (Einstein Cross) to resolve a structure, affected by
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