9/18/2023 0 Comments Event horizon telescope paper![]() There are infinitely many more regions (which correspond to geodesics with diverging m) bunched up near the edge of the shadow (which corresponds to asymptotically bound photon orbits) but their area rapidly decreases with m and they become indiscernible past m > 3. The colours indicate the number m of angular turning points of the geodesic connecting the source to the observer: m = 0 (direct) light appears in the green region, while the yellow, blue and red regions correspond to relativistic images with m = 1, 2 and 3, respectively. The right image, which is reflection symmetric in accordance with the equatorial symmetry of the Kerr black hole, contains two whorls because gravity bends light from both the northern and southern poles back towards the observer. The left image, which is circularly symmetric in accordance with the axisymmetry of the Kerr black hole, depicts a swirling pattern around the pole that resembles a hair whorl. The black hole’s spin is counterclockwise about the origin in the left image, and right-handed about the β o-axis in the right image. Our result is different from the image published by the EHTC. The inner red circle is the locus α o 2 + β o 2 = M 2, corresponding to the would-be location of the event horizon, while the outer red contour is the edge of the shadow. We report our independent image reconstruction of the M 87 from the public data of the Event Horizon Telescope Collaborators (EHTC). The black lines are integral curves of the electric field (2.5). ![]() Polarimetric image observed by a ‘face-on’ observer at the pole ( θ o = 0°) and by an ‘edge-on’ observer in the equatorial plane ( θ o = 90°). ![]()
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