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Fig. 2


Synchrotron emission map created using a GRMHD simulation (see Sect. 4.2.2) made using the HARM code (Gammie et al. 2003). Intensity is given in units of Jy pixel−2. The observer frequency is 100 GHz, the inclination angle is 30 degrees, and the disk-dominated emission model discussed in Sect. 5 is used. Note the optically-thick accretion disk and strong emission to the left of the black-hole shadow (this region appears bright due to relativistic beaming). The ray investigated in Fig. 1 is marked by a white dot in this image. This particular ray, travelling from the plasma to the observer, first passes through the bright, relativistically-boosted region, and then through an optically-thick, non-boosted region of the disk, suggesting that the specific intensity along this ray will sharply increase, then decrease, before reaching the observer. Figure 1 shows that this is indeed the case.

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