Simulations of Gamma-Ray Emission from Magnetized Microquasar Jets

Figure 4

Scenario C (run3): illustration of the synthetic -ray images. In the plots the x-y plane defines the (synthetic) observation plane. -axis represents the intensity at each pixel of the observation plane (arbitrary units). For each one of the latter, a line of sight (LOS) is drawn that crosses the computational domain volume and ends up at the aforementioned pixel. The radiative intensity along the LOS is calculated using the radiative transfer equation. We see two different cases for emission coefficient used, with two snapshots for each case. In the first row, is used as emission coefficient (the intensity appears higher when the matter is denser). In the second row, is used as emission coefficient. The fast-moving jet matter now prevails in terms of -ray intensity, as compared to the clearly lower emission from slower moving surrounding material. In both configurations, we see the distinct signature of the precessing jet on the bent jet emission patterns formed, as well as on resolution effects at a faster pace than the rest of runs. In order to compare those images to actual observations, one would have to convolve them with the “beam” of the observing instrument, as it is provided by the operator. As a first step, it is possible to compare the sensitivity of an observing gamma-ray instrument to the “sensitivity” of the synthetic images, using a process similar to the one described in SK14.

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