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The above radiation pattern was computed using [[EM.Libera]], [[EM.Cube]]'s MoM3D computational module. The φ and θ components of the far-zone electric fields in the standard spherical coordinate system are stored in an ASCII data file with a ".RAD" file extension. With an original angular resolution of 1°, the data file contains a total of 361 × 181 = 65,341 rows containing the real and imaginary parts of the complex-valued E<sub>θ</sub> and E<sub>φ</sub> field components. This provides a fully polarimetric representation of the source's outgoing fields, which are then picked up and traced by [[EM.Terrano]]'s fully coherent and 3D-polarimetric SBR solver. Note that the complexity of the radiation pattern data file does not add any computational overhead to the SBR simulation. The figure below shows the received power coverage map of the Manhattan scene with an X-directed horizontal Yagi-Uda array. You can visibly see the directionality of the pattern of the transmitter from the coverage map in the area below the transmitter. Also note that the maximum received power in this case is -37dBm, which is 7dB larger than the previous case with a vertical dipole transmitter. This increase is accounted for by the greater directivity (D<sub>0</sub> = 10dB) of the transmitter antenna, and hence the larger transmitted EIRP.
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[[EM.Terrano]] allows the user to rotate an imported far-field radiation pattern about the three principal coordinate axes. Next, we rotate the radiation pattern of the Yagi-Uda array by 135° and run a new SBR simulation of the propagation scene. The results are shown in the figure below.
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