Using evolutionary algorithms to model relativistic jets: Application to
  NGC 1052
  High-resolution Very-Long-Baseline Interferometry observations of NGC 1052
show a two sided jet with several regions of enhanced emission and a clear
emission gap between the two jets.This gap shrinks with increasing frequency
and vanishes around $\nu\sim43$ GHz. The observed structures are due to both
the macroscopic fluid dynamics interacting with the surrounding ambient medium
including an obscuring torus and the radiation microphysics. In this paper we
investigate the possible physical conditions in relativistic jets of NGC 1052
by directly modelling the observed emission and spectra via state-of-the-art
special-relativistic hydrodynamic (SRHD) simulations and radiative transfer
calculations. To investigate the physical conditions in the relativistic jet we
coupled our radiative transfer code to evolutionary algorithms and performed
simultaneous modelling of the observed jet structure and the broadband radio
spectrum. During the calculation of the radiation we consider both thermal and
non-thermal emission. In order to compare our model to VLBI observations we
take into account the sparse sampling of the u-v plane, the array properties
and the imaging algorithm. We present for the first time an end-to-end pipeline
for fitting numerical simulations to VLBI observations of relativistic jets
taking into account the macrophysics including fluid dynamics and ambient
medium configurations together with thermal/non-thermal emission and the
properties of the observing array. The detailed analysis of our simulations
shows that the structure and properties of the observed relativistic jets in
NGC 1052 can be reconstructed by a slightly over-pressured jet ($d_k\sim1.5$)
embedded in a decreasing pressure ambient medium
