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The main idea of our research is to estimate the physical coalescence time ofthe double supermassive black hole (SMBH) system in the centre of NGC 6240based on the X-ray observations from the Chandra space observatory. The spectraof the Northern and Southern nuclei were fitted by spectral models from Sherpaand both presented the narrow component of the Fe K$\alpha$ emission line. Itenabled us to apply the spectral model to these lines and to find relativeoffset $\approx0.02$ keV. The enclosed dynamical mass of the central region ofNGC 6240 with radius 1 kpc was estimated $\approx 2.04\times 10^{11} \rm\;M_{\odot}$. These data allowed us to carry on the high resolution direct N-bodysimulations with Newtonian and post-Newtonian (up to $2.5\mathcal{PN}$correction) dynamics for this particular double SMBH system. As a result, fromour numerical models we approximated the central SMBH binary merging time forthe different binary eccentricities. In our numerical parameters range theupper limit for the merging time, even for the very small eccentricities, isstill below $\approx70$ Myr. Gravitational waveforms and amplitude-frequencypictures from such events can be detected using Pulsar Timing Array (PTA)projects at the last merging phase.

NGC 6240 Supermassive Black Hole Binary dynamical evolution based on Chandra data