Broad-Band X-Ray Analysis of NGC 3227

Previously in Project A we carried out analysis of the data obtained by observations of the 1.5 Seyfert galaxy NGC 3227-the two observations performed by XMM-Newton in 2000 and 2006 and six observations by Suzaku in 2008. In the current paper, Project B, our work was extended to joint XMM-Newton and NuSTAR observations in 2016 as well as a NuSTAR observation in 2017. In Project A a unified model was constructed. The model consists of a hard power law ($\Gamma _{\mathrm{ Hard}}=1.4{\!-\!}1.7$) which is interpreted as the Comptonized emission from the corona above an accretion disk. In the high flux states an additional soft excess component dominates, which is consistent with either a power law ($\Gamma _{\mathrm{ Soft}}=3.3{\!-\!}3.85$) or warm Comptonization. These emissions are absorbed by a partially covering material and warm absorbers. A reflection component and several emission lines are also present. In Project B, the model presented in Project A was applied to more recent observations. It was found that this model remains valid. Our conclusion is that this model is consistent, valid with the long observations from 2000 to 2017 and over the broad frequency band from 0.3 keV to 50 keV.