Abstract
Abstract 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 (ΓHard = 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 (ΓSoft = 3.3 − 3.85) or warm Comptonization. These emissions are absorbed by a partial 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.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
