Fig. 3: A zoom-in picture of XRISM/Resolve spectrum of the Circinus galaxy around the Fe Kα emission line.
From: Accurate determination of chemical abundances near a supermassive black hole
They are folded by the instrumental response in units of EFE, where FE is the energy flux at energy E. The observed data are plotted in black with error bars denoting the 1σ confidence limits in photon statistics. The blue, cyan and red lines represent the models of the emission lines from cold matter, the reflection continuum from cold matter and the total, respectively. The dashed lines denote the case where Compton scattering from free electrons at zero temperature is considered. In the inset, the observational data are compared against our best-fit model (red) and a model to which no Gaussian broadening is applied (grey). This shows that Doppler broadening is very small compared with the intrinsic width of the Fe Kα line.
