Notes. The spectral shape was derived from spectral analysis of the time-variable diffuse emission in Chandra data and only normalizations were adjusted to best fit the full spectra (together with other components). Normalization was adjusted by a constant factor 0.85 to match IXPE Stokes I spectra for the same regions. The columns show absorbing column density (N_H), incident powerlaw index Γ, optical depth of the cloud τ_T, cosine of the scattering angle µ, abundance of heavy elements with respect to the Solar values A (see Churazov et al. 2017a for a detailed description of the CREFL16 model), and they were fixed at values found in combined epoch-resolved XMM-Newton and Chandra spectroscopy performed in Marin et al. (2023). The normalizations (defined per arcmin²) of the continuum (Norm_cont) and of the fluorescent lines (Norm_fluor) components of this model were mutually untied and independently fitted for the regions of interest here (the uncertainties correspond to 1σ confidence intervals). Intrinsic model’s normalization equal to 10⁻² corresponds to unabsorbed 3–8 keV flux of 9.1 × 10⁻¹⁴ erg s⁻¹ cm⁻² and 4.2 × 10⁻¹⁴ erg s⁻¹ cm⁻² for the continuum and fluorescent components respectively. The last column, Frac_3−6,cont, gives the relative contribution of the reflected continuum to the total 3–6 keV flux from these regions.