Notes. All errors are quoted at the 90% confidence level. Taking Data set 3 as an example, the probability distributions of parameters obtained through the Markov chain Monte Carlo (MCMC) algorithm are presented in Fig. A.1; ^( ⋆ ) indicates that the parameters between different data sets are linked; N_H is the X-ray absorption column density in units of 10²² atoms cm⁻²; T_in is the inner disk temperature in units of keV; Γ is the power-law photon index of the thermal Comptonization component; kT_e is the electron temperature of the corona in units of keV, standing for the high energy cutoff of the Comptonization continuum; q_in and q_out are respectively the inner and outer emissivity indices for the coronal flavor models; R_in (R_ISCO) is the inner radius of the accretion disk in units of R_ISCO; A_Fe is the iron abundance of the accretion disk in units of solar abundance; ξ is the ionization parameter of the accretion disk in units of erg cm s⁻¹; N is the density of the accretion disk in units of cm⁻³; i is the disk inclination angle in units of deg; norm is the normalization; F_abs and F_unabs are absorbed and unabsorbed fluxes in units of 10⁻⁸ erg cm⁻² s⁻¹; L_X is the absorption-corrected 0.5–100 keV luminosity, calculated by L_X = 4 × π × D² × F_unabs, where D = 7.5 kpc; L_Edd is the Eddington luminosity with BH mass 9.4 M_⊙ (i.e., L_Edd = 1.2 × 10³⁹ erg s⁻¹); F_relxillNS/F_X is the ratio of the flux of the reflection component to the total flux in 0.5–100 keV.