Re-simulated H_α profile for E36 in the LOS along the x-direction. The left column shows results for constant masses of MBHs but varying accretion rates. For the same values of the accretion rates as shown in the left column, we show the results when the primary MBH is ten times more massive than the secondary MBH. The blue (pink) dashed line represents the contribution from primary (secondary) MBH. The bottom inset in each panel refers to the added random noise in the synthetic spectrum along with the residual of the best-fitting model as explained in Sect. 5.2.