Probability, 𝒫, that a galaxy hosting a LISA MBHB (left) and a single MBHs (right) will undergo a galaxy merger within Δt_Bin. Solid, dashed, and dotted lines correspond to any baryonic mass ratio (m_R), m_R > 0.2, and m_R > 0.01, respectively. Top, middle, and bottom panels: results for M_Bin = 10⁴ − 10⁵ M_⊙, 10⁵ − 10⁶ M_⊙, and 10⁶ − 10⁷ M_⊙, respectively. The large probability values shown in this figure show that galaxies hosting the LISA source display merger signatures that are uncorrelated with the galaxy merger that led to the MBHB formation and coalescence.