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Fig. 12.


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Probability, 𝒫, that a galaxy hosting a LISA MBHB (left) and a single MBHs (right) will undergo a galaxy merger within ΔtBin. Solid, dashed, and dotted lines correspond to any baryonic mass ratio (mR), mR > 0.2, and mR > 0.01, respectively. Top, middle, and bottom panels: results for MBin = 104 − 105M, 105 − 106M, and 106 − 107M, 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.

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