Mergers of globular clusters in the Galactic disc: intermediate mass black hole coalescence and implications for gravitational waves detection

Abstract

We propose a new formation channel for intermediate mass black hole (IMBH) binaries via globular cluster collisions in the Galactic disc. Using numerical simulations, we show that the IMBHs form a tight binary that enters the gravitational waves (GWs) emission dominated regime driven by stellar interactions, and ultimately merge in $\lesssim 0.5$ Gyr. These events are clearly audible to LISA and can be associated with electromagnetic emission during the last evolutionary stages. During their orbital evolution, the IMBHs produce runaway stars comparable with GAIA and LAMOST observations.

arXiv comment8 pages, 3 figures, 2 tables. Comments welcome

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Cited by in corpus (9)

• Dynamics of black hole - neutron star binaries in young star clusters
• Dynamics of binary black holes in low-mass young star clusters
• Formation of super-massive black holes in galactic nuclei I: delivering seed intermediate-mass black holes in massive stellar clusters
• Effect of mass loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters
• Formation of supermassive black holes in galactic nuclei II: retention and growth of seed intermediate-mass black holes
• Merging Hierarchical Triple Black Hole Systems with Intermediate-mass Black Holes in Population III Star Clusters
• Dynamically Formed Black Hole Binaries: In-Cluster Versus Ejected Mergers
• A rapid channel for the collisional formation and gravitational wave driven mergers of supermassive black hole seeds at high redshift
• Measuring the Matter Density of the Galactic Disk Using Stellar Streams