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.

8 pages, 3 figures, 2 tables. Comments welcome

References in corpus (6)

• Massive black hole binary mergers within sub-pc scale gas discs
• Observational evidence for intermediate-mass black holes
• Binary Black Hole Accretion During Inspiral and Merger
• A stellar-mass black hole population in the globular cluster NGC 6101?
• Evidence for an intermediate-mass black hole in the globular cluster NGC 6624
• Mass models of NGC 6624 without an intermediate-mass black hole

Cited by in corpus (6)

• Dynamics of binary black holes in low-mass young star 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