2023/11/08 by CJ Harris, Harris, CJ, Kayhan Gültekin +1
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics of Galaxies (astro-ph.GA) #Binary black hole #Binary number #Black hole (networking) #Computer science #Core (optical fiber) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gravitational wave #Mass ratio #Physics #Population #Pulsars and Gravitational Waves Research #Star formation #Stellar mass
paper · pdf · doi:10.48550/arxiv.2311.04877
published in arXiv (Cornell University) (Cornell University)
openalex publication_date 2023/11/08 · openalex created_date 2023/11/11 · openalex updated_date 2026/07/28
We investigate how the properties of massive black hole binaries influence the observed properties of core galaxies. We compare the observed trend in stellar mass deficit as a function of total stellar mass in the core galaxy with predicted trends in IllustrisTNG. We calculate mass deficits in simulated galaxies by applying sub-grid, post-processing physics based on the results of literature N-body experiments. We find the median value of the posterior distribution for the minimum binary mass ratio capable of creating a core is 0.7. For the gas mass fraction above which a core is erased we find a median value of 0.6. Thus low mass ratio binaries do not contribute to core formation and gas-rich mergers must lead to star formation within the nucleus, ultimately erasing the core. Such constraints have important implications for the overall massive black hole binary population, black hole-galaxy co-evolution, and the origin of the gravitational wave background.