The Contribution of Outer H i Disks to the Merging Binary Black Hole Population

2017/10/25 by Sukanya Chakrabarti, Philip Chang, Richard O'Shaughnessy +7 · 8 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Binary black hole #Binary number #Black hole (networking) #Dwarf galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Metallicity #Population #Spiral galaxy #Star formation #astro-ph.GA

paper · pdf · doi:10.3847/2041-8213/aa9655

published in The Astrophysical Journal Letters 850(1), L4 (IOP Publishing) · accepted to ApJL, 5 pages, 2 figures

arxiv created 2017/10/25 · openalex created_date 2017/11/10 · openalex publication_date 2017/11/13 · arxiv updated 2017/11/29 · openalex updated_date 2026/08/06

Abstract

Abstract We investigate the contribution of outer H i disks to the observable population of merging black hole binaries. Like dwarf galaxies, the outer H i disks of spirals have low star formation rates and lower metallicities than the inner disks of spirals. Since low-metallicity star formation can produce more detectable compact binaries than typical star formation, the environments in the outskirts of spiral galaxies may be conducive to producing a rich population of massive binary black holes. We consider here both detailed controlled simulations of spirals and cosmological simulations, as well as the current range of observed values for metallicity and star formation in outer disks. We find that the outer H i disks contribute at least as much as dwarf galaxies do to the observed LIGO/Virgo detection rates. Identifying the host galaxies of merging massive black holes should provide constraints on cosmological parameters and insights into the formation channels of binary mergers.

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