Gravitational wave signals from the first massive black hole seeds. (24th May 2018)

• Record Type: Journal Article
• Authors: Hartwig, Tilman; Agarwal, Bhaskar; Regan, John A
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 479:Number 1(2018:Sep.)
• Page Start: L23
• Page End: L27
• Publication Date: 2018-05-24
• Subjects: gravitational waves -- galaxies: high-redshift -- quasars: supermassive black holes -- cosmology: dark ages, reionization, first stars; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/sly091
• Languages: English
• ISSNs: 1745-3933

Abstract

ABSTRACT: Recent numerical simulations reveal that the isothermal collapse of pristine gas in atomic cooling haloes may result in stellar binaries of supermassive stars with $M_*\gtrsim 10^4\, \mathrm{M}_{\odot }$ . For the first time, we compute the in-situ merger rate for such massive black hole remnants by combining their abundance and multiplicity estimates. For black holes with initial masses in the range $10^{4-6} \, \mathrm{M}_{\odot }$ merging at redshifts z ≳ 15 our optimistic model predicts that Laser Interferometer Space Antenna ( LISA ) should be able to detect 0.6 mergers yr −1 . This rate of detection can be attributed, without confusion, to the in-situ mergers of seeds from the collapse of very massive stars. Equally, in the case where LISA observes no mergers from heavy seeds at z ≳ 15 we can constrain the combined number density, multiplicity, and coalescence times of these high-redshift systems. This letter proposes gravitational wave signatures as a means to constrain theoretical models and processes that govern the abundance of massive black hole seeds in the early Universe.