TY - JOUR

T1 - Black hole mergers from globular clusters observable by LISA II. Resolved eccentric sources and the gravitational wave background

AU - D'Orazio, Daniel J.

AU - Samsing, Johan

PY - 2018/12/1

Y1 - 2018/12/1

N2 - In Paper I of this series we showed that a large per centage of the binary black hole (BBH) mergers that form through dynamical interactions in globular clusters will have significant eccentricity in the ~10-3 to 10-1 Hz LISA band. In this work we quantify the evolution of these highly eccentric binaries through the LISA and LIGO bands, and compute the stochastic gravitational wave background from the merging, eccentric population.We find that the population of BBHs that merge in-between three-body encounters inside their cluster (~50 per cent of all cluster-formed BBH mergers) will have measurable eccentricity for their entire lifetime in the LISA band. The population of BBHs that merge during three-body encounters (~5 per cent of all cluster-formed BBH mergers) will be detectable by LIGO with eccentricities of e ~ 0.1. The gravitational wave background from dynamically assembled BBHs encodes a characteristic bump due to the high initial eccentricities of these systems. The location and amplitude of this bump depend on globular cluster properties.

AB - In Paper I of this series we showed that a large per centage of the binary black hole (BBH) mergers that form through dynamical interactions in globular clusters will have significant eccentricity in the ~10-3 to 10-1 Hz LISA band. In this work we quantify the evolution of these highly eccentric binaries through the LISA and LIGO bands, and compute the stochastic gravitational wave background from the merging, eccentric population.We find that the population of BBHs that merge in-between three-body encounters inside their cluster (~50 per cent of all cluster-formed BBH mergers) will have measurable eccentricity for their entire lifetime in the LISA band. The population of BBHs that merge during three-body encounters (~5 per cent of all cluster-formed BBH mergers) will be detectable by LIGO with eccentricities of e ~ 0.1. The gravitational wave background from dynamically assembled BBHs encodes a characteristic bump due to the high initial eccentricities of these systems. The location and amplitude of this bump depend on globular cluster properties.

KW - Galaxies: star clusters: general

KW - Gravitational waves

UR - http://www.scopus.com/inward/record.url?scp=85056830736&partnerID=8YFLogxK

U2 - 10.1093/MNRAS/STY2568

DO - 10.1093/MNRAS/STY2568

M3 - Journal article

AN - SCOPUS:85056830736

VL - 481

SP - 4775

EP - 4785

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 4

ER -