Are stellar-mass black-hole binaries too quiet for LISA?

  title={Are stellar-mass black-hole binaries too quiet for LISA?},
  author={Christopher J. Moore and Davide Gerosa and Antoine Klein},
  journal={Monthly Notices of the Royal Astronomical Society: Letters},
The progenitors of the high-mass black-hole mergers observed by LIGO and Virgo are potential LISA sources and promising candidates for multiband GW observations. In this letter, we consider the minimum signal-to-noise ratio these sources must have to be detected by LISA bearing in mind the long duration and complexity of the signals. Our revised threshold of ρthr ∼ 15 is higher than previous estimates, which significantly reduces the expected number of events. We also point out the importance… 

Figures and Tables from this paper

Archival searches for stellar-mass binary black holes in LISA data

Stellar-mass binary black holes will sweep through the frequency band of the Laser Interferometer Space Antenna (LISA) for months to years before appearing in the audio-band of ground-based

Parameter estimation of stellar-mass black hole binaries with LISA

Stellar-mass black hole binaries (SBHBs), like those currently being detected with the ground-based gravitational-wave (GW) observatories LIGO and Virgo, are also an anticipated GW source for LISA.

Multiband observation of LIGO/Virgo binary black hole mergers in the gravitational-wave transient catalog GWTC-1

The Advanced LIGO and Virgo detectors opened a new era to study black holes (BHs) in our Universe. A population of stellar-mass binary BHs (BBHs) are discovered to be heavier than previously

Gravitational-wave Detection and Parameter Estimation for Accreting Black-hole Binaries and Their Electromagnetic Counterpart

We study the impact of gas accretion on the orbital evolution of black-hole binaries initially at large separation in the band of the planned Laser Interferometer Space Antenna (LISA). We focus on

Bayesian parameter estimation of stellar-mass black-hole binaries with LISA

A Bayesian parameter-estimation pipeline to measure the properties of inspiralling stellar-mass black hole binaries with LISA is presented and the successful recovery of an eccentric, spin-precessing source at signal-to-noise ratio 15 is reported.

Observing GW190521-like binary black holes and their environment with LISA

Binaries of relatively massive black holes like GW190521 have been proposed to form in dense gas environments, such as the disks of Active Galactic Nuclei (AGNs), and they might be associated with

Peculiar acceleration of stellar-origin black hole binaries: Measurement and biases with LISA

We investigate the ability of the Laser Interferometer Space Antenna (LISA) to measure the center of mass acceleration of stellar-origin black hole binaries emitting gravitational waves. Our analysis

Search for neutron star binaries in the Local Group galaxies using LISA

  • N. Seto
  • Physics
    Monthly Notices of the Royal Astronomical Society
  • 2019
We discuss the prospects of LISA for detecting neutron star binaries (NSBs) in the Local Group galaxies such as LMC and M31. Using the recently estimated merger rate ${\rm 1540 \, Gpc^{-3}\,

Tests of general relativity with stellar-mass black hole binaries observed by LISA

We consider the observation of stellar-mass black holes binaries with the Laser Interferometer Space Antenna (LISA). Preliminary results based on Fisher information matrix analyses have suggested

On detecting stellar binary black holes via the LISA-Taiji network

The detection of gravitational waves (GWs) by ground-based laser interferometer GW observatories (LIGO/Virgo) reveals a population of stellar binary black holes (sBBHs) with (total) masses up to ∼



LISA Sources in Milky Way Globular Clusters.

Some double-compact-object binaries in Milky Way globular clusters that may be detectable by the Laser Interferometer Space Antenna can have signal-to-noise ratios large enough to be detectable at the distance of the Andromeda galaxy or even the Virgo cluster.

Concise estimate of the expected number of detections for stellar-mass binary black holes by eLISA

We study prospects for detecting extragalactic binary black holes similar to GW150914 by evolved Laser Interferometer Space Antenna (eLISA). We find that the majority of detected binary black holes

Black Hole X-ray Transients: The Formation Puzzle

There are 19 confirmed BH binaries in the Galaxy. 16 of them are X-ray transients hosting a ~5-15 Msun BH and a Roche-lobe overflowing low-mass companion. Companion masses are found mostly in 0.1-1

Optimizing LIGO with LISA forewarnings to improve black-hole spectroscopy

The early inspiral of massive stellar-mass black-hole binaries merging in LIGO’s sensitivity band will be detectable at low frequencies by the upcoming space mission LISA. LISA will predict, with

Event Rate Estimates for LISA Extreme Mass Ratio Capture Sources

One of the most exciting prospects for the LISA gravitational wave observatory is the detection of gravitational radiation from the inspiral of a compact object into a supermassive black hole. The

Black Hole Mergers From Globular Clusters Observable by LISA I: Eccentric Sources Originating From Relativistic N-body Dynamics

We show that nearly half of all binary black hole (BBH) mergers dynamically assembled in globular clusters have measurable eccentricities (e > 0.01) in the LISA band (10^−2 Hz), when General

Stellar binary black holes in the LISA band: a new class of standard sirens

The recent Advanced LIGO detections of coalescing black hole binaries (BHBs) imply a large population of such systems emitting at milli-Hz frequencies, accessible to the Laser Interferometer Space

Post-Newtonian phase accuracy requirements for stellar black hole binaries with LISA

The Laser Interferometer Space Antenna (LISA) will observe black hole binaries of stellar origin during their gravitational wave inspiral, months to years before coalescence. Due to the long duration


The recent detections of GW150914 and GW151226 imply an abundance of stellar-mass binary black hole (BBH) mergers in the local universe. While ground-based gravitational wave detectors are limited to

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

The first observational run of the Advanced LIGO detectors, from September 12, 2015 to January 19, 2016, saw the first detections of gravitational waves from binary black hole mergers. In this paper