LISA capture sources: Approximate waveforms, signal-to-noise ratios, and parameter estimation accuracy

  title={LISA capture sources: Approximate waveforms, signal-to-noise ratios, and parameter estimation accuracy},
  author={Leor Barack and Curt Cutler},
  journal={Physical Review D},
Captures of stellar-mass compact objects (COs) by massive ($\sim 10^6 M_\odot$) black holes (MBHs) are potentially an important source for LISA, the proposed space-based gravitational-wave (GW) detector. The orbits of the inspiraling COs are highly complicated; they can remain rather eccentric up until the final plunge, and display extreme versions of relativistic perihelion precession and Lense-Thirring precession of the orbital plane. The strongest capture signals will be ~10 times weaker… 

An Efficient Signal-to-noise Approximation for Eccentric Inspiraling Binaries

This work outlines a method for estimating the signal-to-noise ratio (S/N) for inspiraling binaries at lower frequencies such as those proposed for LISA and DECIGO and shows a distinctive way to identify events with extremely high eccentricity where the signal is enhanced relative to naive expectations on the high-frequency end.

Detecting extreme mass ratio inspirals with LISA using time–frequency methods: II. Search characterization

The inspirals of stellar-mass compact objects into supermassive black holes constitute some of the most important sources for LISA. Detection of these sources using fully coherent matched filtering

Augmented kludge waveforms for detecting extreme-mass-ratio inspirals

The latest implementation of an augmented analytic kludge (AAK) model is presented, publicly available at as part of an EMRI waveform software suite, and is well suited for scoping out data analysis issues in the upcoming round of mock LISA data challenges.

Gravitational wave background from extreme mass ratio inspirals

Extreme mass ratio inspirals (EMRIs), i.e. binary systems comprised by a compact stellar-mass object orbiting a massive black hole, are expected to be among the primary gravitational wave (GW)

Golden Binary Gravitational-Wave Sources: Robust Probes of Strong-Field Gravity

Space-borne gravitational-wave interferometers such as LISA will detect the gravitational wave (GW) signal from the inspiral, plunge, and ringdown phases of massive black hole binary mergers at

A principal component analysis of gravitational-wave signals from extreme-mass-ratio sources

The Laser Interferometer Space Antenna (LISA) will detect the gravitational wave emissions from a vast number of astrophysical sources, but extracting useful information about individual sources or

'Kludge' gravitational waveforms for a test-body orbiting a Kerr black hole

One of the most exciting potential sources of gravitational waves for low-frequency, space-based gravitational wave (GW) detectors such as the proposed Laser Interferometer Space Antenna (LISA) is

Improved time–frequency analysis of extreme-mass-ratio inspiral signals in mock LISA data

The planned Laser Interferometer Space Antenna (LISA) is expected to detect gravitational wave signals from ∼100 extreme-mass-ratio inspirals (EMRIs) of stellar-mass compact objects into massive

Extremely large mass-ratio inspirals

The detection of the gravitational waves (GWs) emitted in the capture process of a compact object by a massive black hole (MBH) is known as an extreme-mass ratio inspiral (EMRI) and represents a

Assessing the detectability of the secondary spin in extreme mass-ratio inspirals with fully relativistic numerical waveforms

Extreme mass-ratio inspirals (EMRIs) detectable by the Laser Inteferometric Space Antenna (LISA) are unique probes of astrophysics and fundamental physics. Parameter estimation for these sources is



Detection template families for gravitational waves from the final stages of binary--black-hole inspirals: Nonspinning case

We investigate the problem of detecting gravitational waves from binaries of nonspinning black holes with masses m=5-20M., moving on quasicircular orbits, which are arguably the most promising

Angular resolution of the LISA gravitational wave detector

We calculate the angular resolution of the planned LISA detector, a space-based laser interferometer for measuring low-frequency gravitational waves from galactic and extragalactic sources. LISA is

Spin-induced orbital precession and its modulation of the gravitational waveforms from merging binaries.

This paper analyzes the resulting modulation of the inspiral gravitational waveform, using post2-Newtonian equations to describe the precession of the orbital plane, but only the leading-order ( newtonian, quadrupole-moment approximation) equations to describes the orbit, the radiation reaction, the inspirals, and the wave generation.

Gravitational waves from merging compact binaries: How accurately can one extract the binary's parameters from the inspiral waveform?

This work investigates how accurately the distance to the source and the masses and spins of the two bodies will be measured from the inspiral gravitational wave signals by the three-detector LIGO-VIRGO network using ``advanced detectors'' (those present a few years after initial operation).

Accuracy of parameter estimation of gravitational waves with LISA

LISA is a space-borne, laser-interferometric gravitational-wave detector currently under study by the European Space Agency. We give a brief introduction about the main features of the detector,

Gravitational waves from a compact star in a circular, inspiral orbit, in the equatorial plane of a massive, spinning black hole, as observed by LISA

Results are presented from high-precision computations of the orbital evolution and emitted gravitational waves for a stellar-mass object spiraling into a massive black hole in a slowly shrinking,

The gravitational wave background from cosmological compact binaries

We use a population synthesis approach to characterize, as a function of cosmic time, the extragalactic close binary population descended from stars of low to intermediate initial mass. The

Gravitational Waves from Stars Orbiting the Sagittarius A* Black Hole

One of the main astrophysical processes leading to strong emission of gravitational waves to be detected by the future space-borne interferometer Laser Interferometer Space Antenna (LISA) is the

The Distance to the Galactic Center

The Optical Gravitational Lensing Experiment (OGLE) data on high‐amplitude δ Scuti stars (HADS) and RR Lyrae stars have been analyzed to determine the distance to the Galactic bulge. Individual color

Measuring black-hole parameters and testing general relativity using gravitational-wave data from space-based interferometers.

  • Poisson
  • Materials Science, Physics
    Physical review. D, Particles and fields
  • 1996
A simple model for the gravitational-wave signal is constructed, in which the phasing of the waves plays the dominant role, and a method for experimentally testing the strong-field predictions of general relativity is suggested.