Interplay of spin-precession and higher harmonics in the parameter estimation of binary black holes

  title={Interplay of spin-precession and higher harmonics in the parameter estimation of binary black holes},
  author={N. V. Krishnendu and Frank Ohme},
  journal={Physical Review D},
Gravitational-wave signals from coalescing compact binaries carry an enormous amount of information about the source dynamics and are an excellent tool to probe unknown astrophysics and fundamental physics. Though the updated catalog of compact binary signals reports evidence for slowly-spinning systems and unequal mass binaries, the data so far cannot provide convincing proof of strongly precessing binaries. Here, we use the gravitational-wave inference library parallel Bilby to compare the… 

Figures and Tables from this paper

Sensitivity of spin-aligned searches for neutron star-black hole systems using future detectors

Current searches for gravitational waves from compact-binary objects are primarily designed to detect the dominant gravitational-wave mode and assume that the binary components have spins which are



Parameter estimation for signals from compact binary inspirals injected into LIGO data

During the fifth science run of the Laser Interferometer Gravitational-Wave Observatory (LIGO), signals modelling the gravitational waves emitted by coalescing non-spinning compact-object binaries

Constraints on compact binary merger evolution from spin-orbit misalignment in gravitational-wave observations

The identification of the first confirmed neutron star black hole (NS-BH) binary mergers by the LIGO, Virgo and KAGRA collaboration provides the opportunity to investigate the properties of the early

Population Properties of Compact Objects from the Second LIGO–Virgo Gravitational-Wave Transient Catalog

We report on the population of 47 compact binary mergers detected with a false-alarm rate of < in the second LIGO–Virgo Gravitational-Wave Transient Catalog. We observe several characteristics of the

Gravitational-Wave Astronomy with Inspiral Signals of Spinning Compact-Object Binaries

Inspiral signals from binary compact objects (black holes and neutron stars) are primary targets of the ongoing searches by ground-based gravitational-wave interferometers (LIGO, Virgo, and GEO-600).

Mapping the Universe Expansion: Enabling Percent-level Measurements of the Hubble Constant with a Single Binary Neutron-star Merger Detection

The joint observation of the gravitational-wave (GW) and electromagnetic (EM) signal from the binary neutron-star merger GW170817 allowed for a new independent measurement of the Hubble constant H 0,

Precessional dynamics of black hole triples: binary mergers with near-zero effective spin

The binary black hole mergers detected by Advanced LIGO/Virgo have shown no evidence of large black hole spins. However, because LIGO/Virgo best measures the effective combination of the two spins

Eccentricity estimate for black hole mergers with numerical relativity simulations

The origin of black hole mergers discovered by the LIGO 1 and Virgo 2 gravitational-wave observatories is currently unknown. GW190521 3 , 4 is the heaviest black hole merger detected so far. Its

The origin of spin in binary black holes

Context. After years of scientific progress, the origin of stellar binary black holes is still a great mystery. Several formation channels for merging black holes have been proposed in the

Distinguishing spin-aligned and isotropic black hole populations with gravitational waves

The best-measured combination of spin parameters for each of the four likely binary black hole detections GW150914, LVT151012, GW151226 and GW170104 is the ‘effective’ spin, indicating that the effective spins for these systems indicate a 0.015 odds ratio against an aligned angular distribution compared to an isotropic one.

Extreme recoils: impact on the detection of gravitational waves from massive black hole binaries

Recent numerical simulations of the coalescence of highly spinning massive black hole binaries (MBHBs) suggest that the remnant can suffer a recoil velocity of the order of few thousand km s−1. We