Theoretical groundwork supporting the precessing-spin two-body dynamics of the effective-one-body waveform models SEOBNRv5

Khalil, Mohammed; Buonanno, Alessandra; Estellés, Héctor; Mihaylov, Deyan P.; Ossokine, Serguei; Pompili, Lorenzo; Ramos-Buades, Antoni

doi:10.1103/physrevd.108.124036

Cited by 14 publications

(1 citation statement)

References 240 publications

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“…Systematic errors in inferred source properties due to waveform modeling may be significant for NSBH systems (Huang et al 2021). We mitigate these effects by combining the posteriors inferred using two different signal models: the phenomenological frequency-domain model IMRPhenomXPHM (García-Quirós et al 2020;Pratten et al 2020Pratten et al , 2021, and a timedomain effective-one-body (EOB) model SEOBNRv5PHM (Khalil et al 2023;Pompili et al 2023;Ramos-Buades et al 2023;van de Meent et al 2023). The posterior samples obtained independently using the two signal models are broadly consistent.…”

Section: Source Propertiesmentioning

confidence: 99%

Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M _⊙ Compact Object and a Neutron Star

Abac,

Abbott,

Abouelfettouh

et al. 2024

ApJL

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We report the observation of a coalescing compact binary with component masses 2.5–4.5 M ⊙ and 1.2–2.0 M ⊙ (all measurements quoted at the 90% credible level). The gravitational-wave signal GW230529_181500 was observed during the fourth observing run of the LIGO–Virgo–KAGRA detector network on 2023 May 29 by the LIGO Livingston observatory. The primary component of the source has a mass less than 5 M ⊙ at 99% credibility. We cannot definitively determine from gravitational-wave data alone whether either component of the source is a neutron star or a black hole. However, given existing estimates of the maximum neutron star mass, we find the most probable interpretation of the source to be the coalescence of a neutron star with a black hole that has a mass between the most massive neutron stars and the least massive black holes observed in the Galaxy. We provisionally estimate a merger rate density of 55 − 47 + 127 Gpc − 3 yr − 1 for compact binary coalescences with properties similar to the source of GW230529_181500; assuming that the source is a neutron star–black hole merger, GW230529_181500-like sources may make up the majority of neutron star–black hole coalescences. The discovery of this system implies an increase in the expected rate of neutron star–black hole mergers with electromagnetic counterparts and provides further evidence for compact objects existing within the purported lower mass gap.

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Section: Source Propertiesmentioning

confidence: 99%

Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M _⊙ Compact Object and a Neutron Star

Abac,

Abbott,

Abouelfettouh

et al. 2024

ApJL

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Massive twistor worldline in electromagnetic fields

Kim,

Lee

2024

J. High Energ. Phys.

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We study the (ambi-)twistor model for spinning particles interacting via electromagnetic field, as a toy model for studying classical dynamics of gravitating bodies including effects of both spins to all orders. We compute the momentum kick and spin kick up to one-loop order and show precisely how they are encoded in the classical eikonal. The all-orders-in-spin effects are encoded as a dynamical implementation of the Newman-Janis shift, and we find that the expansion in both spins can be resummed to simple expressions in special kinematic configurations, at least up to one-loop order. We confirm that the classical eikonal can be understood as the generator of canonical transformations that map the in-states of a scattering process to the out-states. We also remark that cut contributions for converting worldline propagators from time-symmetric to retarded amount to the iterated action of the leading eikonal at one-loop order.

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Laying the foundation of the effective-one-body waveform models SEOBNRv5: Improved accuracy and efficiency for spinning nonprecessing binary black holes

Pompili,

Buonanno,

Estellés

et al. 2023

Phys. Rev. D

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Theoretical groundwork supporting the precessing-spin two-body dynamics of the effective-one-body waveform models SEOBNRv5

Cited by 14 publications

References 240 publications

Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M _⊙ Compact Object and a Neutron Star

Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M _⊙ Compact Object and a Neutron Star

Massive twistor worldline in electromagnetic fields

Laying the foundation of the effective-one-body waveform models SEOBNRv5: Improved accuracy and efficiency for spinning nonprecessing binary black holes

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Theoretical groundwork supporting the precessing-spin two-body dynamics of the effective-one-body waveform models SEOBNRv5

Cited by 14 publications

References 240 publications

Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M ⊙ Compact Object and a Neutron Star

Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M ⊙ Compact Object and a Neutron Star

Massive twistor worldline in electromagnetic fields

Laying the foundation of the effective-one-body waveform models SEOBNRv5: Improved accuracy and efficiency for spinning nonprecessing binary black holes

Contact Info

Product

Resources

About

Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M _⊙ Compact Object and a Neutron Star

Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M _⊙ Compact Object and a Neutron Star