Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2
Black hole binaries formed dynamically in globular clusters are believed to be one of the main sources of gravitational waves in the Universe. Here, we use our new population synthesis code, cbhbd, to determine the redshift evolution of the merger rate density and masses of black hole binaries forme...
| Autores: | , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2020 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/237072 |
| Acceso en línea: | http://hdl.handle.net/10261/237072 |
| Access Level: | acceso abierto |
| id |
ES_cd81dc0c698a7096bbcd480668e2f799 |
|---|---|
| oai_identifier_str |
oai:digital.csic.es:10261/237072 |
| network_acronym_str |
ES |
| network_name_str |
España |
| repository_id_str |
|
| spelling |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2Antonini, FabioGieles, MarkBlack hole binaries formed dynamically in globular clusters are believed to be one of the main sources of gravitational waves in the Universe. Here, we use our new population synthesis code, cbhbd, to determine the redshift evolution of the merger rate density and masses of black hole binaries formed in globular clusters. We simulate ∼2million models to explore the parameter space that is relevant to real globular clusters and overall mass scales. We show that when uncertainties on the initial cluster mass function and their initial half-mass density are properly taken into account, they become the two dominant factors in setting the theoretical error bars on merger rates. Uncertainties in other model parameters (e.g., natal kicks, black hole masses, and metallicity) have virtually no effect on the local merger rate density, although they affect the masses of the merging black holes. Modeling the merger rate density as a function of redshift as R(z)=R0(1+z)κ at z<2, and marginalizing over uncertainties, we find: R0=7.2+21.5−5.5Gpc−3 yr−1 and κ=1.6+0.4−0.6 (90% credibility). The rate parameters for binaries that merge inside the clusters are R0,in=1.6+1.9−1.0 Gpc−3yr−1 and κ in=2.3+1.3−1.0; ∼20% of these form as the result of a gravitational-wave capture, implying that eccentric mergers from globular clusters contribute ≲0.4Gpc−3 yr−1 to the local rate. A comparison to the merger rate reported by Laser Interferometer Gravitational Wave Observatory-Virgo shows that a scenario in which most of the detected black hole mergers are formed in globular clusters is consistent with current constraints and requires initial cluster half-mass densities ≳104M⊙pc-3. Interestingly, these models also reproduce the inferred black hole mass function in the range 13–30M⊙. However, all models underpredict the data outside this range, suggesting that other mechanisms might be responsible for the formation of these sources.F. A. acknowledges support from a Rutherford Fellowship (ST/P00492X/1) from the Science and Technology Facilities Council. We acknowledge the support of the Supercomputing Wales project, which is partly funded by the European Regional Development Fund (ERDF) via the Welsh government.Peer reviewedAmerican Physical SocietyScience and Technology Facilities Council (UK)European CommissionWelsh GovernmentConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202120212020info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/237072reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttps://doi.org/10.1103/PhysRevD.102.123016Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2370722026-05-22T06:33:51Z |
| dc.title.none.fl_str_mv |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2 |
| title |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2 |
| spellingShingle |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2 Antonini, Fabio |
| title_short |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2 |
| title_full |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2 |
| title_fullStr |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2 |
| title_full_unstemmed |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2 |
| title_sort |
Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2 |
| dc.creator.none.fl_str_mv |
Antonini, Fabio Gieles, Mark |
| author |
Antonini, Fabio |
| author_facet |
Antonini, Fabio Gieles, Mark |
| author_role |
author |
| author2 |
Gieles, Mark |
| author2_role |
author |
| dc.contributor.none.fl_str_mv |
Science and Technology Facilities Council (UK) European Commission Welsh Government Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| description |
Black hole binaries formed dynamically in globular clusters are believed to be one of the main sources of gravitational waves in the Universe. Here, we use our new population synthesis code, cbhbd, to determine the redshift evolution of the merger rate density and masses of black hole binaries formed in globular clusters. We simulate ∼2million models to explore the parameter space that is relevant to real globular clusters and overall mass scales. We show that when uncertainties on the initial cluster mass function and their initial half-mass density are properly taken into account, they become the two dominant factors in setting the theoretical error bars on merger rates. Uncertainties in other model parameters (e.g., natal kicks, black hole masses, and metallicity) have virtually no effect on the local merger rate density, although they affect the masses of the merging black holes. Modeling the merger rate density as a function of redshift as R(z)=R0(1+z)κ at z<2, and marginalizing over uncertainties, we find: R0=7.2+21.5−5.5Gpc−3 yr−1 and κ=1.6+0.4−0.6 (90% credibility). The rate parameters for binaries that merge inside the clusters are R0,in=1.6+1.9−1.0 Gpc−3yr−1 and κ in=2.3+1.3−1.0; ∼20% of these form as the result of a gravitational-wave capture, implying that eccentric mergers from globular clusters contribute ≲0.4Gpc−3 yr−1 to the local rate. A comparison to the merger rate reported by Laser Interferometer Gravitational Wave Observatory-Virgo shows that a scenario in which most of the detected black hole mergers are formed in globular clusters is consistent with current constraints and requires initial cluster half-mass densities ≳104M⊙pc-3. Interestingly, these models also reproduce the inferred black hole mass function in the range 13–30M⊙. However, all models underpredict the data outside this range, suggesting that other mechanisms might be responsible for the formation of these sources. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020 2021 2021 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
| format |
article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/10261/237072 |
| url |
http://hdl.handle.net/10261/237072 |
| dc.language.none.fl_str_mv |
Inglés |
| language_invalid_str_mv |
Inglés |
| dc.relation.none.fl_str_mv |
https://doi.org/10.1103/PhysRevD.102.123016 Sí |
| dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess |
| eu_rights_str_mv |
openAccess |
| dc.publisher.none.fl_str_mv |
American Physical Society |
| publisher.none.fl_str_mv |
American Physical Society |
| dc.source.none.fl_str_mv |
reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC instname:Consejo Superior de Investigaciones Científicas (CSIC) |
| instname_str |
Consejo Superior de Investigaciones Científicas (CSIC) |
| reponame_str |
DIGITAL.CSIC. Repositorio Institucional del CSIC |
| collection |
DIGITAL.CSIC. Repositorio Institucional del CSIC |
| repository.name.fl_str_mv |
|
| repository.mail.fl_str_mv |
|
| _version_ |
1869419861027848192 |
| score |
15.812455 |