Stochastic gravitational wave background from stellar origin binary black holes in LISA

We use the latest constraints on the population of stellar origin binary black holes (SOBBH) from LIGO/Virgo/KAGRA (LVK) observations, to estimate the stochastic gravitational wave background (SGWB) they generate in the frequency band of LISA. In order to account for the faint and distant binaries,...

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Autores: Babak, S., Caprini, Chiara, Figueroa, Daniel G., Karnesis, Nikolaos, Marcoccia, Paolo, Nardini, Germano, Pieroni, Mauro, Ricciardone, Angelo, Sesana, Alberto, Torrado, Jesús
Tipo de documento: artigo
Estado:Versão publicada
Data de publicação:2023
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositório:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/363332
Acesso em linha:http://hdl.handle.net/10261/363332
Access Level:Acceso aberto
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spelling Stochastic gravitational wave background from stellar origin binary black holes in LISABabak, S.Caprini, ChiaraFigueroa, Daniel G.Karnesis, NikolaosMarcoccia, PaoloNardini, GermanoPieroni, MauroRicciardone, AngeloSesana, AlbertoTorrado, JesúsWe use the latest constraints on the population of stellar origin binary black holes (SOBBH) from LIGO/Virgo/KAGRA (LVK) observations, to estimate the stochastic gravitational wave background (SGWB) they generate in the frequency band of LISA. In order to account for the faint and distant binaries, which contribute the most to the SGWB, we extend the merger rate at high redshift assuming that it tracks the star formation rate. We adopt different methods to compute the SGWB signal: we perform an analytical evaluation, we use Monte Carlo sums over the SOBBH population realisations, and we account for the role of the detector by simulating LISA data and iteratively removing the resolvable signals until only the confusion noise is left. The last method allows the extraction of both the expected SGWB and the number of resolvable SOBBHs. Since the latter are few for signal-to-noise ratio thresholds larger than five, we confirm that the spectral shape of the SGWB in the LISA band agrees with the analytical prediction of a single power law. We infer the probability distribution of the SGWB amplitude from the LVK GWTC-3 posterior of the binary population model: at the reference frequency of 0.003 Hz it has an interquartile range of hΩ(f = 3 × 10 Hz) ∈ [5.65, 11.5] × 10, in agreement with most previous estimates. We then perform a MC analysis to assess LISA's capability to detect and characterise this signal. Accounting for both the instrumental noise and the galactic binaries foreground, with four years of data, LISA will be able to detect the SOBBH SGWB with percent accuracy, narrowing down the uncertainty on the amplitude by one order of magnitude with respect to the range of possible amplitudes inferred from the population model. A measurement of this signal by LISA will help to break the degeneracy among some of the population parameters, and provide interesting constraints, in particular on the redshift evolution of the SOBBH merger rate.Peer reviewedInstitute of Physics PublishingEuropean CommissionMinisterio de Ciencia e Innovación (España)Generalitat ValencianaAgencia Estatal de Investigación (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2024202420232024info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/363332reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/818691info:eu-repo/grantAgreement/AEI//RYC-2017-23493info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-113644GB-I00http://dx.doi.org/10.1088/1475-7516/2023/08/034Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3633322026-05-22T06:33:51Z
dc.title.none.fl_str_mv Stochastic gravitational wave background from stellar origin binary black holes in LISA
title Stochastic gravitational wave background from stellar origin binary black holes in LISA
spellingShingle Stochastic gravitational wave background from stellar origin binary black holes in LISA
Babak, S.
title_short Stochastic gravitational wave background from stellar origin binary black holes in LISA
title_full Stochastic gravitational wave background from stellar origin binary black holes in LISA
title_fullStr Stochastic gravitational wave background from stellar origin binary black holes in LISA
title_full_unstemmed Stochastic gravitational wave background from stellar origin binary black holes in LISA
title_sort Stochastic gravitational wave background from stellar origin binary black holes in LISA
dc.creator.none.fl_str_mv Babak, S.
Caprini, Chiara
Figueroa, Daniel G.
Karnesis, Nikolaos
Marcoccia, Paolo
Nardini, Germano
Pieroni, Mauro
Ricciardone, Angelo
Sesana, Alberto
Torrado, Jesús
author Babak, S.
author_facet Babak, S.
Caprini, Chiara
Figueroa, Daniel G.
Karnesis, Nikolaos
Marcoccia, Paolo
Nardini, Germano
Pieroni, Mauro
Ricciardone, Angelo
Sesana, Alberto
Torrado, Jesús
author_role author
author2 Caprini, Chiara
Figueroa, Daniel G.
Karnesis, Nikolaos
Marcoccia, Paolo
Nardini, Germano
Pieroni, Mauro
Ricciardone, Angelo
Sesana, Alberto
Torrado, Jesús
author2_role author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv European Commission
Ministerio de Ciencia e Innovación (España)
Generalitat Valenciana
Agencia Estatal de Investigación (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
description We use the latest constraints on the population of stellar origin binary black holes (SOBBH) from LIGO/Virgo/KAGRA (LVK) observations, to estimate the stochastic gravitational wave background (SGWB) they generate in the frequency band of LISA. In order to account for the faint and distant binaries, which contribute the most to the SGWB, we extend the merger rate at high redshift assuming that it tracks the star formation rate. We adopt different methods to compute the SGWB signal: we perform an analytical evaluation, we use Monte Carlo sums over the SOBBH population realisations, and we account for the role of the detector by simulating LISA data and iteratively removing the resolvable signals until only the confusion noise is left. The last method allows the extraction of both the expected SGWB and the number of resolvable SOBBHs. Since the latter are few for signal-to-noise ratio thresholds larger than five, we confirm that the spectral shape of the SGWB in the LISA band agrees with the analytical prediction of a single power law. We infer the probability distribution of the SGWB amplitude from the LVK GWTC-3 posterior of the binary population model: at the reference frequency of 0.003 Hz it has an interquartile range of hΩ(f = 3 × 10 Hz) ∈ [5.65, 11.5] × 10, in agreement with most previous estimates. We then perform a MC analysis to assess LISA's capability to detect and characterise this signal. Accounting for both the instrumental noise and the galactic binaries foreground, with four years of data, LISA will be able to detect the SOBBH SGWB with percent accuracy, narrowing down the uncertainty on the amplitude by one order of magnitude with respect to the range of possible amplitudes inferred from the population model. A measurement of this signal by LISA will help to break the degeneracy among some of the population parameters, and provide interesting constraints, in particular on the redshift evolution of the SOBBH merger rate.
publishDate 2023
dc.date.none.fl_str_mv 2023
2024
2024
2024
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/10261/363332
url http://hdl.handle.net/10261/363332
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/EC/H2020/818691
info:eu-repo/grantAgreement/AEI//RYC-2017-23493
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-113644GB-I00
http://dx.doi.org/10.1088/1475-7516/2023/08/034
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Institute of Physics Publishing
publisher.none.fl_str_mv Institute of Physics Publishing
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
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