False alarms induced by Gaussian noise in gravitational wave detectors

Gaussian noise is an irreducible component of the background in gravitational wave (GW) detectors. Although stationary Gaussian noise is uncorrelated in frequencies, we show that there is an important correlation in time when looking at the matched filter signal-to-noise ratio (SNR) of a template, w...

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Detalhes bibliográficos
Autores: Morras Gutiérrez, Gonzalo, Siles, Jose Francisco Nuño, García-Bellido Capdevila, Juan, Morales, Ester Ruiz
Tipo de documento: artigo
Data de publicação:2023
País:España
Recursos:Universidad Autónoma de Madrid
Repositório:Biblos-e Archivo. Repositorio Institucional de la UAM
Idioma:inglês
OAI Identifier:oai:repositorio.uam.es:10486/707017
Acesso em linha:http://hdl.handle.net/10486/707017
https://dx.doi.org/10.1103/PhysRevD.107.023027
Access Level:Acceso aberto
Palavra-chave:Gravitational Waves
LIGO (Observatory)
Compact
Física
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spelling False alarms induced by Gaussian noise in gravitational wave detectorsMorras Gutiérrez, GonzaloSiles, Jose Francisco NuñoGarcía-Bellido Capdevila, JuanMorales, Ester RuizGravitational WavesLIGO (Observatory)CompactFísicaGaussian noise is an irreducible component of the background in gravitational wave (GW) detectors. Although stationary Gaussian noise is uncorrelated in frequencies, we show that there is an important correlation in time when looking at the matched filter signal-to-noise ratio (SNR) of a template, with a typical autocorrelation time that depends on the template and the shape of the noise power spectral density (PSD). Taking this correlation into account, we compute from first principles the false alarm rate (FAR) of a template in Gaussian noise, defined as the number of occurrences per unit time that the template's matched filter SNR goes over a threshold ρ. We find that the Gaussian FAR can be well approximated by the usual expression for uncorrelated noise, if we replace the sampling rate by an effective sampling rate that depends on the parameters of the template, the noise PSD, and the threshold ρ. This results in a minimum SNR threshold needed for a given GW trigger, if we want to keep events generated from Gaussian noise below a certain FAR. We extend the formalism to multiple detectors and to the analysis of GW events. We apply our method to the GW candidates added in the GWTC-3 catalog and discuss the possibility that GW200308_173609 and GW200322_091133 could be generated by Gaussian noise fluctuationsAmerican Physical SocietyDepartamento de Física TeóricaFacultad de Ciencias20232023-01-31research articlehttp://purl.org/coar/resource_type/c_2df8fbb1VoRhttp://purl.org/coar/version/c_970fb48d4fbd8a85info:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10486/707017https://dx.doi.org/10.1103/PhysRevD.107.023027reponame:Biblos-e Archivo. Repositorio Institucional de la UAMinstname:Universidad Autónoma de MadridInglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:repositorio.uam.es:10486/7070172026-06-23T12:46:27Z
dc.title.none.fl_str_mv False alarms induced by Gaussian noise in gravitational wave detectors
title False alarms induced by Gaussian noise in gravitational wave detectors
spellingShingle False alarms induced by Gaussian noise in gravitational wave detectors
Morras Gutiérrez, Gonzalo
Gravitational Waves
LIGO (Observatory)
Compact
Física
title_short False alarms induced by Gaussian noise in gravitational wave detectors
title_full False alarms induced by Gaussian noise in gravitational wave detectors
title_fullStr False alarms induced by Gaussian noise in gravitational wave detectors
title_full_unstemmed False alarms induced by Gaussian noise in gravitational wave detectors
title_sort False alarms induced by Gaussian noise in gravitational wave detectors
dc.creator.none.fl_str_mv Morras Gutiérrez, Gonzalo
Siles, Jose Francisco Nuño
García-Bellido Capdevila, Juan
Morales, Ester Ruiz
author Morras Gutiérrez, Gonzalo
author_facet Morras Gutiérrez, Gonzalo
Siles, Jose Francisco Nuño
García-Bellido Capdevila, Juan
Morales, Ester Ruiz
author_role author
author2 Siles, Jose Francisco Nuño
García-Bellido Capdevila, Juan
Morales, Ester Ruiz
author2_role author
author
author
dc.contributor.none.fl_str_mv Departamento de Física Teórica
Facultad de Ciencias
dc.subject.none.fl_str_mv Gravitational Waves
LIGO (Observatory)
Compact
Física
topic Gravitational Waves
LIGO (Observatory)
Compact
Física
description Gaussian noise is an irreducible component of the background in gravitational wave (GW) detectors. Although stationary Gaussian noise is uncorrelated in frequencies, we show that there is an important correlation in time when looking at the matched filter signal-to-noise ratio (SNR) of a template, with a typical autocorrelation time that depends on the template and the shape of the noise power spectral density (PSD). Taking this correlation into account, we compute from first principles the false alarm rate (FAR) of a template in Gaussian noise, defined as the number of occurrences per unit time that the template's matched filter SNR goes over a threshold ρ. We find that the Gaussian FAR can be well approximated by the usual expression for uncorrelated noise, if we replace the sampling rate by an effective sampling rate that depends on the parameters of the template, the noise PSD, and the threshold ρ. This results in a minimum SNR threshold needed for a given GW trigger, if we want to keep events generated from Gaussian noise below a certain FAR. We extend the formalism to multiple detectors and to the analysis of GW events. We apply our method to the GW candidates added in the GWTC-3 catalog and discuss the possibility that GW200308_173609 and GW200322_091133 could be generated by Gaussian noise fluctuations
publishDate 2023
dc.date.none.fl_str_mv 2023
2023-01-31
dc.type.none.fl_str_mv research article
http://purl.org/coar/resource_type/c_2df8fbb1
VoR
http://purl.org/coar/version/c_970fb48d4fbd8a85
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv http://hdl.handle.net/10486/707017
https://dx.doi.org/10.1103/PhysRevD.107.023027
url http://hdl.handle.net/10486/707017
https://dx.doi.org/10.1103/PhysRevD.107.023027
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv American Physical Society
publisher.none.fl_str_mv American Physical Society
dc.source.none.fl_str_mv reponame:Biblos-e Archivo. Repositorio Institucional de la UAM
instname:Universidad Autónoma de Madrid
instname_str Universidad Autónoma de Madrid
reponame_str Biblos-e Archivo. Repositorio Institucional de la UAM
collection Biblos-e Archivo. Repositorio Institucional de la UAM
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15.300719

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