Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613

Autores
Brigitte, Maïmouna; Castro Segura, Noel; García, Federico; Svoboda, Jirí; Díaz Trigo, María; Méndez, Mariano; Vincentelli, Federico M.; Buisson, Douglas J. K.; Altamirano, Diego
Año de publicación
2025
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Timing analysis of accreting systems is key to probing the structure and dynamics around compact objects. In black-hole low-mass X-ray binaries (BH LMXBs), the compact object accretes matter from a low-mass companion star via Roche-Lobe overflow and forms an accretion disk that occasionally exhibits bright eruptions. The BH LMXB Swift J1727.8−1613 (hereafter J1727) underwent one of the brightest outbursts ever recorded in X-rays in August 2023. Aims. We study the timing properties of J1727 in the decaying phase of its outburst based on XMM─Newton data with a high-time resolution. Methods. We analyzed the power spectrum (PS) and cross spectrum (CS) of J1727, which we modeled with Lorentzians. The PS reveals the power distribution of the source across frequencies, and the real and imaginary parts of the CS compare the displacement of the light curves in different energy bands for the different observations. Finally, we simultaneously derived the phase lags and the coherence using a constant phase-lag model. Results. While the first (soft-state) observation shows no strong variability, the two harder observations exhibit quasi-periodic oscillations (QPOs). Because the QPO is more significantly detected in the imaginary part of the CS than in the PS, we refer to it as the "imaginary QPO". The QPO is more prominent in the soft 0.3−2 keV band than in the hard 2−12 keV band. As the source evolves toward the hard state, the imaginary QPO shifts to lower frequencies, the broadband fractional rms amplitude in the 0.3−2 keV energy band increases, and the rms covariance of the imaginary QPO decreases. Simultaneously, the phase lags increase, and the coherence function drops at the imaginary QPO frequency. Conclusions. This analysis provides the first type-C QPO detection in a BH XB during the soft─to─hard transition using XMM─Newton data. The QPO is detected at particularly low energy (0.3−2 keV). Notably, the QPO is significantly detected in the imaginary part of the CS and the PS. Thus, we confirm the physical origin of the coherence drop and the phase-lag excess, which were only observed with NICER before.
Fil: Brigitte, Maïmouna. Czech Academy Of Sciences.; República Checa
Fil: Castro Segura, Noel. University of Warwick; Reino Unido
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Svoboda, Jirí. Czech Academy of Sciences; República Checa
Fil: Díaz Trigo, María. European Southern Observatory (eso); Alemania
Fil: Méndez, Mariano. Kapteyn Astronomical Institute; Países Bajos
Fil: Vincentelli, Federico M.. Istituto Nazionale di Astrofisica; Italia
Fil: Buisson, Douglas J. K.. University of Southampton; Reino Unido
Fil: Altamirano, Diego. University of Southampton; Reino Unido
Materia
X-RAY: BINARIES
STARS: BLACK HOLES
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/289761
Acceder
id CONICETDig_fa87350cddbf6812477a80da3d3a837b
oai_identifier_str oai:ri.conicet.gov.ar:11336/289761
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613Brigitte, MaïmounaCastro Segura, NoelGarcía, FedericoSvoboda, JiríDíaz Trigo, MaríaMéndez, MarianoVincentelli, Federico M.Buisson, Douglas J. K.Altamirano, DiegoX-RAY: BINARIESSTARS: BLACK HOLEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Timing analysis of accreting systems is key to probing the structure and dynamics around compact objects. In black-hole low-mass X-ray binaries (BH LMXBs), the compact object accretes matter from a low-mass companion star via Roche-Lobe overflow and forms an accretion disk that occasionally exhibits bright eruptions. The BH LMXB Swift J1727.8−1613 (hereafter J1727) underwent one of the brightest outbursts ever recorded in X-rays in August 2023. Aims. We study the timing properties of J1727 in the decaying phase of its outburst based on XMM─Newton data with a high-time resolution. Methods. We analyzed the power spectrum (PS) and cross spectrum (CS) of J1727, which we modeled with Lorentzians. The PS reveals the power distribution of the source across frequencies, and the real and imaginary parts of the CS compare the displacement of the light curves in different energy bands for the different observations. Finally, we simultaneously derived the phase lags and the coherence using a constant phase-lag model. Results. While the first (soft-state) observation shows no strong variability, the two harder observations exhibit quasi-periodic oscillations (QPOs). Because the QPO is more significantly detected in the imaginary part of the CS than in the PS, we refer to it as the "imaginary QPO". The QPO is more prominent in the soft 0.3−2 keV band than in the hard 2−12 keV band. As the source evolves toward the hard state, the imaginary QPO shifts to lower frequencies, the broadband fractional rms amplitude in the 0.3−2 keV energy band increases, and the rms covariance of the imaginary QPO decreases. Simultaneously, the phase lags increase, and the coherence function drops at the imaginary QPO frequency. Conclusions. This analysis provides the first type-C QPO detection in a BH XB during the soft─to─hard transition using XMM─Newton data. The QPO is detected at particularly low energy (0.3−2 keV). Notably, the QPO is significantly detected in the imaginary part of the CS and the PS. Thus, we confirm the physical origin of the coherence drop and the phase-lag excess, which were only observed with NICER before.Fil: Brigitte, Maïmouna. Czech Academy Of Sciences.; República ChecaFil: Castro Segura, Noel. University of Warwick; Reino UnidoFil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Svoboda, Jirí. Czech Academy of Sciences; República ChecaFil: Díaz Trigo, María. European Southern Observatory (eso); AlemaniaFil: Méndez, Mariano. Kapteyn Astronomical Institute; Países BajosFil: Vincentelli, Federico M.. Istituto Nazionale di Astrofisica; ItaliaFil: Buisson, Douglas J. K.. University of Southampton; Reino UnidoFil: Altamirano, Diego. University of Southampton; Reino UnidoEDP Sciences2025-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/289761Brigitte, Maïmouna; Castro Segura, Noel; García, Federico; Svoboda, Jirí; Díaz Trigo, María; et al.; Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613; EDP Sciences; Astronomy and Astrophysics; 703; 11-2025; 1-90004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202555486info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202555486info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-08-25T14:33:33Zoai:ri.conicet.gov.ar:11336/289761instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982026-08-25 14:33:34.126CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613
title Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613
spellingShingle Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613
Brigitte, Maïmouna
X-RAY: BINARIES
STARS: BLACK HOLES
title_short Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613
title_full Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613
title_fullStr Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613
title_full_unstemmed Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613
title_sort Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613
dc.creator.none.fl_str_mv Brigitte, Maïmouna
Castro Segura, Noel
García, Federico
Svoboda, Jirí
Díaz Trigo, María
Méndez, Mariano
Vincentelli, Federico M.
Buisson, Douglas J. K.
Altamirano, Diego
author Brigitte, Maïmouna
author_facet Brigitte, Maïmouna
Castro Segura, Noel
García, Federico
Svoboda, Jirí
Díaz Trigo, María
Méndez, Mariano
Vincentelli, Federico M.
Buisson, Douglas J. K.
Altamirano, Diego
author_role author
author2 Castro Segura, Noel
García, Federico
Svoboda, Jirí
Díaz Trigo, María
Méndez, Mariano
Vincentelli, Federico M.
Buisson, Douglas J. K.
Altamirano, Diego
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv X-RAY: BINARIES
STARS: BLACK HOLES
topic X-RAY: BINARIES
STARS: BLACK HOLES
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. Timing analysis of accreting systems is key to probing the structure and dynamics around compact objects. In black-hole low-mass X-ray binaries (BH LMXBs), the compact object accretes matter from a low-mass companion star via Roche-Lobe overflow and forms an accretion disk that occasionally exhibits bright eruptions. The BH LMXB Swift J1727.8−1613 (hereafter J1727) underwent one of the brightest outbursts ever recorded in X-rays in August 2023. Aims. We study the timing properties of J1727 in the decaying phase of its outburst based on XMM─Newton data with a high-time resolution. Methods. We analyzed the power spectrum (PS) and cross spectrum (CS) of J1727, which we modeled with Lorentzians. The PS reveals the power distribution of the source across frequencies, and the real and imaginary parts of the CS compare the displacement of the light curves in different energy bands for the different observations. Finally, we simultaneously derived the phase lags and the coherence using a constant phase-lag model. Results. While the first (soft-state) observation shows no strong variability, the two harder observations exhibit quasi-periodic oscillations (QPOs). Because the QPO is more significantly detected in the imaginary part of the CS than in the PS, we refer to it as the "imaginary QPO". The QPO is more prominent in the soft 0.3−2 keV band than in the hard 2−12 keV band. As the source evolves toward the hard state, the imaginary QPO shifts to lower frequencies, the broadband fractional rms amplitude in the 0.3−2 keV energy band increases, and the rms covariance of the imaginary QPO decreases. Simultaneously, the phase lags increase, and the coherence function drops at the imaginary QPO frequency. Conclusions. This analysis provides the first type-C QPO detection in a BH XB during the soft─to─hard transition using XMM─Newton data. The QPO is detected at particularly low energy (0.3−2 keV). Notably, the QPO is significantly detected in the imaginary part of the CS and the PS. Thus, we confirm the physical origin of the coherence drop and the phase-lag excess, which were only observed with NICER before.
Fil: Brigitte, Maïmouna. Czech Academy Of Sciences.; República Checa
Fil: Castro Segura, Noel. University of Warwick; Reino Unido
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Svoboda, Jirí. Czech Academy of Sciences; República Checa
Fil: Díaz Trigo, María. European Southern Observatory (eso); Alemania
Fil: Méndez, Mariano. Kapteyn Astronomical Institute; Países Bajos
Fil: Vincentelli, Federico M.. Istituto Nazionale di Astrofisica; Italia
Fil: Buisson, Douglas J. K.. University of Southampton; Reino Unido
Fil: Altamirano, Diego. University of Southampton; Reino Unido
description Context. Timing analysis of accreting systems is key to probing the structure and dynamics around compact objects. In black-hole low-mass X-ray binaries (BH LMXBs), the compact object accretes matter from a low-mass companion star via Roche-Lobe overflow and forms an accretion disk that occasionally exhibits bright eruptions. The BH LMXB Swift J1727.8−1613 (hereafter J1727) underwent one of the brightest outbursts ever recorded in X-rays in August 2023. Aims. We study the timing properties of J1727 in the decaying phase of its outburst based on XMM─Newton data with a high-time resolution. Methods. We analyzed the power spectrum (PS) and cross spectrum (CS) of J1727, which we modeled with Lorentzians. The PS reveals the power distribution of the source across frequencies, and the real and imaginary parts of the CS compare the displacement of the light curves in different energy bands for the different observations. Finally, we simultaneously derived the phase lags and the coherence using a constant phase-lag model. Results. While the first (soft-state) observation shows no strong variability, the two harder observations exhibit quasi-periodic oscillations (QPOs). Because the QPO is more significantly detected in the imaginary part of the CS than in the PS, we refer to it as the "imaginary QPO". The QPO is more prominent in the soft 0.3−2 keV band than in the hard 2−12 keV band. As the source evolves toward the hard state, the imaginary QPO shifts to lower frequencies, the broadband fractional rms amplitude in the 0.3−2 keV energy band increases, and the rms covariance of the imaginary QPO decreases. Simultaneously, the phase lags increase, and the coherence function drops at the imaginary QPO frequency. Conclusions. This analysis provides the first type-C QPO detection in a BH XB during the soft─to─hard transition using XMM─Newton data. The QPO is detected at particularly low energy (0.3−2 keV). Notably, the QPO is significantly detected in the imaginary part of the CS and the PS. Thus, we confirm the physical origin of the coherence drop and the phase-lag excess, which were only observed with NICER before.
publishDate 2025
dc.date.none.fl_str_mv 2025-11
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/289761
Brigitte, Maïmouna; Castro Segura, Noel; García, Federico; Svoboda, Jirí; Díaz Trigo, María; et al.; Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613; EDP Sciences; Astronomy and Astrophysics; 703; 11-2025; 1-9
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/289761
identifier_str_mv Brigitte, Maïmouna; Castro Segura, Noel; García, Federico; Svoboda, Jirí; Díaz Trigo, María; et al.; Detection of a type-C quasi-periodic oscillation during the soft-to-hard transition in Swift J1727.8–1613; EDP Sciences; Astronomy and Astrophysics; 703; 11-2025; 1-9
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202555486
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202555486
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.365483

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