FBQ 0951+2635: time delay and structure of the main lensing galaxy

As there is a long-standing controversy over the time delay between the two images of the gravitationally lensed quasar FBQ 0951+2635, we combined early and new optical light curves to robustly measure a delay of 13.5 ± 1.6 d (1σ interval). The new optical records covering the last 17 yr were also u...

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Autores: Shalyapin, Vyacheslav N., Goicoechea Santamaría, Luis Julián|||0000-0003-0110-834X, Ruiz-Hinojosa, Eleana
Tipo de recurso: artículo
Fecha de publicación:2025
País:España
Institución:Universidad de Cantabria (UC)
Repositorio:UCrea Repositorio Abierto de la Universidad de Cantabria
Idioma:inglés
OAI Identifier:oai:repositorio.unican.es:10902/35523
Acceso en línea:https://hdl.handle.net/10902/35523
Access Level:acceso abierto
Palabra clave:Gravitational lensing: strong
Galaxies: structure
Quasars: individual: FBQ 0951+2635
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spelling FBQ 0951+2635: time delay and structure of the main lensing galaxyShalyapin, Vyacheslav N.Goicoechea Santamaría, Luis Julián|||0000-0003-0110-834XRuiz-Hinojosa, EleanaGravitational lensing: strongGalaxies: structureQuasars: individual: FBQ 0951+2635As there is a long-standing controversy over the time delay between the two images of the gravitationally lensed quasar FBQ 0951+2635, we combined early and new optical light curves to robustly measure a delay of 13.5 ± 1.6 d (1σ interval). The new optical records covering the last 17 yr were also used to trace the long-timescale evolution of the microlensing variability. Additionally, the new time-delay interval and a relatively rich set of further observational constraints allowed us to discuss the mass structure of the main lensing galaxy at a redshift of 0.26. This lens system is of particular interest because the external shear from secondary gravitational deflectors is relatively low, but the external convergence is one of the highest known. When modelling the galaxy as a singular power-law ellipsoid without hypotheses or priors on the power-law index, ellipticity, and position angle, we demonstrated that its mass profile is close to isothermal, and there is a good agreement between the shape of the mass distribution and that of the near-IR light.We also recovered the true mass scale of the galaxy. Finally, a constant mass-to-light ratio model also worked acceptably well.VNS acknowledges the Universidad de Cantabria (UC) and the Spanish Agencia Estatal de Investigación (AEI) for financial support for a long stay at the UC in the period 2022–2024. This research has been supported by the grant PID2020-118990GB-I00 funded by MCIN/AEI/10.13039/501100011033.EDP SciencesUniversidad de Cantabria20252025-02-01journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articlehttps://hdl.handle.net/10902/35523Astronomy & Astrophysics, 2024, 694, A31reponame:UCrea Repositorio Abierto de la Universidad de Cantabriainstname:Universidad de Cantabria (UC)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Attribution 4.0 Internationalhttp://creativecommons.org/licenses/by/4.0/info:eu-repo/semantics/openAccessoai:repositorio.unican.es:10902/355232026-06-02T12:39:31Z
dc.title.none.fl_str_mv FBQ 0951+2635: time delay and structure of the main lensing galaxy
title FBQ 0951+2635: time delay and structure of the main lensing galaxy
spellingShingle FBQ 0951+2635: time delay and structure of the main lensing galaxy
Shalyapin, Vyacheslav N.
Gravitational lensing: strong
Galaxies: structure
Quasars: individual: FBQ 0951+2635
title_short FBQ 0951+2635: time delay and structure of the main lensing galaxy
title_full FBQ 0951+2635: time delay and structure of the main lensing galaxy
title_fullStr FBQ 0951+2635: time delay and structure of the main lensing galaxy
title_full_unstemmed FBQ 0951+2635: time delay and structure of the main lensing galaxy
title_sort FBQ 0951+2635: time delay and structure of the main lensing galaxy
dc.creator.none.fl_str_mv Shalyapin, Vyacheslav N.
Goicoechea Santamaría, Luis Julián|||0000-0003-0110-834X
Ruiz-Hinojosa, Eleana
author Shalyapin, Vyacheslav N.
author_facet Shalyapin, Vyacheslav N.
Goicoechea Santamaría, Luis Julián|||0000-0003-0110-834X
Ruiz-Hinojosa, Eleana
author_role author
author2 Goicoechea Santamaría, Luis Julián|||0000-0003-0110-834X
Ruiz-Hinojosa, Eleana
author2_role author
author
dc.contributor.none.fl_str_mv Universidad de Cantabria
dc.subject.none.fl_str_mv Gravitational lensing: strong
Galaxies: structure
Quasars: individual: FBQ 0951+2635
topic Gravitational lensing: strong
Galaxies: structure
Quasars: individual: FBQ 0951+2635
description As there is a long-standing controversy over the time delay between the two images of the gravitationally lensed quasar FBQ 0951+2635, we combined early and new optical light curves to robustly measure a delay of 13.5 ± 1.6 d (1σ interval). The new optical records covering the last 17 yr were also used to trace the long-timescale evolution of the microlensing variability. Additionally, the new time-delay interval and a relatively rich set of further observational constraints allowed us to discuss the mass structure of the main lensing galaxy at a redshift of 0.26. This lens system is of particular interest because the external shear from secondary gravitational deflectors is relatively low, but the external convergence is one of the highest known. When modelling the galaxy as a singular power-law ellipsoid without hypotheses or priors on the power-law index, ellipticity, and position angle, we demonstrated that its mass profile is close to isothermal, and there is a good agreement between the shape of the mass distribution and that of the near-IR light.We also recovered the true mass scale of the galaxy. Finally, a constant mass-to-light ratio model also worked acceptably well.
publishDate 2025
dc.date.none.fl_str_mv 2025
2025-02-01
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
NA
http://purl.org/coar/version/c_be7fb7dd8ff6fe43
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/10902/35523
url https://hdl.handle.net/10902/35523
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
Attribution 4.0 International
http://creativecommons.org/licenses/by/4.0/
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
Attribution 4.0 International
http://creativecommons.org/licenses/by/4.0/
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv Astronomy & Astrophysics, 2024, 694, A31
reponame:UCrea Repositorio Abierto de la Universidad de Cantabria
instname:Universidad de Cantabria (UC)
instname_str Universidad de Cantabria (UC)
reponame_str UCrea Repositorio Abierto de la Universidad de Cantabria
collection UCrea Repositorio Abierto de la Universidad de Cantabria
repository.name.fl_str_mv
repository.mail.fl_str_mv
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