Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417

Autores
Santerne, A.; Beaulieu, J. P.; Rojas Ayala, B.; Boisse, I.; Schlawin, E.; Almenara, J.-M.; Batista, V.; Bennett, D.; Diaz, Rodrigo Fernando; Figueira, P.; James, D. J.; Herter, T.; Lillo Box, J.; Marquette, J. B.; Ranc, C.; Santos, N. C.; Sousa, S. G.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The microlensing event OGLE-2011-BLG-0417 is an exceptionally bright lens binary that was predicted to present radial velocity variation at the level of several km s-1. Pioneer radial velocity follow-up observations with the UVES spectrograph at the ESO−VLT of this system clearly ruled out the large radial velocity variation, leaving a discrepancy between the observation and the prediction. In this paper, we further characterise the microlensing system by analysing its spectral energy distribution (SED) derived using the UVES spectrum and new observations with the ARCoIRIS (CTIO) near-infrared spectrograph and the Keck adaptive optics instrument NIRC2 in the J, H, and Ks-bands. We determine the mass and distance of the stars independently from the microlensing modelling. We find that the SED is compatible with a giant star in the Galactic bulge and a foreground star with a mass of 0.94 ± 0.09 M⊙  at a distance of 1.07 ± 0.24 kpc. We find that this foreground star is likely the lens. Its parameters are not compatible with the ones previously reported in the literature (0.52 ± 0.04 M⊙ at 0.95 ± 0.06 kpc), based on the microlensing light curve. A thoughtful re-analysis of the microlensing event is mandatory to fully understand the reason of this new discrepancy. More importantly, this paper demonstrates that spectroscopic follow-up observations of microlensing events are possible and provide independent constraints on the parameters of the lens and source stars, hence breaking some degeneracies in the analysis. UV-to-NIR low-resolution spectrographs like X-shooter (ESO−VLT) could substantially contribute to this follow-up efforts, with magnitude limits above all microlensing events detected so far.
Fil: Santerne, A.. Universidade do Porto; Portugal
Fil: Beaulieu, J. P.. Université Pierre & Marie Curie; Francia
Fil: Rojas Ayala, B.. Universidad Andres Bello; Chile
Fil: Boisse, I.. Laboratoire d’Astrophysique de Marseille; Francia
Fil: Schlawin, E.. University Of Arizona; Estados Unidos
Fil: Almenara, J.-M.. Institut de Planétologie et d’Astrophysique de Grenoble; Francia
Fil: Batista, V.. Université Pierre & Marie Curie; Francia
Fil: Bennett, D.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados Unidos
Fil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Figueira, P.. Universidade do Porto; Portugal
Fil: James, D. J.. Cerro Tololo Inter-American Observatory; Chile
Fil: Herter, T.. Cornell University; Estados Unidos
Fil: Lillo Box, J.. European Southern Observatory; Chile
Fil: Marquette, J. B.. Université Pierre & Marie Curie; Francia
Fil: Ranc, C.. Université Pierre & Marie Curi; Francia
Fil: Santos, N. C.. Universidade do Porto; Portugal
Fil: Sousa, S. G.. Universidade do Porto; Portugal
Materia
techniques: spectroscopic
techniques: high angular resolution
stars: individual: OGLE-2011-BLG-0417
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:11336/18441
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/18441
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417Santerne, A.Beaulieu, J. P.Rojas Ayala, B.Boisse, I.Schlawin, E.Almenara, J.-M.Batista, V.Bennett, D.Diaz, Rodrigo FernandoFigueira, P.James, D. J.Herter, T.Lillo Box, J.Marquette, J. B.Ranc, C.Santos, N. C.Sousa, S. G.techniques: spectroscopictechniques: high angular resolutionstars: individual: OGLE-2011-BLG-0417https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The microlensing event OGLE-2011-BLG-0417 is an exceptionally bright lens binary that was predicted to present radial velocity variation at the level of several km s-1. Pioneer radial velocity follow-up observations with the UVES spectrograph at the ESO−VLT of this system clearly ruled out the large radial velocity variation, leaving a discrepancy between the observation and the prediction. In this paper, we further characterise the microlensing system by analysing its spectral energy distribution (SED) derived using the UVES spectrum and new observations with the ARCoIRIS (CTIO) near-infrared spectrograph and the Keck adaptive optics instrument NIRC2 in the J, H, and Ks-bands. We determine the mass and distance of the stars independently from the microlensing modelling. We find that the SED is compatible with a giant star in the Galactic bulge and a foreground star with a mass of 0.94 ± 0.09 M⊙  at a distance of 1.07 ± 0.24 kpc. We find that this foreground star is likely the lens. Its parameters are not compatible with the ones previously reported in the literature (0.52 ± 0.04 M⊙ at 0.95 ± 0.06 kpc), based on the microlensing light curve. A thoughtful re-analysis of the microlensing event is mandatory to fully understand the reason of this new discrepancy. More importantly, this paper demonstrates that spectroscopic follow-up observations of microlensing events are possible and provide independent constraints on the parameters of the lens and source stars, hence breaking some degeneracies in the analysis. UV-to-NIR low-resolution spectrographs like X-shooter (ESO−VLT) could substantially contribute to this follow-up efforts, with magnitude limits above all microlensing events detected so far.Fil: Santerne, A.. Universidade do Porto; PortugalFil: Beaulieu, J. P.. Université Pierre & Marie Curie; FranciaFil: Rojas Ayala, B.. Universidad Andres Bello; ChileFil: Boisse, I.. Laboratoire d’Astrophysique de Marseille; FranciaFil: Schlawin, E.. University Of Arizona; Estados UnidosFil: Almenara, J.-M.. Institut de Planétologie et d’Astrophysique de Grenoble; FranciaFil: Batista, V.. Université Pierre & Marie Curie; FranciaFil: Bennett, D.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados UnidosFil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Figueira, P.. Universidade do Porto; PortugalFil: James, D. J.. Cerro Tololo Inter-American Observatory; ChileFil: Herter, T.. Cornell University; Estados UnidosFil: Lillo Box, J.. European Southern Observatory; ChileFil: Marquette, J. B.. Université Pierre & Marie Curie; FranciaFil: Ranc, C.. Université Pierre & Marie Curi; FranciaFil: Santos, N. C.. Universidade do Porto; PortugalFil: Sousa, S. G.. Universidade do Porto; PortugalEdp Sciences2016-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/18441Santerne, A.; Beaulieu, J. P.; Rojas Ayala, B.; Boisse, I.; Schlawin, E.; et al.; Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417; Edp Sciences; Astronomy And Astrophysics; 595; L11; 11-2016; 1-80004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527710info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1610.04446info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/11/aa27710-15/aa27710-15.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:37:23Zoai:ri.conicet.gov.ar:11336/18441instacron: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:34982025-10-22 11:37:23.415CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417
title Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417
spellingShingle Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417
Santerne, A.
techniques: spectroscopic
techniques: high angular resolution
stars: individual: OGLE-2011-BLG-0417
title_short Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417
title_full Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417
title_fullStr Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417
title_full_unstemmed Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417
title_sort Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417
dc.creator.none.fl_str_mv Santerne, A.
Beaulieu, J. P.
Rojas Ayala, B.
Boisse, I.
Schlawin, E.
Almenara, J.-M.
Batista, V.
Bennett, D.
Diaz, Rodrigo Fernando
Figueira, P.
James, D. J.
Herter, T.
Lillo Box, J.
Marquette, J. B.
Ranc, C.
Santos, N. C.
Sousa, S. G.
author Santerne, A.
author_facet Santerne, A.
Beaulieu, J. P.
Rojas Ayala, B.
Boisse, I.
Schlawin, E.
Almenara, J.-M.
Batista, V.
Bennett, D.
Diaz, Rodrigo Fernando
Figueira, P.
James, D. J.
Herter, T.
Lillo Box, J.
Marquette, J. B.
Ranc, C.
Santos, N. C.
Sousa, S. G.
author_role author
author2 Beaulieu, J. P.
Rojas Ayala, B.
Boisse, I.
Schlawin, E.
Almenara, J.-M.
Batista, V.
Bennett, D.
Diaz, Rodrigo Fernando
Figueira, P.
James, D. J.
Herter, T.
Lillo Box, J.
Marquette, J. B.
Ranc, C.
Santos, N. C.
Sousa, S. G.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv techniques: spectroscopic
techniques: high angular resolution
stars: individual: OGLE-2011-BLG-0417
topic techniques: spectroscopic
techniques: high angular resolution
stars: individual: OGLE-2011-BLG-0417
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The microlensing event OGLE-2011-BLG-0417 is an exceptionally bright lens binary that was predicted to present radial velocity variation at the level of several km s-1. Pioneer radial velocity follow-up observations with the UVES spectrograph at the ESO−VLT of this system clearly ruled out the large radial velocity variation, leaving a discrepancy between the observation and the prediction. In this paper, we further characterise the microlensing system by analysing its spectral energy distribution (SED) derived using the UVES spectrum and new observations with the ARCoIRIS (CTIO) near-infrared spectrograph and the Keck adaptive optics instrument NIRC2 in the J, H, and Ks-bands. We determine the mass and distance of the stars independently from the microlensing modelling. We find that the SED is compatible with a giant star in the Galactic bulge and a foreground star with a mass of 0.94 ± 0.09 M⊙  at a distance of 1.07 ± 0.24 kpc. We find that this foreground star is likely the lens. Its parameters are not compatible with the ones previously reported in the literature (0.52 ± 0.04 M⊙ at 0.95 ± 0.06 kpc), based on the microlensing light curve. A thoughtful re-analysis of the microlensing event is mandatory to fully understand the reason of this new discrepancy. More importantly, this paper demonstrates that spectroscopic follow-up observations of microlensing events are possible and provide independent constraints on the parameters of the lens and source stars, hence breaking some degeneracies in the analysis. UV-to-NIR low-resolution spectrographs like X-shooter (ESO−VLT) could substantially contribute to this follow-up efforts, with magnitude limits above all microlensing events detected so far.
Fil: Santerne, A.. Universidade do Porto; Portugal
Fil: Beaulieu, J. P.. Université Pierre & Marie Curie; Francia
Fil: Rojas Ayala, B.. Universidad Andres Bello; Chile
Fil: Boisse, I.. Laboratoire d’Astrophysique de Marseille; Francia
Fil: Schlawin, E.. University Of Arizona; Estados Unidos
Fil: Almenara, J.-M.. Institut de Planétologie et d’Astrophysique de Grenoble; Francia
Fil: Batista, V.. Université Pierre & Marie Curie; Francia
Fil: Bennett, D.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados Unidos
Fil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Figueira, P.. Universidade do Porto; Portugal
Fil: James, D. J.. Cerro Tololo Inter-American Observatory; Chile
Fil: Herter, T.. Cornell University; Estados Unidos
Fil: Lillo Box, J.. European Southern Observatory; Chile
Fil: Marquette, J. B.. Université Pierre & Marie Curie; Francia
Fil: Ranc, C.. Université Pierre & Marie Curi; Francia
Fil: Santos, N. C.. Universidade do Porto; Portugal
Fil: Sousa, S. G.. Universidade do Porto; Portugal
description The microlensing event OGLE-2011-BLG-0417 is an exceptionally bright lens binary that was predicted to present radial velocity variation at the level of several km s-1. Pioneer radial velocity follow-up observations with the UVES spectrograph at the ESO−VLT of this system clearly ruled out the large radial velocity variation, leaving a discrepancy between the observation and the prediction. In this paper, we further characterise the microlensing system by analysing its spectral energy distribution (SED) derived using the UVES spectrum and new observations with the ARCoIRIS (CTIO) near-infrared spectrograph and the Keck adaptive optics instrument NIRC2 in the J, H, and Ks-bands. We determine the mass and distance of the stars independently from the microlensing modelling. We find that the SED is compatible with a giant star in the Galactic bulge and a foreground star with a mass of 0.94 ± 0.09 M⊙  at a distance of 1.07 ± 0.24 kpc. We find that this foreground star is likely the lens. Its parameters are not compatible with the ones previously reported in the literature (0.52 ± 0.04 M⊙ at 0.95 ± 0.06 kpc), based on the microlensing light curve. A thoughtful re-analysis of the microlensing event is mandatory to fully understand the reason of this new discrepancy. More importantly, this paper demonstrates that spectroscopic follow-up observations of microlensing events are possible and provide independent constraints on the parameters of the lens and source stars, hence breaking some degeneracies in the analysis. UV-to-NIR low-resolution spectrographs like X-shooter (ESO−VLT) could substantially contribute to this follow-up efforts, with magnitude limits above all microlensing events detected so far.
publishDate 2016
dc.date.none.fl_str_mv 2016-11
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/11336/18441
Santerne, A.; Beaulieu, J. P.; Rojas Ayala, B.; Boisse, I.; Schlawin, E.; et al.; Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417; Edp Sciences; Astronomy And Astrophysics; 595; L11; 11-2016; 1-8
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/18441
identifier_str_mv Santerne, A.; Beaulieu, J. P.; Rojas Ayala, B.; Boisse, I.; Schlawin, E.; et al.; Spectroscopic characterisation of microlensing events: Towards a new interpretation of OGLE-2011-BLG-0417; Edp Sciences; Astronomy And Astrophysics; 595; L11; 11-2016; 1-8
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/doi/10.1051/0004-6361/201527710
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1610.04446
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/11/aa27710-15/aa27710-15.html
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 12.982451

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