A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192

We report the detection of an extrasolar planet of mass ratio q ~ 2 × 10−4 in microlensing event MOA-2007-BLG-192. The best-fit microlensing model shows both the microlensing parallax and finite source effects, and these can be combined to obtain the lens masses of M = 0.060+ 0.028−0.021 M☉ for the...

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Detalles Bibliográficos
Autores: Bennett, D.P., Bond, I.A., Pietrzynski, G.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2008
País:Chile
Idioma:inglés
OAI Identifier:oai:repositorio.anid.cl:10533/236908
Acceso en línea:https://hdl.handle.net/10533/236908
Access Level:acceso abierto
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spelling Pietrzynski, G.Bond, I.A.Bennett, D.P.200810.1086/589940https://hdl.handle.net/10533/236908http://purl.org/coar/access_right/c_abf2A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192Bennett, D.P.Bond, I.A.Pietrzynski, G.2019-12-18T18:14:17Z2022-07-07T21:57:47Z2019-12-18T18:14:17Z2022-07-07T21:57:47Z2008We report the detection of an extrasolar planet of mass ratio q ~ 2 × 10−4 in microlensing event MOA-2007-BLG-192. The best-fit microlensing model shows both the microlensing parallax and finite source effects, and these can be combined to obtain the lens masses of M = 0.060+ 0.028−0.021 M☉ for the primary and m = 3.3+ 4.9−1.6 M⊕ for the planet. However, the observational coverage of the planetary deviation is sparse and incomplete, and the radius of the source was estimated without the benefit of a source star color measurement. As a result, the 2 σ limits on the mass ratio and finite source measurements are weak. Nevertheless, the microlensing parallax signal clearly favors a substellar mass planetary host, and the measurement of finite source effects in the light curve supports this conclusion. Adaptive optics images taken with the Very Large Telescope (VLT) NACO instrument are consistent with a lens star that is either a brown dwarf or a star at the bottom of the main sequence. Follow-up VLT and/or Hubble Space Telescope (HST) observations will either confirm that the primary is a brown dwarf or detect the low-mass lens star and enable a precise determination of its mass. In either case, the lens star, MOA-2007-BLG-192L, is the lowest mass primary known to have a companion with a planetary mass ratio, and the planet, MOA-2007-BLG-192Lb, is probably the lowest mass exoplanet found to date, aside from the lowest mass pulsar planet.FONDAPFONDAP1501000315010003virtual::31175-1WOS:000258730700050https://hdl.handle.net/10533/236908enginstname: Conicytreponame: Repositorio Digital RI2.010.1086/589940info:eu-repo/grantAgreement/Fondap/15010003https://iopscience.iop.org/article/10.1086/589940Atribución-NoComercial-SinDerivadas 3.0 Chilehttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/info:eu-repo/semantics/openAccessA Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192Astrophysical JournalArticuloinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttps://hdl.handle.net/10533/236908http://purl.org/coar/resource_type/c_2df8fbb1045fc0e1-ef55-4532-8afe-69fe789d964dvirtual::31175-1045fc0e1-ef55-4532-8afe-69fe789d964dvirtual::31175-110533/236908oai:repositorio.anid.cl:10533/2369082023-07-24 15:51:06.137https://repositorio.anid.clRepositorio ANIDaletelier@anid.cl
dc.title.none.fl_str_mv A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192
dc.title.journal.none.fl_str_mv Astrophysical Journal
title A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192
spellingShingle A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192
Bennett, D.P.
title_short A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192
title_full A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192
title_fullStr A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192
title_full_unstemmed A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192
title_sort A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192
dc.creator.none.fl_str_mv Bennett, D.P.
Bond, I.A.
Pietrzynski, G.
author Bennett, D.P.
author_facet Bennett, D.P.
Bond, I.A.
Pietrzynski, G.
author_role author
author2 Bond, I.A.
Pietrzynski, G.
author2_role author
author
description We report the detection of an extrasolar planet of mass ratio q ~ 2 × 10−4 in microlensing event MOA-2007-BLG-192. The best-fit microlensing model shows both the microlensing parallax and finite source effects, and these can be combined to obtain the lens masses of M = 0.060+ 0.028−0.021 M☉ for the primary and m = 3.3+ 4.9−1.6 M⊕ for the planet. However, the observational coverage of the planetary deviation is sparse and incomplete, and the radius of the source was estimated without the benefit of a source star color measurement. As a result, the 2 σ limits on the mass ratio and finite source measurements are weak. Nevertheless, the microlensing parallax signal clearly favors a substellar mass planetary host, and the measurement of finite source effects in the light curve supports this conclusion. Adaptive optics images taken with the Very Large Telescope (VLT) NACO instrument are consistent with a lens star that is either a brown dwarf or a star at the bottom of the main sequence. Follow-up VLT and/or Hubble Space Telescope (HST) observations will either confirm that the primary is a brown dwarf or detect the low-mass lens star and enable a precise determination of its mass. In either case, the lens star, MOA-2007-BLG-192L, is the lowest mass primary known to have a companion with a planetary mass ratio, and the planet, MOA-2007-BLG-192Lb, is probably the lowest mass exoplanet found to date, aside from the lowest mass pulsar planet.
publishDate 2008
dc.date.issued.none.fl_str_mv 2008
dc.date.accessioned.none.fl_str_mv 2019-12-18T18:14:17Z
2022-07-07T21:57:47Z
dc.date.available.none.fl_str_mv 2019-12-18T18:14:17Z
2022-07-07T21:57:47Z
dc.type.none.fl_str_mv Articulo
dc.type.driver.none.fl_str_mv info:eu-repo/semantics/article
dc.type.openaire.none.fl_str_mv info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.folio.none.fl_str_mv 15010003
15010003
dc.identifier.idwos.none.fl_str_mv WOS:000258730700050
dc.identifier.uri.none.fl_str_mv https://hdl.handle.net/10533/236908
identifier_str_mv 15010003
WOS:000258730700050
url https://hdl.handle.net/10533/236908
dc.language.iso.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv instname: Conicyt
reponame: Repositorio Digital RI2.0
dc.relation.doi.none.fl_str_mv 10.1086/589940
dc.relation.projectid.none.fl_str_mv info:eu-repo/grantAgreement/Fondap/15010003
dc.relation.uri.none.fl_str_mv https://iopscience.iop.org/article/10.1086/589940
dc.rights.none.fl_str_mv Atribución-NoComercial-SinDerivadas 3.0 Chile
http://creativecommons.org/licenses/by-nc-nd/3.0/cl/
dc.rights.driver.none.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv Atribución-NoComercial-SinDerivadas 3.0 Chile
http://creativecommons.org/licenses/by-nc-nd/3.0/cl/
eu_rights_str_mv openAccess
repository.name.fl_str_mv Repositorio ANID
repository.mail.fl_str_mv aletelier@anid.cl
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