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Adaptive Optics Imaging Can Break the Central Caustic Cusp Approach Degeneracy in High-magnification Microlensing Events

dc.contributor.authorTERRY, Sean
dc.contributor.authorBENNETT, David
dc.contributor.authorBHATTACHARYA, Aparna
dc.contributor.authorKOSHIMOTO, Naoki
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorBEAULIEU, Jean-Philippe
dc.contributor.authorBLACKMAN, Joshua
dc.contributor.authorBOND, Ian
dc.contributor.authorCOLE, Andrew
dc.contributor.authorLU, Jessica
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorMARQUETTE, Jean Baptiste
dc.contributor.authorRANC, Clément
dc.contributor.authorREKTSINI, Natalia
dc.contributor.authorVANDOROU, Aikaterini
dc.date.issued2022-10-26
dc.identifier.issn0004-6256
dc.description.abstractEnAbstract We report new results for the gravitational microlensing target OGLE-2011-BLG-0950 from adaptive optics images using the Keck Observatory. The original analysis by Choi et al. and reanalysis by Suzuki et al. report degenerate solutions between planetary and stellar binary lens systems. This particular case is the most important type of degeneracy for exoplanet demographics because the distinction between a planetary mass or stellar binary companion has direct consequences for microlensing exoplanet statistics. The 8 and 10 yr baselines allow us to directly measure a relative proper motion of 4.20 ± 0.21 mas yr −1 , confirming the detection of the lens star system and ruling out the planetary companion models that predict a ∼4× smaller relative proper motion. The Keck data also rule out the wide stellar binary solution unless one of the components is a stellar remnant. The combination of the lens brightness and close stellar binary light-curve parameters yields primary and secondary star masses of M A = 1.12 − 0.09 + 0.11 and M B = 0.47 − 0.10 + 0.13 M ☉ at a distance of D L = 6.70 − 0.30 + 0.55 kpc and a projected separation of 0.39 − 0.04 + 0.05 au. Assuming that the predicted proper motions are measurably different, the high-resolution imaging method described here can be used to disentangle this degeneracy for events observed by the Roman exoplanet microlensing survey using Roman images taken near the beginning or end of the survey.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.title.enAdaptive Optics Imaging Can Break the Central Caustic Cusp Approach Degeneracy in High-magnification Microlensing Events
dc.typeArticle de revue
dc.identifier.doi10.3847/1538-3881/ac9518
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
bordeaux.journalThe Astronomical Journal
bordeaux.page217
bordeaux.volume164
bordeaux.issue5
bordeaux.peerReviewedoui
hal.identifierhal-03974286
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03974286v1
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