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dc.contributor.authorTsapras, Y.
dc.contributor.authorHundertmark, M.
dc.contributor.authorWyrzykowski, Ł.
dc.contributor.authorHorne, Keith Douglas
dc.contributor.authorUdalski, A.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorStreet, R.
dc.contributor.authorBramich, D. M.
dc.contributor.authorDominik, Martin
dc.contributor.authorBozza, V.
dc.contributor.authorFiguera Jaimes, R.
dc.contributor.authorKains, N.
dc.contributor.authorSkowron, J.
dc.contributor.authorSzymański, M. K.
dc.contributor.authorPietrzyński, G.
dc.contributor.authorSoszyński, I.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorKozłowski, S.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorPoleski, R.
dc.date.accessioned2016-03-28T11:03:48Z
dc.date.available2016-03-28T11:03:48Z
dc.date.issued2016-04-01
dc.identifier.citationTsapras , Y , Hundertmark , M , Wyrzykowski , Ł , Horne , K D , Udalski , A , Snodgrass , C , Street , R , Bramich , D M , Dominik , M , Bozza , V , Figuera Jaimes , R , Kains , N , Skowron , J , Szymański , M K , Pietrzyński , G , Soszyński , I , Ulaczyk , K , Kozłowski , S , Pietrukowicz , P & Poleski , R 2016 , ' The OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008) ' , Monthly Notices of the Royal Astronomical Society , vol. 457 , no. 2 , pp. 1320-1331 . https://doi.org/10.1093/mnras/stw023en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 241587919
dc.identifier.otherPURE UUID: a046962a-6b5e-4655-a48e-ae817e920304
dc.identifier.otherRIS: urn:E9D390AD8F948B35B9C8E65150C5B7A6
dc.identifier.otherScopus: 84963533500
dc.identifier.otherWOS: 000373580500016
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996687
dc.identifier.urihttp://hdl.handle.net/10023/8500
dc.descriptionKH, DB, MD and MH are supported by NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of Qatar Foundation). KH acknowledges support from STFC grant ST/M001296/1. NK acknowledges an ESO Fellowship. The research leading to these results has received funding from the European Community’s Seventh Framework Programme (/FP7/2007-2013/) under grant agreement no. 229517. This publication was made possible by NPRP grant no. X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). CS received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 268421.en
dc.description.abstractWe use six years (2003–2008) of Optical Gravitational Lensing Experiment-III microlensing observations to derive the survey detection efficiency for a range of planetary masses and projected distances from the host star. We perform an independent analysis of the microlensing light curves to extract the event parameters and compute the planet detection probability given the data. 2433 light curves satisfy our quality selection criteria and are retained for further processing. The aggregate of the detection probabilities over the range explored yields the expected number of microlensing planet detections. We employ a Galactic model to convert this distribution from dimensionless to physical units, α/au and M⊕. The survey sensitivity to small planets is highest in the range 1–4 au, shifting to slightly larger separations for more massive ones.
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016 The Authors. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://dx.doi.org/10.1093/mnras/stw023en
dc.subjectGravitational lensing: microen
dc.subjectPlanetary systemsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe OGLE-III planet detection efficiency from six years of microlensing observations (2003–2008)en
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stw023
dc.description.statusPeer revieweden


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