MOA-2010-BLG-311 : a planetary candidate below the threshold of reliable detection
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We analyze MOA-2010-BLG-311, a high magnification (Amax > 600) microlensing event with complete data coverage over the peak, making it very sensitive to planetary signals. We fit this event with both a point lens and a two-body lens model and find that the two-body lens model is a better fit but with only Δχ2 ~ 80. The preferred mass ratio between the lens star and its companion is q = 10−3.7 ± 0.1, placing the candidate companion in the planetary regime. Despite the formal significance of the planet, we show that because of systematics in the data the evidence for a planetary companion to the lens is too tenuous to claim a secure detection. When combined with analyses of other high-magnification events, this event helps empirically define the threshold for reliable planet detection in high-magnification events, which remains an open question.
Yee , J C , Hung , L -W , Bond , I A , Allen , W , Monard , L A G , Albrow , M D , Fouque , P , Dominik , M , Tsapras , Y , Udalski , A , Gould , A , Zellem , R , Bos , M , Christie , G W , DePoy , D L , Dong , S , Drummond , J , Gaudi , B S , Gorbikov , E , Han , C , Kaspi , S , Klein , N , Lee , C -U , Maoz , D , McCormick , J , Moorhouse , D , Natusch , T , Nola , M , Park , B -G , Pogge , R W , Polishook , D , Shporer , A , Shvartzvald , Y , Skowron , J , Thornley , G , Abe , F , Bennett , D P , Botzler , C S , Chote , P , Freeman , M , Fukui , A , Furusawa , K , Harris , P , Itow , Y , Ling , C H , Masuda , K , Matsubara , Y , Miyake , N , Ohnishi , K , Rattenbury , N J , Saito , T , Sullivan , D J , Sumi , T , Suzuki , D , Sweatman , W L , Tristram , P J , Wada , K , Yock , P C M , Szymanski , M K , Soszynski , I , Kubiak , M , Poleski , R , Ulaczyk , K , Pietrzynski , G , Wyrzykowski , L , Bachelet , E , Batista , V , Beatty , T G , Beaulieu , J -P , Bennett , C S , Bowens-Rubin , R , Brillant , S , Caldwell , J A R , Cassan , A , Cole , A A , Corrales , E , Coutures , C , Dieters , S , Prester , D D , Donatowicz , J , Greenhill , J , Henderson , C B , Kubas , D , Marquette , J -B , Martin , R , Menzies , J W , Shappee , B , Williams , A , Wouters , D , van Saders , J , Zub , M , Street , R A , Horne , K , Bramich , D M , Steele , I A , Alsubai , K A , Bozza , V , Browne , P , Burgdorf , M J , Calchi Novati , S , Dodds , P , Finet , F , Gerner , T , Hardis , S , Harpsoe , K , Hessman , F V , Hinse , T C , Hundertmark , M , Jorgensen , U G , Kains , N , Kerins , E , Liebig , C , Mancini , L , Mathiasen , M , Penny , M T , Proft , S , Rahvar , S , Ricci , D , Sahu , K C , Scarpetta , G , Schaefer , S , Schoenebeck , F , Snodgrass , C , Southworth , J , Surdej , J & Wambsganss , J 2013 , ' MOA-2010-BLG-311 : a planetary candidate below the threshold of reliable detection ' Astrophysical Journal , vol 769 , no. 1 , 77 . DOI: 10.1088/0004-637X/769/1/77
© 2013. The American Astronomical Society. All rights reserved.
DescriptionThe MOA Collaboration acknowledges the support of grants JSPS20340052 and JSPS22403003. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A. Udalski. Work by J. C. Yee was supported by a National Science Foundation Graduate Research Fellowship under Grant No. 2009068160. A. Gould and J. C. Yee acknowledge support from NSF AST-1103471. B. S. Gaudi, A. Gould, L.-W. Hung, and R. W. Pogge acknowledge support from NASA grant NNX12AB99G. A. Gould and D. Maoz acknowledge support by a grant from the US Israel Binational Science Foundation. Work by C. Han was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. Work by S. Dong was performed under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. Mount Canopus Observatory is supported by Dr. David Warren. T. C. Hinse gratefully acknowledges financial support from the Korea Research Council for Fundamental Science and Technology (KRCF) through the Young Research Scientist Fellowship Program. T. C. Hinse and C.-U. Lee acknowledge financial support from KASI (Korea Astronomy and Space Science Institute) grant number 2012-1-410-02. B. Shappee and J. van Saders are also supported by National Science Foundation Graduate Research Fellowships. K. Alsubai, D. M. Bramich, M. Dominik, K. Horne, M. Hundertmark, C. Liebig, C. Snodgrass, R. A. Street, and Y. Tsapras thank the Qatar Foundation for support from QNRF grant NPRP-09-476-1-078. The MiNDSTEp monitoring campaign is powered by ARTEMiS (Automated Terrestrial Exoplanet Microlensing Search; Dominik et al. 2008). M. Hundertmark acknowledges support by the German Research Foundation (DFG). D. Ricci (boursier FRIA) and J. Surdej acknowledge support from the Communaut/'e française Belgique Actions de recherche concertées—Acad/'emie universitaire Wallonie-Europe. C. Snodgrass received funding from the European Union Seventh Framework Programme (FPT/2007-2013) under grant agreement 268421. This work is based in part on data collected by MiNDSTEp with the Danish 1.54 m telescope at the ESO La Silla Observatory. The Danish 1.54 m telescope is operated based on a grant from the Danish Natural Science Foundation (FNU). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The National Geographic Society—Palomar Observatory Sky Atlas (POSS-I) was made by the California Institute of Technology with grants from the National Geographic Society. The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation. The Oschin Schmidt Telescope is operated by the California Institute of Technology and Palomar Observatory. The UK Schmidt Telescope was operated by the Royal Observatory Edinburgh, with funding from the UK Science and Engineering Research Council (later the UK Particle Physics and Astronomy Research Council), until 1988 June, and thereafter by the Anglo-Australian Observatory.
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