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Related papers: OGLE 2003-BLG-235/MOA 2003-BLG-53: A planetary mic…

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We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K or M-dwarf star in the inner Galactic disk or Galactic bulge. The high cadence observations of the MOA-II survey discovered…

Earth and Planetary Astrophysics · Physics 2015-05-20 N. Miyake , T. Sumi , Subo Dong , R. Street , L. Mancini , A. Gould , D. P. Bennett , Y. Tsapras , J. C. Yee , M. D. Albrow , I. A. Bond , P. Fouque , P. Browne , C. Han , C. Snodgrass , F. Finet , K. Furusawa , K. Harpsoe , W. Allen , M. Hundertmark , M. Freeman , D. Suzuki , F. Abe , C. S. Botzler , D. Douchin , A. Fukui , F. Hayashi , J. B. Hearnshaw , S. Hosaka , Y. Itow , K. Kamiya , P. M. Kilmartin , A. Korpela , W. Lin , C. H. Ling , S. Makita , K. Masuda , Y. Matsubara , Y. Muraki , T. Nagayama , K. Nishimoto , K. Ohnishi , Y. C. Perrott , N. Rattenbury , To. Saito , L. Skuljan , D. J. Sullivan , W. L. Sweatman , P. J. Tristram , K. Wada , P. C. M. Yock , The MOA Collaboration , G. Bolt , M. Bos , G. W. Christie , D. L. DePoy , J. Drummond , A. Gal-Yam , B. S. Gaudi , E. Gorbikov , D. Higgins , K. -H. Hwang J. Janczak , S. Kaspi , C. -U. Lee , J. -R. Koo , S. Koz lowski , Y. Lee , F. Mallia , A. Maury , D. Maoz , J. McCormick , L. A. G. Monard , D. Moorhouse , J. A. Mu~noz , T. Natusch , E. O. Ofek , R. W. Pogge , D. Polishook , R. Santallo , A. Shporer , O. Spector , G. Thornley , The Micro FUN Collaboration , A. Allan , D. M. Bramich , K. Horne , N. Kains , I. Steele , The RoboNet Collaboration , V. Bozza , M. J. Burgdorf , S. Calchi Novati , M. Dominik , S. Dreizler , M. Glitrup , F. V. Hessman , T. C. Hinse , U. G. Jorgensen , C. Liebig , G. Maier , M. Mathiasen , S. Rahvar , D. Ricci , G. Scarpetta , J. Skottfelt , J. Southworth , J. Surdej , J. Wambsganss , F. Zimmer , The MiNDSTEp Consortium , V. Batista , J. P. Beaulieu , S. Brillant , A. Cassan , A. Cole , E. Corrales , Ch. Coutures , S. Dieters , J. Greenhill , D. Kubas , J. Menzies , The PLANET Collaboration

We investigated microlensing events detected by the OGLE and KMTNet surveys during the 2024 observing season, focusing on those that exhibit very complex anomaly features. Through this analysis, we found that the light curves of three…

We have investigated the lensing event KMT-2024-BLG-0404. The light curve of the event exhibited a complex structure with multiple distinct features, including two prominent caustic spikes, two cusp bumps, and a brief discontinuous feature…

Microlensing can provide a useful tool to probe binary distributions down to low-mass limits of binary companions. In this paper, we analyze the light curves of 8 binary lensing events detected through the channel of high-magnification…

Solar and Stellar Astrophysics · Physics 2015-05-30 I. -G. Shin , J. -Y. Choi , S. -Y. Park , C. Han , A. Gould , T. Sumi , A. Udalski , J. -P. Beaulieu , M. Dominik , W. Allen , M. Bos , G. W. Christie , D. L. Depoy , S. Dong , J. Drummond , A. Gal-Yam , B. S. Gaudi , L. -W. Hung , J. Janczak , S. Kaspi , C. -U. Lee , F. Mallia , D. Maoz , A. Maury , J. McCormick , L. A. G. Monard , D. Moorhouse , J. A. Muñoz , T. Natusch , C. Nelson , B. -G. Park , R. W. Pogge , D. Polishook , Y. Shvartzvald , A. Shporer , G. Thornley , J. C. Yee , F. Abe , D. P. Bennett , I. A. Bond , C. S. Botzler , A. Fukui , K. Furusawa , F. Hayashi , J. B. Hearnshaw , S. Hosaka , Y. Itow , K. Kamiya , P. M. Kilmartin , S. Kobara , A. Korpela , W. Lin , C. H. Ling , S. Makita , K. Masuda , Y. Matsubara , N. Miyake , Y. Muraki , M. Nagaya , K. Nishimoto , K. Ohnishi , T. Okumura , K. Omori , Y. C. Perrott , N. Rattenbury , To. Saito , L. Skuljan , D. J. Sullivan , D. Suzuki , W. L. Sweatman , P. J. Tristram , K. Wada , P. C. M. Yock , M. K. Szymański , M. Kubiak , G. Pietrzyński , I. Soszyński , R. Poleski , K. Ulaczyk , Ł. Wyrzykowski , S. Kozłowski , P. Pietrukowicz , M. D. Albrow , V. Batista , D. M. Bramich , S. Brillant , J. A. R. Caldwell , J. J. Calitz , A. Cassan , A. Cole , K. H. Cook , E. Corrales , Ch. Coutures , S. Dieters , D. Dominis Prester , J. Donatowicz , P. Fouqué , J. Greenhill , M. Hoffman , U. G. Jørgensen , S. R. Kane , D. Kubas , J. -B. Marquette , R. Martin , P. Meintjes , J. Menzies , K. R. Pollard , K. C. Sahu , J. Wambsganss , A. Williams , C. Vinter , M. Zub , A. Allan , P. Browne , K. Horne , C. Snodgrass , I. Steele , R. Street , Y. Tsapras , K. A. Alsubai , V. Bozza , P. Browne , M. J. Burgdorf , S. Calchi Novati , P. Dodds , S. Dreizler , F. Finet , T. Gerner , M. Glitrup , F. Grundahl , S. Hardis , K. Harpsøe , F. V. Hessman , T. C. Hinse , M. Hundertmark , N. Kains , E. Kerins , C. Liebig , G. Maier , L. Mancini , M. Mathiasen , M. T. Penny , S. Proft , S. Rahvar , D. Ricci , G. Scarpetta , S. Schäfer , F. Schönebeck , J. Skottfelt , J. Surdej , J. Southworth , F. Zimmer

Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation history. In this paper, we present the candidate binaries with brown dwarf…

Solar and Stellar Astrophysics · Physics 2015-06-11 I. -G. Shin , C. Han , A. Gould , A. Udalski , T. Sumi , M. Dominik , J. -P. Beaulieu , Y. Tsapras , V. Bozza , M. K. Szymański , M. Kubiak , I. Soszyński , G. Pietrzyński , R. Poleski , K. Ulaczyk , P. Pietrukowicz , S. Kozłowski , J. Skowron , Ł. Wyrzykowski , F. Abe , D. P. Bennett , I. A. Bond , C. S. Botzler , M. Freeman , A. Fukui , K. Furusawa , F. Hayashi , J. B. Hearnshaw , S. Hosaka , Y. Itow , K. Kamiya , P. M. Kilmartin , S. Kobara , A. Korpela , W. Lin , C. H. Ling , S. Makita , K. Masuda , Y. Matsubara , N. Miyake , Y. Muraki , M. Nagaya , K. Nishimoto , K. Ohnishi , T. Okumura , K. Omori , Y. C. Perrott , N. Rattenbury , To. Saito , L. Skuljan , D. J. Sullivan , D. Suzuki , W. L. Sweatman , P. J. Tristram , K. Wada , P. C. M. Yock , G. W. Christie , D. L. Depoy , S. Dong , A. Gal-Yam , B. S. Gaudi , L. -W. Hung , J. Janczak , S. Kaspi , D. Maoz , J. McCormick , D. McGregor , D. Moorhouse , J. A. Muñoz , T. Natusch , C. Nelson , R. W. Pogge , T. -G. Tan , D. Polishook , Y. Shvartzvald , A. Shporer , G. Thornley , U. Malamud , J. C. Yee , J. -Y. Choi , Y. -K. Jung , H. Park , C. -U. Lee , B. -G. Park , J. -R. Koo , D. Bajek , D. M. Bramich , P. Browne , K. Horne , S. Ipatov , C. Snodgrass , I. Steele , R. Street , K. A. Alsubai , M. J. Burgdorf , S. Calchi Novati , P. Dodds , S. Dreizler , X. -S. Fang , F. Grundahl , C. -H. Gu , S. Hardis , K. Harpsøe , T. C. Hinse , M. Hundertmark , J. Jessen-Hansen , U. G. Jørgensen , N. Kains , E. Kerins , C. Liebig , M. Lund , M. Lundkvist , L. Mancini , M. Mathiasen , A. Hornstrup , M. T. Penny , S. Proft , S. Rahvar , D. Ricci , G. Scarpetta , J. Skottfelt , J. Southworth , J. Surdej , J. Tregloan-Reed , O. Wertz , F. Zimmer , M. D. Albrow , V. Batista , S. Brillant , J. A. R. Caldwell , J. J. Calitz , A. Cassan , A. Cole , K. H. Cook , E. Corrales , Ch. Coutures , S. Dieters , D. Dominis Prester , J. Donatowicz , P. Fouqué , J. Greenhill , K. Hill , M. Hoffman , S. R. Kane , D. Kubas , J. -B. Marquette , R. Martin , P. Meintjes , J. Menzies , K. R. Pollard , K. C. Sahu , J. Wambsganss , A. Williams , C. Vinter , M. Zub

We present the analysis of the binary gravitational microlensing event MOA-2015-BLG-020. The event has a fairly long timescale (about 63 days) and thus the light curve deviates significantly from the lensing model that is based on the…

Microlensing is able to reveal multiple body systems located several kilo-parsec away from the Earth. Since it does not require the measurement of light from the lens, microlensing is sensitive to a range of objects from free-floating…

Earth and Planetary Astrophysics · Physics 2018-10-17 E. Bachelet , J. -P. Beaulieu , I. Boisse , A. Santerne , R. A. Street

OGLE-2004-BLG-343 was a microlensing event with peak magnification A_{max}=3000+/-1100, by far the highest-magnification event ever analyzed and hence potentially extremely sensitive to planets orbiting the lens star. Due to human error,…

We report the analysis of OGLE-2019-BLG-0960, which contains the smallest mass-ratio microlensing planet found to date (q = 1.2--1.6 x 10^{-5} at 1-sigma). Although there is substantial uncertainty in the satellite parallax measured by…

In this paper, we report the discovery of a binary composed of a brown dwarf and a low-mass M dwarf from the observation of the microlensing event OGLE-2014-BLG-0257. Resolution of the very short-lasting caustic crossing combined with the…

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. Pioneer radial velocity follow-up observations with the UVES spectrograph…

Microlensing is the only known direct method to measure the masses of stars that lack visible companions. In terms of microlensing observables, the mass is given by M=(c^2/4G)\tilde r_E \theta_E and so requires the measurement of both the…

Due to the nature depending on only the gravitational field, microlensing, in principle, provides an important tool to detect faint and even dark brown dwarfs. However, the number of identified brown dwarfs is limited due to the difficulty…

We investigate constraints on additional planets orbiting the distant M-dwarf star OGLE-2005-BLG-390L, around which photometric microlensing data has revealed the existence of the sub-Neptune-mass planet OGLE-2005-BLG-390Lb. We specifically…

Astrophysics · Physics 2009-11-13 D. Kubas , A. Cassan , M. Dominik , D. Bennett

We report the discovery, via the microlensing method, of a new very-low-mass binary system. By combining measurements from Earth and from the Spitzer telescope in Earth-trailing orbit, we are able to measure the microlensing parallax of the…

We present an analysis of microlensing event OGLE-2016-BLG-0693, based on the survey-only microlensing observations by the OGLE and KMTNet groups. In order to analyze the light curve, we consider the effects of parallax, orbital motion, and…

We report the discovery of the microlensing planet OGLE-2018-BLG-0740Lb. The planet is detected with a very strong signal of $\Delta\chi^2\sim 4630$, but the interpretation of the signal suffers from two types of degeneracies. One type is…