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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 present the results of HST observations of the host star for the first definitive extrasolar planet detected by microlensing. The light curve model for this event predicts that the lens star should be separated from the source star by…

Astrophysics · Physics 2009-11-11 David P. Bennett , Jay Anderson , Ian A. Bond , Andrzej Udalski , Andrew Gould

We present the discovery of a Neptune-mass planet orbiting a 0.8 +- 0.3 M_Sun star in the Galactic bulge. The planet manifested itself during the microlensing event MOA 2011-BLG-028/OGLE-2011-BLG-0203 as a low-mass companion to the lens…

An extra-solar planet can be detected by microlensing because the planet can perturb the smooth lensing light curve created by the primary lens. However, it was shown by Gaudi that a subset of binary-source events can produce light curves…

Astrophysics · Physics 2009-11-06 Cheongho Han

We present the analysis of the microlensing event OGLE-2016-BLG-1227. The light curve of this short-duration event appears to be a single-lens event affected by severe finite-source effects. Analysis of the light curve based on single-lens…

We analyze KMT-2019-BLG-1339, a microlensing event with an obvious but incompletely resolved brief anomaly feature around the peak of the light curve. Although the origin of the anomaly is identified to be a companion to the lens with a low…

Recently, the discovery of a Venus-mass planet orbiting a brown-dwarf host in a binary system was reported from the analysis of the microlensing event OGLE-2013-BLG-0723. We reanalyze the event considering the possibility of other…

Earth and Planetary Astrophysics · Physics 2016-07-06 Cheongho Han , David P. Bennett , Andrzej Udalski , Youn Kil Jung

We constrain the host-star flux of the microlensing planet OGLE-2014-BLG-0676Lb using adaptive optics (AO) images taken by the Magellan and Keck telescopes. We measure the flux of the light blended with the microlensed source to be K =…

High-magnification gravitational microlensing events provide an important channel of detecting planetary systems with multiple giants located at their birth places. In order to investigate the potential existence of additional planets, we…

Earth and Planetary Astrophysics · Physics 2015-06-23 I. -G. Shin , C. Han , J. -Y. Choi , K. -H. Hwang , Y. K. Jung , H. Park

We announce the discovery of a microlensing planetary system, in which a sub-Saturn planet is orbiting an ultracool dwarf host. We detect the planetary system by analyzing the short-timescale ($t_{\rm E}\sim 4.4$~days) lensing event…

We present high resolution follow-up data of the planetary microlensing event MOA-2010-BLG-328, using Keck and the Hubble. Keck data, taken 8 years after the event, reveal a strong lens detection enabling a direct measurement of lens flux…

Gravitational microlensing offers a powerful method with which to probe a variety of binary-lens systems, as the binarity of the lens introduces deviations from the typical (single-lens) Paczy\'nski behaviour in the event light curves.…

Solar and Stellar Astrophysics · Physics 2015-06-18 A. A. Nucita , M. Giordano , F. De Paolis , G. Ingrosso

Light curves of microlensing events involving stellar binaries and planetary systems can provide information about the orbital elements of the system due to orbital modulations of the caustic structure. Accurately measuring the orbit in…

We present the analysis of high-resolution images of MOA-2013-BLG-220, taken with the Keck adaptive optics system 6 years after the initial observation, identifying the lens as a solar-type star hosting a super-Jupiter mass planet. The…

We present a detailed analysis of survey and follow-up observations of microlensing event OGLE-2012-BLG-0406 based on data obtained from 10 different observatories. Intensive coverage of the lightcurve, especially the perturbation part,…

Earth and Planetary Astrophysics · Physics 2015-06-17 Y. Tsapras , J. -Y. Choi , R. A. Street , C. Han , V. Bozza , A. Gould , M. Dominik , J. -P. Beaulieu , A. Udalski , U. G. Jørgensen , T. Sumi , D. M. Bramich , P. Browne , K. Horne , M. Hundertmark , S. Ipatov , N. Kains , C. Snodgrass , I. A. Steele , K. A. Alsubai , J. M. Andersen , S. Calchi Novati , Y. Damerdji , C. Diehl , A. Elyiv , E. Giannini , S. Hardis , K. Harpsøe , T. C. Hinse , D. Juncher , E. Kerins , H. Korhonen , C. Liebig , L. Mancini , M. Mathiasen , M. T. Penny , M. Rabus , S. Rahvar , G. Scarpetta , J. Skottfelt , J. Southworth , J. Surdej , J. Tregloan-Reed , C. Vilela , J. Wambsganss , J. Skowron , R. Poleski , S. Kozłowski , Łukasz Wyrzykowski , M. K. Szymański , M. Kubiak , P. Pietrukowicz , G. Pietrzyński , I. Soszyński , K. Ulaczyk , M. D. Albrow , E. Bachelet , R. Barry , V. Batista , A. Bhattacharya , S. Brillant , J. A. R. Caldwell , A. Cassan , A. Cole , E. Corrales , Ch. Coutures , S. Dieters , D. Dominis Prester , J. Donatowicz , P. Fouqué , J. Greenhill , S. R. Kane , D. Kubas , J. -B. Marquette , J. Menzies , C. P`ere , K. R. Pollard , D. Wouters , G. Christie , D. L. DePoy , S. Dong , J. Drummond , B. S. Gaudi , C. B. Henderson , K. H. Hwang , Y. K. Jung , A. Kavka , J. -R. Koo , C. -U. Lee , D. Maoz , L. A. G. Monard , T. Natusch , H. Ngan , H. Park , R. W. Pogge , I. Porritt , I. -G. Shin , Y. Shvartzvald , T. G. Tan , J. C. Yee , F. Abe , D. P. Bennett , I. A. Bond , C. S. Botzler , M. Freeman , A. Fukui , D. Fukunaga , Y. Itow , N. Koshimoto , C. H. Ling , K. Masuda , Y. Matsubara , Y. Muraki , S. Namba , K. Ohnishi , N. J. Rattenbury , To. Saito , D. J. Sullivan , W. L. Sweatman , D. Suzuki , P. J. Tristram , N. Tsurumi , K. Wada , N. Yamai , P. C. M. Yock A. Yonehara

We performed optical spectroscopic monitoring of the BL Lac object AO 0235+164 (z=0.94) with the VLT and TNG telescopes from Aug. 2003 to Dec. 2004, during an extended WEBT campaign. The flux of this source is both contaminated and absorbed…

Astrophysics · Physics 2009-11-13 C. M. Raiteri , M. Villata , A. Capetti , J. Heidt , M. Arnaboldi , A. Magazzu`