I. A. Bond - The MOA Collaboration

I. A. Bond
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I. A. Bond
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The MOA Collaboration
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Earth and Planetary Astrophysics (42)
 
Solar and Stellar Astrophysics (10)
 
Astrophysics of Galaxies (4)
 
High Energy Astrophysical Phenomena (1)

Publications Authored By I. A. Bond

We present a detailed elemental abundance study of 90 F and G dwarf, turn-off and subgiant stars in the Galactic bulge. Based on high-resolution spectra acquired during gravitational microlensing events, stellar ages and abundances for 11 elements (Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Zn, Y and Ba) have been determined. We find that the Galactic bulge has a wide metallicity distribution with significant peaks at [Fe/H]=-1. Read More

It has recently been discovered that some, if not all, classical novae emit GeV gamma-rays during outburst, but the mechanics of this gamma-ray emission are still not well understood. We present here a comprehensive, multi-wavelength dataset---from radio to X-rays---for the most gamma-ray luminous classical nova to-date, V1324 Sco. Using this dataset, we show that V1324 Sco is a canonical dusty Fe-II type nova, with a bulk ejecta velocity of $1150 \pm 40~\rm km~s^{-1}$ and an ejecta mass of $2. Read More

We report the results of the statistical analysis of planetary signals discovered in MOA-II microlensing survey alert system events from 2007 to 2012. We determine the survey sensitivity as a function of planet-star mass ratio, $q$, and projected planet-star separation, $s$, in Einstein radius units. We find that the mass ratio function is not a single power-law, but has a change in slope at $q \sim 10^{-4}$, corresponding to $\sim 20 M_{\oplus}$ for the median host star mass of $\sim 0. Read More

We report the discovery of a planet --- OGLE-2014-BLG-0676Lb --- via gravitational microlensing. Observations for the lensing event were made by the MOA, OGLE, Wise, RoboNET/LCOGT, MiNDSTEp and $\mu$FUN groups. All analyses of the light curve data favour a lens system comprising a planetary mass orbiting a host star. Read More

In the process of analyzing an observed light curve, one often confronts various scenarios that can mimic the planetary signals causing difficulties in the accurate interpretation of the lens system. In this paper, we present the analysis of the microlensing event OGLE-2016-BLG-0733. The light curve of the event shows a long-term asymmetric perturbation that would appear to be due to a planet. Read More

We present the analysis of the first circumbinary planet microlensing event, OGLE-2007-BLG-349. This event has a strong planetary signal that is best fit with a mass ratio of $q \approx 3.4\times10^{-4}$, but there is an additional signal due to an additional lens mass, either another planet or another star. Read More

We report the discovery of a microlensing planet OGLE-2012-BLG-0950Lb with the planet/host mass ratio of $q \sim 2 \times 10^{-4}$. A long term distortion detected in both MOA and OGLE light curve can be explained by the microlens parallax due to the Earth's orbital motion around the Sun. Although the finite source effect is not detected, we obtain the lens flux by the high resolution Keck AO observation. Read More

Simultaneous observations of microlensing events from multiple locations allow for the breaking of degeneracies between the physical properties of the lensing system, specifically by exploring different regions of the lens plane and by directly measuring the "microlens parallax". We report the discovery of a 30-55$M_J$ brown dwarf orbiting a K dwarf in microlensing event OGLE-2015-BLG-1319. The system is located at a distance of $\sim$5 kpc toward the Galactic bulge. Read More

We report the discovery of a planet by the microlensing method, OGLE-2012-BLG-0724Lb. Although the duration of the planetary signal for this event was one of the shortest seen for a planetary event, the anomaly was well covered thanks to high cadence observations taken by the survey groups OGLE and MOA. By analyzing the light curve, this planetary system is found to have a mass ratio $q=(1. Read More

Spitzer microlensing parallax observations of OGLE-2015-BLG-1212 decisively breaks a degeneracy between planetary and binary solutions that is somewhat ambiguous when only ground-based data are considered. Only eight viable models survive out of an initial set of 32 local minima in the parameter space. These models clearly indicate that the lens is a stellar binary system possibly located within the bulge of our Galaxy, ruling out the planetary alternative. Read More

2015Dec
Authors: Calen B. Henderson, Radosław Poleski, Matthew Penny, Rachel A. Street, David P. Bennett, David W. Hogg, B. Scott Gaudi, W. Zhu, T. Barclay, G. Barentsen, S. B. Howell, F. Mullally, A. Udalski, M. K. Szymański, J. Skowron, P. Mróz, S. Kozłowski, Ł. Wyrzykowski, P. Pietrukowicz, I. Soszyński, K. Ulaczyk, M. Pawlak, T. Sumi, F. Abe, Y. Asakura, R. K. Barry, A. Bhattacharya, I. A. Bond, M. Donachie, M. Freeman, A. Fukui, Y. Hirao, Y. Itow, N. Koshimoto, M. C. A. Li, C. H. Ling, K. Masuda, Y. Matsubara, Y. Muraki, M. Nagakane, K. Ohnishi, H. Oyokawa, N. Rattenbury, To. Saito, A. Sharan, D. J. Sullivan, P. J. Tristram, A. Yonehara, E. Bachelet, D. M. Bramich, A. Cassan, M. Dominik, R. Figuera Jaimes, K. Horne, M. Hundertmark, S. Mao, C. Ranc, R. Schmidt, C. Snodgrass, I. A. Steele, Y. Tsapras, J. Wambsganss, V. Bozza, M. J. Burgdorf, U. G. Jørgensen, S. Calchi Novati, S. Ciceri, G. D'Ago, D. F. Evans, F. V. Hessman, T. C. Hinse, T. -O. Husser, L. Mancini, A. Popovas, M. Rabus, S. Rahvar, G. Scarpetta, J. Skottfelt, J. Southworth, E. Unda-Sanzana, S. T. Bryson, D. A. Caldwell, M. R. Haas, K. Larson, K. McCalmont, M. Packard, C. Peterson, D. Putnam, L. Reedy, S. Ross, J. E. Van Cleve, R. Akeson, V. Batista, J. -P. Beaulieu, C. A. Beichman, G. Bryden, D. Ciardi, A. Cole, C. Coutures, D. Foreman-Mackey, P. Fouqué, M. Friedmann, C. Gelino, S. Kaspi, E. Kerins, H. Korhonen, D. Lang, C. -H. Lee, C. H. Lineweaver, D. Maoz, J. -B. Marquette, F. Mogavero, J. C. Morales, D. Nataf, R. W. Pogge, A. Santerne, Y. Shvartzvald, D. Suzuki, M. Tamura, P. Tisserand, D. Wang

$K2$'s Campaign 9 ($K2$C9) will conduct a $\sim$3.7 deg$^{2}$ survey toward the Galactic bulge from 7/April through 1/July of 2016 that will leverage the spatial separation between $K2$ and the Earth to facilitate measurement of the microlens parallax $\pi_{\rm E}$ for $\gtrsim$127 microlensing events. These will include several that are planetary in nature as well as many short-timescale microlensing events, which are potentially indicative of free-floating planets (FFPs). Read More

2015Dec
Affiliations: 1The OGLE Collaboration, 2The OGLE Collaboration, 3The OGLE Collaboration, 4The OGLE Collaboration, 5The OGLE Collaboration, 6The OGLE Collaboration, 7The OGLE Collaboration, 8The OGLE Collaboration, 9The OGLE Collaboration, 10The OGLE Collaboration, 11The MOA Collaboration, 12The MOA Collaboration, 13The MOA Collaboration, 14The MOA Collaboration, 15The MOA Collaboration, 16The MOA Collaboration, 17The MOA Collaboration, 18The MOA Collaboration, 19The MOA Collaboration, 20The MOA Collaboration, 21The MOA Collaboration, 22The MOA Collaboration, 23The MOA Collaboration, 24The MOA Collaboration, 25The MOA Collaboration, 26The MOA Collaboration, 27The MOA Collaboration, 28The MOA Collaboration, 29The MOA Collaboration, 30The MOA Collaboration, 31The MOA Collaboration, 32The MOA Collaboration, 33The MiNDSTEp Collaboration, 34The MiNDSTEp Collaboration, 35The MiNDSTEp Collaboration, 36The MiNDSTEp Collaboration, 37The MiNDSTEp Collaboration, 38The MiNDSTEp Collaboration

We present the discovery of a Neptune-mass planet orbiting a 0.8 +- 0.3 M_Sun star in the Galactic bulge. Read More

2015Nov
Affiliations: 1The MOA Collaboration, 2The MOA Collaboration, 3The MOA Collaboration, 4The MOA Collaboration, 5The MOA Collaboration, 6The MOA Collaboration, 7The MOA Collaboration, 8The MOA Collaboration, 9The MOA Collaboration, 10The MOA Collaboration, 11The MOA Collaboration, 12The MOA Collaboration, 13The MOA Collaboration, 14The MOA Collaboration, 15The MOA Collaboration, 16The MOA Collaboration, 17The MOA Collaboration, 18The MOA Collaboration, 19The MOA Collaboration, 20The MOA Collaboration, 21The MOA Collaboration, 22The MOA Collaboration, 23The MOA Collaboration, 24The MOA Collaboration, 25The MOA Collaboration, 26The MOA Collaboration, 27The MOA Collaboration, 28The MOA Collaboration, 29The MOA Collaboration, 30The MOA Collaboration, 31The MOA Collaboration, 32The MOA Collaboration, 33The MOA Collaboration, 34The MOA Collaboration, 35The MOA Collaboration, 36The MOA Collaboration, 37The MOA Collaboration

We present the discovery of the first Neptune analog exoplanet or super-Earth with Neptune-like orbit, MOA-2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at $9\sim 14$ times the expected position of the snow-line, $a_{\rm snow}$, which is similar to Neptune's separation of $ 11\,a_{\rm snow}$ from the Sun. The planet/host-star mass ratio is $q=(3. Read More

We present a statistical analysis of the first four seasons from a "second-generation" microlensing survey for extrasolar planets, consisting of near-continuous time coverage of 8 deg$^2$ of the Galactic bulge by the OGLE, MOA, and Wise microlensing surveys. During this period, 224 microlensing events were observed by all three groups. Over 12% of the events showed a deviation from single-lens microlensing, and for $\sim$1/3 of those the anomaly is likely caused by a planetary companion. Read More

For all exoplanet candidates, the reliability of a claimed detection needs to be assessed through a careful study of systematic errors in the data to minimize the false positives rate. We present a method to investigate such systematics in microlensing datasets using the microlensing event OGLE-2013-BLG-0446 as a case study. The event was observed from multiple sites around the world and its high magnification (A_{max} \sim 3000) allowed us to investigate the effects of terrestrial and annual parallax. Read More

We report the discovery of a possible planet in microlensing event MOA-2010-BLG-353. This event was only recognised as having a planetary signal after the microlensing event had finished, and following a systematic analysis of all archival data for binary lens microlensing events collected to date. Data for event MOA-2010-BLG-353 were only recorded by the high cadence observations of the OGLE and MOA survey groups. Read More

2015Aug

We report the detection of a Cold Neptune m_planet=21+/-2MEarth orbiting a 0.38MSol M dwarf lying 2.5-3. Read More

To move one step forward toward a Galactic distribution of planets, we present the first planet sensitivity analysis for microlensing events with simultaneous observations from space and the ground. We present this analysis for two such events, OGLE-2014-BLG-0939 and OGLE-2014-BLG-0124, which both show substantial planet sensitivity even though neither of them reached high magnification. This suggests that an ensemble of low to moderate magnification events can also yield significant planet sensitivity and therefore probability to detect planets. Read More

We present Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) observations of the source and lens stars for planetary microlensing event OGLE-2005-BLG-169, which confirm the relative proper motion prediction due to the planetary light curve signal observed for this event. This (and the companion Keck result) provide the first confirmation of a planetary microlensing signal, for which the deviation was only 2%. The follow-up observations determine the flux of the planetary host star in multiple passbands and remove light curve model ambiguity caused by sparse sampling of part of the light curve. Read More

We report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet-star mass ratio ~1 x 10^{-3}. Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK'-band images obtained by the Subaru/AO188 and IRCS instruments, allowing us to constrain the absolute physical parameters of the planetary system. Read More

2015May
Affiliations: 1Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 2Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 3University of Canterbury, Dept. of Physics and Astronomy, New Zealand, 4Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 5Institute of Natural and Mathematical Sciences, Massey University, Auckland, New Zealand, 6Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 7Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 8Department of Physics, University of Notre Dame, 9SUPA, School of Physics & Astronomy, North Haugh, University of St Andrews, 10Kavli Institute for Astronomy and Astrophysics, Peking University, 11IRAP, CNRS - Université de Toulouse, 12Department of Astronomy, Ohio State University, 13School of Math and Physics, University of Tasmania, Australia, 14Niels Bohr Institutet, Københavns Universitet, Denmark, 15Space Telescope Science Institute, Baltimore, MD, 16South African Astronomical Observatory, South Africa, 17Department of Earth and Space Science, Osaka University, Japan, 18Qatar Environment and Energy Research Institute, Qatar Foundation, 19Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 20Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 21Department of Physics, University of Rijeka, Croatia, 22Technical University of Vienna, Department of Computing, 23Department of Astronomy, Ohio State University, 24Department of Physics, Chungbuk National University, Korea, 25SUPA, School of Physics & Astronomy, North Haugh, University of St Andrews, 26SUPA, School of Physics & Astronomy, North Haugh, University of St Andrews, 27Department of Physics and Astronomy, San Francisco State University, 28Korea Astronomy and Space Science Institute, Daejeon, Korea, 29Sorbonne Universités, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, 30Korea Astronomy and Space Science Institute, Daejeon, Korea, 31University of Canterbury, Dept. of Physics and Astronomy, New Zealand, 32Space Telescope Science Institute, Baltimore, MD, 33Las Cumbres Observatory Global Telescope Network, Goleta, CA, 34Las Cumbres Observatory Global Telescope Network, Goleta, CA, 35Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, 36Perth Observatory, Walnut Road, Bickley, Perth 6076, Australia, 37Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, 38Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 39Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, 40Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 41Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 42Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 43Solar-Terrestrial Environment Laboratory, Nagoya University, Japan, 44Nagano National College of Technology, Japan, 45Department of Physics, University of Auckland, New Zealand, 46Tokyo Metropolitan College of Aeronautics, Japan, 47School of Chemical and Physical Sciences, Victoria University, Wellington, New Zealand, 48Institute of Information and Mathematical Sciences, Massey University at Albany, Auckland, New Zealand, 49Mt. John University Observatory, Lake Tekapo, New Zealand, 50Department of Physics, University of Auckland, New Zealand, 51Department of Physics, Faculty of Science, Kyoto Sangyo University, Japan

We present the analysis of MOA-2007-BLG-197Lb, the first brown dwarf companion to a Sun-like star detected through gravitational microlensing. The event was alerted and followed-up photometrically by a network of telescopes from the PLANET, MOA, and uFUN collaborations, and observed at high angular resolution using the NaCo instrument at the VLT. From the modelling of the microlensing light curve, we derived the binary lens separation in Einstein radius units (s~1. Read More

We reanalyze microlensing events in the published list of anomalous events that were observed from the OGLE lensing survey conducted during 2004-2008 period. In order to check the existence of possible degenerate solutions and extract extra information, we conduct analyses based on combined data from other survey and follow-up observation and consider higher-order effects. Among the analyzed events, we present analyses of 8 events for which either new solutions are identified or additional information is obtained. Read More

Recently Sumi et al. (2011) reported evidence for a large population of planetary-mass objects (PMOs) that are either unbound or orbit host stars in orbits > 10 AU. Their result was deduced from the statistical distribution of durations of gravitational microlensing events observed by the MOA collaboration during 2006 and 2007. Read More

We present microlens parallax measurements for 21 (apparently) isolated lenses observed toward the Galactic bulge that were imaged simultaneously from Earth and Spitzer, which was ~1 AU West of Earth in projection. We combine these measurements with a kinematic model of the Galaxy to derive distance estimates for each lens, with error bars that are small compared to the Sun's Galactocentric distance. The ensemble therefore yields a well-defined cumulative distribution of lens distances. Read More

2014Oct
Authors: J. Skowron, I. -G. Shin, A. Udalski, C. Han, T. Sumi, Y. Shvartzvald, A. Gould, D. Dominis-Prester, R. A. Street, U. G. Jørgensen, D. P. Bennett, V. Bozza, M. K. Szymański, M. Kubiak, G. Pietrzyński, I. Soszyński, R. Poleski, S. Kozłowski, P. Pietrukowicz, K. Ulaczyk, Ł. Wyrzykowski, F. Abe, A. Bhattacharya, I. A. Bond, C. S. Botzler, M. Freeman, A. Fukui, D. Fukunaga, Y. Itow, C. H. Ling, N. Koshimoto, K. Masuda, Y. Matsubara, Y. Muraki, S. Namba, K. Ohnishi, L. C. Philpott, N. Rattenbury, T. Saito, D. J. Sullivan, D. Suzuki, P. J. Tristram, P. C. M. Yock, D. Maoz, S. Kaspi, M. Friedman, L. A. Almeida, V. Batista, G. Christie, J. -Y. Choi, D. L. DePoy, B. S. Gaudi, C. Henderson, K. -H. Hwang, F. Jablonski, Y. K. Jung, C. -U. Lee, J. McCormick, T. Natusch, H. Ngan, H. Park, R. W. Pogge, J. Yee, M. D. Albrow, E. Bachelet, J. -P. Beaulieu, S. Brillant, J. A. R. Caldwell, A. Cassan, A. Cole, E. Corrales, Ch. Coutures, S. Dieters, J. Donatowicz, P. Fouqué, J. Greenhill, N. Kains, S. R. Kane, D. Kubas, J. -B. Marquette, R. Martin, J. Menzies, K. R. Pollard, C. Ranc, K. C. Sahu, J. Wambsganss, A. Williams, D. Wouters, Y. Tsapras, D. M. Bramich, K. Horne, M. Hundertmark, C. Snodgrass, I. A. Steele, K. A. Alsubai, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, M. Dominik, S. Dreizler, X. -S. Fang, C. -H. Gu, Hardis, K. Harpsøe, F. V. Hessman, T. C. Hinse, A. Hornstrup, J. Jessen-Hansen, E. Kerins, C. Liebig, M. Lund, M. Lundkvist, L. Mancini, M. Mathiasen, M. T. Penny, S. Rahvar, D. Ricci, G. Scarpetta, J. Skottfelt, J. Southworth, J. Surdej, J. Tregloan-Reed, O. Wertz

We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal combined with extended observations throughout the event allows us to accurately model the observed light curve. Read More

The mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lens-source proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. Read More

Characterizing a microlensing planet is done from modeling an observed lensing light curve. In this process, it is often confronted that solutions of different lensing parameters result in similar light curves, causing difficulties in uniquely interpreting the lens system, and thus understanding the causes of different types of degeneracy is important. In this work, we show that incomplete coverage of a planetary perturbation can result in degenerate solutions even for events where the planetary signal is detected with a high level of statistical significance. Read More

We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M_host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The data are well fit by this exomoon model, but an alternate star+planet model fits the data almost as well. Nevertheless, these results indicate the potential of microlensing to detect exomoons, albeit ones that are different from the giant planet moons in our solar system. Read More

We report analysis of high microlensing event MOA-2008-BLG-379, which has a strong microlensing anomaly at its peak, due to a massive planet with a mass ratio of q = 6.9 x 10^{-3}. Because the faint source star crosses the large resonant caustic, the planetary signal dominates the light curve. Read More

2013Oct
Authors: 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 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, allowed us to accurately measure the parallax effect and lens orbital motion. Combining our measurement of the lens parallax with the angular Einstein radius determined from finite-source effects, we estimate the physical parameters of the lens system. Read More

Global "second-generation" microlensing surveys aim to discover and characterize extrasolar planets and their frequency, by means of round-the-clock high-cadence monitoring of a large area of the Galactic bulge, in a controlled experiment. We report the discovery of a giant planet in microlensing event MOA-2011-BLG-322. This moderate-magnification event, which displays a clear anomaly induced by a second lensing mass, was inside the footprint of our second-generation microlensing survey, involving MOA, OGLE and the Wise Observatory. Read More

2013Sep
Authors: K. Furusawa, A. Udalski, T. Sumi, D. P. Bennett, I. A. Bond, A. Gould, U. G. Jorgensen, C. Snodgrass, D. Dominis Prester, M. D. Albrow, F. Abe, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, P. Harris, Y. Itow, C. H. Ling, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, K. Ohnishi, N. J. Rattenbury, To. Saito, D. J. Sullivan, D. Suzuki, W. L. Sweatman, P. J. Tristram, K. Wada, P. C. M. Yock, M. K. Szymanski, I. Soszynski, M. Kubiak, R. Poleski, K. Ulaczyk, G. Pietrzynski, L. Wyrzykowski, J. Y. Choi, G. W. Christie, D. L. DePoy, S. Dong, J. Drummond, B. S. Gaudi, C. Han, L. -W. Hung, Y. -K. Jung, C. -U. Lee, J. McCormick, D. Moorhouse, T. Natusch, M. Nola, E. Ofek, B. G. Park, H. Park, R. W. Pogge, I. -G. Shin, J. Skowron, G. Thornley, J. C. Yee, K. A. Alsubai, V. Bozza, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, M. Dominik, F. Finet, T. Gerner, S. Hardis, K. Harpsoe, T. C. Hinse, M. Hundertmark, N. Kains, E. Kerins, C. Liebig, L. Mancini, M. Mathiasen, M. T. Penny, S. Proft, S. Rahvar, D. Ricci, G. Scarpetta, S. Schafer, F. Schonebeck, J. Southworth, J. Surdej, J. Wambsganss, R. A. Street, D. M. Bramich, I. A. Steele, Y. Tsapras, K. Horne, J. Donatowicz, K. C. Sahu, E. Bachelet, V. Batista, T. G. Beatty, J. -P. Beaulieu, C. S. Bennett, C. Black, R. Bowens-Rubin, S. Brillant, J. A. R. Caldwell, A. Cassan, A. A. Cole, E. Corrales, C. Coutures, S. Dieters, P. Fouque, J. Greenhill, C. B. Henderson, D. Kubas, J. -B. Marquette, R. Martin, J. W. Menzies, B. Shappee, A. Williams, D. Wouters, J. van Saders, R. Zellem, M. Zub

We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of Mh = 0.11+/-0. Read More

A planetary microlensing signal is generally characterized by a short-term perturbation to the standard single lensing light curve. A subset of binary-source events can produce perturbations that mimic planetary signals, thereby introducing an ambiguity between the planetary and binary-source interpretations. In this paper, we present analysis of the microlensing event MOA-2012-BLG-486, for which the light curve exhibits a short-lived perturbation. Read More

Observations of accretion disks around young brown dwarfs have led to the speculation that they may form planetary systems similar to normal stars. While there have been several detections of planetary-mass objects around brown dwarfs (2MASS 1207-3932 and 2MASS 0441-2301), these companions have relatively large mass ratios and projected separations, suggesting that they formed in a manner analogous to stellar binaries. We present the discovery of a planetary-mass object orbiting a field brown dwarf via gravitational microlensing, OGLE-2012-BLG-0358Lb. Read More

We present measurements of the microlensing optical depth and event rate toward the Galactic Bulge based on two years of the MOA-II survey. This sample contains ~1000 microlensing events, with an Einstein Radius crossing time of t_E < 200 days between -5 Read More

2013Mar
Authors: N. Kains, R. Street, J. -Y. Choi, C. Han, A. Udalski, L. A. Almeida, F. Jablonski, P. Tristram, U. G. Jorgensen, M. K. Szymanski, M. Kubiak, G. Pietrzynski, I. Soszynski, R. Poleski, S. Kozlowski, P. Pietrukowicz, K. Ulaczyk, L. Wyrzykowski, J. Skowron, K. A. Alsubai, V. Bozza, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, M. Dominik, S. Dreizler, X. -S. Fang, F. Grundahl, C. -H. Gu, S. Hardis, K. Harpsoe, F. V. Hessman, T. C. Hinse, A. Hornstrup, M. Hundertmark, J. Jessen-Hansen, E. Kerins, C. Liebig, M. Lund, M. Lundkvist, L. Mancini, M. Mathiasen, M. T. Penny, S. Rahvar, D. Ricci, K. C. Sahu, G. Scarpetta, J. Skottfelt, C. Snodgrass, J. Southworth, J. Surdej, J. Tregloan-Reed, J. Wambsganss, O. Wertz, D. Bajek, D. M. Bramich, K. Horne, S. Ipatov, I. A. Steele, Y. Tsapras, F. Abe, D. P. Bennett, I. A. Bond, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, K. Furusawa, Y. Itow, C. H. Ling, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, K. Ohnishi, N. Rattenbury, T. Saito, D. J. Sullivan, T. Sumi, D. Suzuki, K. Suzuki, W. L. Sweatman, S. Takino, K. Wada, P. C. M. Yock, W. Allen, V. Batista, S. -J. Chung, G. Christie, D. L. DePoy, J. Drummond, B. S. Gaudi, A. Gould, C. Henderson, Y. -K. Jung, J. -R. Koo, C. -U. Lee, J. McCormick, D. McGregor, J. A. Munoz, T. Natusch, H. Ngan, H. Park, R. W. Pogge, I. -G. Shin, J. Yee, M. D. Albrow, E. Bachelet, J. -P. Beaulieu, S. Brillant, J. A. R. Caldwell, A. Cassan, A. Cole, E. Corrales, Ch. Coutures, S. Dieters, D. Dominis Prester, J. Donatowicz, P. Fouque, J. Greenhill, S. R. Kane, D. Kubas, J. -B. Marquette, R. Martin, P. Meintjes, J. Menzies, K. R. Pollard, A. Williams, D. Wouters, M. Zub

We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic Bulge. Based on detailed modelling of the observed light curve, we find that the lens is composed of two masses with a mass ratio q=1. Read More

2013Feb
Authors: J. -Y. Choi, C. Han, A. Udalski, T. Sumi, B. S. Gaudi, A. Gould, D. P. Bennett, M. Dominik, J. -P. Beaulieu, Y. Tsapras, V. Bozza, F. Abe, I. A. Bond, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, K. Furusawa, Y. Itow, C. H. Ling, K. Masuda, Y. Matsubara, N. Miyake, Y. Muraki, K. Ohnishi, N. J. Rattenbury, To. Saito, D. J. Sullivan, K. Suzuki, W. L. Sweatman, D. Suzuki, S. Takino, P. J. Tristram, K. Wada, P. C. M. Yock, M. K. Szymański, M. Kubiak, G. Pietrzyński, I. Soszyński, J. Skowron, S. Kozłowski, R. Poleski, K. Ulaczyk, Ł. Wyrzykowski, P. Pietrukowicz, L. A. Almeida, D. L. DePoy, Subo Dong, E. Gorbikov, F. Jablonski, C. B. Henderson, K. -H. Hwang, J. Janczak, Y. -K. Jung, S. Kaspi, C. -U. Lee, U. Malamud, D. Maoz, D. McGregor, J. A. Munoz, B. -G. Park, H. Park, R. W. Pogge, Y. Shvartzvald, I. -G. Shin, J. C. Yee, K. A. Alsubai, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, X. -S. Fang, F. Finet, M. Glitrup, F. Grundahl, S. -H. Gu, S. Hardis, K. Harpsøe, T. C. Hinse, A. Hornstrup, M. Hundertmark, J. Jessen-Hansen, U. G. Jørgensen, N. Kains, E. Kerins, C. Liebig, M. N. Lund, M. Lundkvist, G. Maier, L. Mancini, M. Mathiasen, M. T. Penny, S. Rahvar, D. Ricci, G. Scarpetta, J. Skottfelt, C. Snodgrass, J. Southworth, J. Surdej, J. Tregloan-Reed, J. Wambsganss, O. Wertz, F. Zimmer, M. D. Albrow, E. Bachelet, V. Batista, S. Brillant, A. Cassan, A. A. Cole, C. Coutures, S. Dieters, D. Dominis Prester, J. Donatowicz, P. Fouqué, J. Greenhill, D. Kubas, J. -B. Marquette, J. W. Menzies, K. C. Sahu, M. Zub, D. M. Bramich, K. Horne, I. A. Steele, R. A. Street

Although many models have been proposed, the physical mechanisms responsible for the formation of low-mass brown dwarfs are poorly understood. The multiplicity properties and minimum mass of the brown-dwarf mass function provide critical empirical diagnostics of these mechanisms. We present the discovery via gravitational microlensing of two very low-mass, very tight binary systems. Read More

Based on high-resolution spectra obtained during gravitational microlensing events we present a detailed elemental abundance analysis of 32 dwarf and subgiant stars in the Galactic bulge. [ABRIDGED], we now have 58 microlensed bulge dwarfs and subgiants that have been homogeneously analysed. The main characteristics of the sample and the findings that can be drawn are: (i) The metallicity distribution (MDF) is wide and spans all metallicities between [Fe/H]=-1. Read More

2012Nov
Authors: R. A. Street1, J. -Y. Choi2, Y. Tsapras3, C. Han4, K. Furusawa5, M. Hundertmark6, A. Gould7, T. Sumi8, I. A. Bond9, D. Wouters10, R. Zellem11, A. Udalski12, C. Snodgrass13, K. Horne14, M. Dominik15, P. Browne16, N. Kains17, D. M. Bramich18, D. Bajek19, I. A. Steele20, S. Ipatov21, F. Abe22, D. P. Bennett23, C. S. Botzler24, P. Chote25, M. Freeman26, A. Fukui27, P. Harris28, Y. Itow29, C. H. Ling30, K. Masuda31, Y. Matsubara32, N. Miyake33, Y. Muraki34, T. Nagayama35, S. Nishimaya36, K. Ohnishi37, N. Rattenbury38, To. Saito39, D. J. Sullivan40, D. Suzuki41, W. L. Sweatman42, P. J. Tristram43, K. Wada44, P. C. M. Yock45, M. K. Szymanski46, M. Kubiak47, G. Pietrzynski48, I. Soszynski49, R. Poleski50, K. Ulaczyk51, L. Wyrzykowski52, J. Yee53, S. Dong54, I. -G. Shin55, C. -U. Lee56, J. Skowron57, L. Andrade De Almeida58, D. L. DePoy59, B. S. Gaudi60, L. -W. Hung61, F. Jablonski62, S. Kaspi63, N. Klein64, K. -H. Hwang65, J. -R. Koo66, D. Maoz67, J. A. Munoz68, R. W. Pogge69, D. Polishhook70, A. Shporer71, J. McCormick72, G. Christie73, T. Natusch74, B. Allen75, J. Drummond76, D. Moorhouse77, G. Thornley78, M. Knowler79, M. Bos80, G. Bolt81, J. -P. Beaulieu82, M. D. Albrow83, V. Batista84, S. Brillant85, J. A. R. Caldwell86, A. Cassan87, A. Cole88, E. Corrales89, Ch. Coutures90, S. Dieters91, D. Dominis Prester92, J. Donatowicz93, P. Fouque94, E. Bachelet95, J. Greenhill96, S. R. Kane97, D. Kubas98, J. -B. Marquette99, R. Martin100, J. Menzies101, K. R. Pollard102, K. C. Sahu103, J. Wambsganss104, A. Williams105, M. Zub106, K. A. Alsubai, V. Bozza, M. J. Burgdorf, S. Calchi Novati, P. Dodds, S. Dreizler, F. Finet, T. Gerner, S. Hardis, K. Harpsoe, F. Hessman, T. C. Hinse, U. G. Jorgensen, E. Kerins, C. Liebig, L. Mancini, M. Mathiasen, M. T. Penny, S. Proft, S. Rahvar, D. Ricci, G. Scarpetta, S. Schafer, F. Schonebeck, J. Southworth, J. Surdej
Affiliations: 1The RoboNet Collaboration, 2The RoboNet Collaboration, 3The RoboNet Collaboration, 4The RoboNet Collaboration, 5The RoboNet Collaboration, 6The RoboNet Collaboration, 7The RoboNet Collaboration, 8The RoboNet Collaboration, 9The RoboNet Collaboration, 10The RoboNet Collaboration, 11The RoboNet Collaboration, 12The RoboNet Collaboration, 13The MOA Collaboration, 14The MOA Collaboration, 15The MOA Collaboration, 16The MOA Collaboration, 17The MOA Collaboration, 18The MOA Collaboration, 19The MOA Collaboration, 20The MOA Collaboration, 21The MOA Collaboration, 22The OGLE Collaboration, 23The OGLE Collaboration, 24The OGLE Collaboration, 25The OGLE Collaboration, 26The OGLE Collaboration, 27The OGLE Collaboration, 28The OGLE Collaboration, 29The OGLE Collaboration, 30The OGLE Collaboration, 31The OGLE Collaboration, 32The OGLE Collaboration, 33The OGLE Collaboration, 34The OGLE Collaboration, 35The OGLE Collaboration, 36The OGLE Collaboration, 37The OGLE Collaboration, 38The OGLE Collaboration, 39The OGLE Collaboration, 40The OGLE Collaboration, 41The OGLE Collaboration, 42The OGLE Collaboration, 43The OGLE Collaboration, 44The OGLE Collaboration, 45The OGLE Collaboration, 46The MicroFUN Collaboration, 47The MicroFUN Collaboration, 48The MicroFUN Collaboration, 49The MicroFUN Collaboration, 50The MicroFUN Collaboration, 51The MicroFUN Collaboration, 52The MicroFUN Collaboration, 53The PLANET Collaboration, 54The PLANET Collaboration, 55The PLANET Collaboration, 56The PLANET Collaboration, 57The PLANET Collaboration, 58The PLANET Collaboration, 59The PLANET Collaboration, 60The PLANET Collaboration, 61The PLANET Collaboration, 62The PLANET Collaboration, 63The PLANET Collaboration, 64The PLANET Collaboration, 65The PLANET Collaboration, 66The PLANET Collaboration, 67The PLANET Collaboration, 68The PLANET Collaboration, 69The PLANET Collaboration, 70The PLANET Collaboration, 71The PLANET Collaboration, 72The PLANET Collaboration, 73The PLANET Collaboration, 74The PLANET Collaboration, 75The PLANET Collaboration, 76The PLANET Collaboration, 77The PLANET Collaboration, 78The PLANET Collaboration, 79The PLANET Collaboration, 80The PLANET Collaboration, 81The PLANET Collaboration, 82MiNDSTEp, 83MiNDSTEp, 84MiNDSTEp, 85MiNDSTEp, 86MiNDSTEp, 87MiNDSTEp, 88MiNDSTEp, 89MiNDSTEp, 90MiNDSTEp, 91MiNDSTEp, 92MiNDSTEp, 93MiNDSTEp, 94MiNDSTEp, 95MiNDSTEp, 96MiNDSTEp, 97MiNDSTEp, 98MiNDSTEp, 99MiNDSTEp, 100MiNDSTEp, 101MiNDSTEp, 102MiNDSTEp, 103MiNDSTEp, 104MiNDSTEp, 105MiNDSTEp, 106MiNDSTEp

We present an analysis of the anomalous microlensing event, MOA-2010-BLG-073, announced by the Microlensing Observations in Astrophysics survey on 2010-03-18. This event was remarkable because the source was previously known to be photometrically variable. Analyzing the pre-event source lightcurve, we demonstrate that it is an irregular variable over time scales >200d. Read More

2012Oct
Authors: J. C. Yee1, L. -W. Hung2, I. A. Bond3, W. Allen4, L. A. G. Monard5, M. D. Albrow6, P. Fouque7, M. Dominik8, Y. Tsapras9, A. Udalski10, A. Gould11, R. Zellem12, M. Bos13, G. W. Christie14, D. L. DePoy15, Subo Dong16, J. Drummond17, B. S. Gaudi18, E. Gorbikov19, C. Han20, S. Kaspi21, N. Klein22, C. -U. Lee23, D. Maoz24, J. McCormick25, D. Moorhouse26, T. Natusch27, M. Nola28, B. -G. Park29, R. W. Pogge30, D. Polishook31, A. Shporer32, Y. Shvartzvald33, J. Skowron34, G. Thornley35, F. Abe36, D. P. Bennett37, C. S. Botzler38, P. Chote39, M. Freeman40, A. Fukui41, K. Furusawa42, P. Harris43, Y. Itow44, C. H. Ling45, K. Masuda46, Y. Matsubara47, N. Miyake48, K. Ohnishi49, N. J. Rattenbury50, To. Saito51, D. J. Sullivan52, T. Sumi53, D. Suzuki54, W. L. Sweatman55, P. J. Tristram56, K. Wada57, P. C. M. Yock58, M. K. Szymanski59, I. Soszynski60, M. Kubiak61, R. Poleski62, K. Ulaczyk63, G. Pietrzynski64, L. Wyrzykowski65, E. Bachelet66, V. Batista67, T. G. Beatty68, J. -P. Beaulieu69, C. S. Bennett70, R. Bowens-Rubin71, S. Brillant72, J. A. R. Caldwell73, A. Cassan74, A. A. Cole75, E. Corrales76, C. Coutures77, S. Dieters78, D. Dominis Prester79, J. Donatowicz80, J. Greenhill81, C. B. Henderson82, D. Kubas83, J. -B. Marquette84, R. Martin85, J. W. Menzies86, B. Shappee87, A. Williams88, D. Wouters89, J. van Saders90, M. Zub91, R. A. Street92, K. Horne93, D. M. Bramich94, I. A. Steele95, K. A. Alsubai96, V. Bozza97, P. Browne98, M. J. Burgdorf99, S. Calchi Novati100, P. Dodds101, F. Finet102, T. Gerner103, S. Hardis104, K. Harpsoe105, F. V. Hessman106, T. C. Hinse107, M. Hundertmark108, U. G. Jorgensen109, N. Kains110, E. Kerins111, C. Liebig112, L. Mancini113, M. Mathiasen114, M. T. Penny115, S. Proft116, S. Rahvar117, D. Ricci118, K. C. Sahu119, G. Scarpetta120, S. Schafer121, F. Schonebeck122, C. Snodgrass123, J. Southworth124, J. Surdej125, J. Wambsgans126
Affiliations: 1The uFUN Collaboration, 2The uFUN Collaboration, 3The uFUN Collaboration, 4The uFUN Collaboration, 5The uFUN Collaboration, 6The uFUN Collaboration, 7The uFUN Collaboration, 8The uFUN Collaboration, 9The uFUN Collaboration, 10The uFUN Collaboration, 11The uFUN Collaboration, 12The uFUN Collaboration, 13The uFUN Collaboration, 14The uFUN Collaboration, 15The uFUN Collaboration, 16The uFUN Collaboration, 17The uFUN Collaboration, 18The uFUN Collaboration, 19The uFUN Collaboration, 20The uFUN Collaboration, 21The uFUN Collaboration, 22The uFUN Collaboration, 23The uFUN Collaboration, 24The uFUN Collaboration, 25The uFUN Collaboration, 26The uFUN Collaboration, 27The uFUN Collaboration, 28The uFUN Collaboration, 29The uFUN Collaboration, 30The uFUN Collaboration, 31The uFUN Collaboration, 32The uFUN Collaboration, 33The uFUN Collaboration, 34The uFUN Collaboration, 35The uFUN Collaboration, 36The MOA Collaboration, 37The MOA Collaboration, 38The MOA Collaboration, 39The MOA Collaboration, 40The MOA Collaboration, 41The MOA Collaboration, 42The MOA Collaboration, 43The MOA Collaboration, 44The MOA Collaboration, 45The MOA Collaboration, 46The MOA Collaboration, 47The MOA Collaboration, 48The MOA Collaboration, 49The MOA Collaboration, 50The MOA Collaboration, 51The MOA Collaboration, 52The MOA Collaboration, 53The MOA Collaboration, 54The MOA Collaboration, 55The MOA Collaboration, 56The MOA Collaboration, 57The MOA Collaboration, 58The MOA Collaboration, 59The OGLE Collaboration, 60The OGLE Collaboration, 61The OGLE Collaboration, 62The OGLE Collaboration, 63The OGLE Collaboration, 64The OGLE Collaboration, 65The OGLE Collaboration, 66The PLANET Collaboration, 67The PLANET Collaboration, 68The PLANET Collaboration, 69The PLANET Collaboration, 70The PLANET Collaboration, 71The PLANET Collaboration, 72The PLANET Collaboration, 73The PLANET Collaboration, 74The PLANET Collaboration, 75The PLANET Collaboration, 76The PLANET Collaboration, 77The PLANET Collaboration, 78The PLANET Collaboration, 79The PLANET Collaboration, 80The PLANET Collaboration, 81The PLANET Collaboration, 82The PLANET Collaboration, 83The PLANET Collaboration, 84The PLANET Collaboration, 85The PLANET Collaboration, 86The PLANET Collaboration, 87The PLANET Collaboration, 88The PLANET Collaboration, 89The PLANET Collaboration, 90The PLANET Collaboration, 91The PLANET Collaboration, 92The RoboNet Collaboration, 93The RoboNet Collaboration, 94The RoboNet Collaboration, 95The RoboNet Collaboration, 96The MiNDSTEp Consortium, 97The MiNDSTEp Consortium, 98The MiNDSTEp Consortium, 99The MiNDSTEp Consortium, 100The MiNDSTEp Consortium, 101The MiNDSTEp Consortium, 102The MiNDSTEp Consortium, 103The MiNDSTEp Consortium, 104The MiNDSTEp Consortium, 105The MiNDSTEp Consortium, 106The MiNDSTEp Consortium, 107The MiNDSTEp Consortium, 108The MiNDSTEp Consortium, 109The MiNDSTEp Consortium, 110The MiNDSTEp Consortium, 111The MiNDSTEp Consortium, 112The MiNDSTEp Consortium, 113The MiNDSTEp Consortium, 114The MiNDSTEp Consortium, 115The MiNDSTEp Consortium, 116The MiNDSTEp Consortium, 117The MiNDSTEp Consortium, 118The MiNDSTEp Consortium, 119The MiNDSTEp Consortium, 120The MiNDSTEp Consortium, 121The MiNDSTEp Consortium, 122The MiNDSTEp Consortium, 123The MiNDSTEp Consortium, 124The MiNDSTEp Consortium, 125The MiNDSTEp Consortium, 126The MiNDSTEp Consortium

We analyze MOA-2010-BLG-311, a high magnification (A_max>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 2-body lens model and find that the 2-body lens model is a better fit but with only Delta chi^2~80. The preferred mass ratio between the lens star and its companion is $q=10^(-3. Read More

2012Oct
Authors: A. Gould1, J. C. Yee2, I. A. Bond3, A. Udalski4, C. Han5, U. G. Jorgensen6, J. Greenhill7, Y. Tsapras8, M. H. Pinsonneault9, T. Bensby10, W. Allen11, L. A. Almeida12, M. Bos13, G. W. Christie14, D. L. DePoy15, Subo Dong16, B. S. Gaudi17, L. -W. Hung18, F. Jablonski19, C. -U. Lee20, J. McCormick21, D. Moorhouse22, J. A. Munoz23, T. Natusch24, M. Nola25, R. W. Pogge26, J. Skowron27, G. Thornley28, F. Abe29, D. P. Bennett30, C. S. Botzler31, P. Chote32, M. Freeman33, A. Fukui34, K. Furusawa35, P. Harris36, Y. Itow37, C. H. Ling38, K. Masuda39, Y. Matsubara40, N. Miyake41, K. Ohnishi42, N. J. Rattenbury43, To. Saito44, D. J. Sullivan45, T. Sumi46, D. Suzuki47, W. L. Sweatman48, P. J. Tristram49, K. Wada50, P. C. M. Yock51, M. K. Szymanski52, I. Soszynski53, M. Kubiak54, R. Poleski55, K. Ulaczyk56, G. Pietrzynski57, L. Wyrzykowski58, K. A. Alsubai59, V. Bozza60, P. Browne61, M. J. Burgdorf62, S. Calchi Novati63, P. Dodds64, M. Dominik65, F. Finet66, T. Gerner67, S. Hardis68, K. Harpsoe69, F. V. Hessman70, T. C. Hinse71, M. Hundertmark72, N. Kains73, E. Kerins74, C. Liebig75, L. Mancini76, M. Mathiasen77, M. T. Penny78, S. Proft79, S. Rahvar80, D. Ricci81, K. C. Sahu82, G. Scarpetta83, S. Schafer84, F. Schonebeck85, C. Snodgrass86, J. Southworth87, J. Surdej88, J. Wambsganss89, R. A. Street90, K. Horne91, D. M. Bramich92, I. A. Steele93, M. D. Albrow94, E. Bachelet95, V. Batista96, T. G. Beatty97, J. -P. Beaulieu98, C. S. Bennett99, R. Bowens-Rubin100, S. Brillant101, J. A. R. Caldwell102, A. Cassan103, A. A. Cole104, E. Corrales105, C. Coutures106, S. Dieters107, D. Dominis Prester108, J. Donatowicz109, P. Fouque110, C. B. Henderson111, D. Kubas112, J. -B Marquette113, R. Martin114, J. W. Menzies115, B. Shappee116, A. Williams117, J. van Saders118, M. Zub119
Affiliations: 1OSU, 2OSU, 3Massey U., 4Warsaw Obs., 5Chungbuk Nat. U., 6Niels Bohr Inst., 7U. of Tasmania, 8LCOGT, 9OSU, 10Lund Obs., 11The uFUN Collaboration, 12The uFUN Collaboration, 13The uFUN Collaboration, 14The uFUN Collaboration, 15The uFUN Collaboration, 16The uFUN Collaboration, 17The uFUN Collaboration, 18The uFUN Collaboration, 19The uFUN Collaboration, 20The uFUN Collaboration, 21The uFUN Collaboration, 22The uFUN Collaboration, 23The uFUN Collaboration, 24The uFUN Collaboration, 25The uFUN Collaboration, 26The uFUN Collaboration, 27The uFUN Collaboration, 28The uFUN Collaboration, 29The OGLE Collaboration, 30The OGLE Collaboration, 31The OGLE Collaboration, 32The OGLE Collaboration, 33The OGLE Collaboration, 34The OGLE Collaboration, 35The OGLE Collaboration, 36The OGLE Collaboration, 37The OGLE Collaboration, 38The OGLE Collaboration, 39The OGLE Collaboration, 40The OGLE Collaboration, 41The OGLE Collaboration, 42The OGLE Collaboration, 43The OGLE Collaboration, 44The OGLE Collaboration, 45The OGLE Collaboration, 46The OGLE Collaboration, 47The OGLE Collaboration, 48The OGLE Collaboration, 49The OGLE Collaboration, 50The OGLE Collaboration, 51The OGLE Collaboration, 52The OGLE Collaboration, 53The OGLE Collaboration, 54The OGLE Collaboration, 55The OGLE Collaboration, 56The OGLE Collaboration, 57The OGLE Collaboration, 58The OGLE Collaboration, 59The MiNDSTEp Consortium, 60The MiNDSTEp Consortium, 61The MiNDSTEp Consortium, 62The MiNDSTEp Consortium, 63The MiNDSTEp Consortium, 64The MiNDSTEp Consortium, 65The MiNDSTEp Consortium, 66The MiNDSTEp Consortium, 67The MiNDSTEp Consortium, 68The MiNDSTEp Consortium, 69The MiNDSTEp Consortium, 70The MiNDSTEp Consortium, 71The MiNDSTEp Consortium, 72The MiNDSTEp Consortium, 73The MiNDSTEp Consortium, 74The MiNDSTEp Consortium, 75The MiNDSTEp Consortium, 76The MiNDSTEp Consortium, 77The MiNDSTEp Consortium, 78The MiNDSTEp Consortium, 79The MiNDSTEp Consortium, 80The MiNDSTEp Consortium, 81The MiNDSTEp Consortium, 82The MiNDSTEp Consortium, 83The MiNDSTEp Consortium, 84The MiNDSTEp Consortium, 85The MiNDSTEp Consortium, 86The MiNDSTEp Consortium, 87The MiNDSTEp Consortium, 88The MiNDSTEp Consortium, 89The MiNDSTEp Consortium, 90The RoboNet Collaboration, 91The RoboNet Collaboration, 92The RoboNet Collaboration, 93The RoboNet Collaboration, 94The PLANET Collaboration, 95The PLANET Collaboration, 96The PLANET Collaboration, 97The PLANET Collaboration, 98The PLANET Collaboration, 99The PLANET Collaboration, 100The PLANET Collaboration, 101The PLANET Collaboration, 102The PLANET Collaboration, 103The PLANET Collaboration, 104The PLANET Collaboration, 105The PLANET Collaboration, 106The PLANET Collaboration, 107The PLANET Collaboration, 108The PLANET Collaboration, 109The PLANET Collaboration, 110The PLANET Collaboration, 111The PLANET Collaboration, 112The PLANET Collaboration, 113The PLANET Collaboration, 114The PLANET Collaboration, 115The PLANET Collaboration, 116The PLANET Collaboration, 117The PLANET Collaboration, 118The PLANET Collaboration, 119The PLANET Collaboration

The Galactic bulge source MOA-2010-BLG-523S exhibited short-term deviations from a standard microlensing lightcurve near the peak of an Amax ~ 265 high-magnification microlensing event. The deviations originally seemed consistent with expectations for a planetary companion to the principal lens. We combine long-term photometric monitoring with a previously published high-resolution spectrum taken near peak to demonstrate that this is an RS CVn variable, so that planetary microlensing is not required to explain the lightcurve deviations. Read More

Microlensing can provide an important tool to study binaries, especially those composed of faint or dark objects. However, accurate analysis of binary-lens light curves is often hampered by the well-known degeneracy between close (s<1) and wide (s>1) binaries, which can be very severe due to an intrinsic symmetry in the lens equation. Here s is the normalized projected binary separation. Read More

2012Aug
Authors: 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

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 companions that are found by analyzing binary microlensing events discovered during 2004 - 2011 observation seasons. Based on the low mass ratio criterion of q < 0. Read More

2012Jul
Affiliations: 1The OGLE Collaboration, 2The OGLE Collaboration, 3The OGLE Collaboration, 4The OGLE Collaboration, 5The OGLE Collaboration, 6The OGLE Collaboration, 7The OGLE Collaboration, 8The OGLE Collaboration, 9The OGLE Collaboration, 10The OGLE Collaboration, 11The OGLE Collaboration, 12The OGLE Collaboration, 13The OGLE Collaboration, 14The OGLE Collaboration, 15The OGLE Collaboration, 16The MOA Collaboration, 17The MOA Collaboration, 18The MOA Collaboration, 19The MOA Collaboration, 20The MOA Collaboration, 21The MOA Collaboration, 22The MOA Collaboration, 23The MOA Collaboration, 24The MOA Collaboration, 25The MOA Collaboration, 26The MOA Collaboration, 27The MOA Collaboration, 28The MOA Collaboration, 29The MOA Collaboration, 30The MOA Collaboration, 31The MOA Collaboration, 32The MOA Collaboration, 33The MOA Collaboration, 34The MOA Collaboration, 35The muFUN Collaboration, 36The muFUN Collaboration, 37The muFUN Collaboration, 38The muFUN Collaboration, 39The muFUN Collaboration, 40The muFUN Collaboration, 41The muFUN Collaboration, 42The muFUN Collaboration, 43The muFUN Collaboration, 44The muFUN Collaboration, 45The muFUN Collaboration, 46The RoboNet Collaboration, 47The RoboNet Collaboration, 48The RoboNet Collaboration, 49The RoboNet Collaboration, 50The RoboNet Collaboration, 51The RoboNet Collaboration, 52The RoboNet Collaboration, 53The RoboNet Collaboration, 54The RoboNet Collaboration, 55The RoboNet Collaboration, 56The RoboNet Collaboration, 57The PLANET Collaboration, 58The PLANET Collaboration, 59The PLANET Collaboration, 60The PLANET Collaboration, 61The PLANET Collaboration, 62The PLANET Collaboration, 63The PLANET Collaboration, 64The PLANET Collaboration, 65The PLANET Collaboration, 66The PLANET Collaboration, 67The PLANET Collaboration, 68The PLANET Collaboration, 69The PLANET Collaboration, 70The PLANET Collaboration, 71The PLANET Collaboration, 72The PLANET Collaboration, 73The PLANET Collaboration, 74The PLANET Collaboration, 75The PLANET Collaboration, 76The PLANET Collaboration, 77The PLANET Collaboration, 78The PLANET Collaboration, 79The PLANET Collaboration, 80The PLANET Collaboration, 81The PLANET Collaboration

We report the extremely high magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q = 0. Read More

2012May
Authors: E. Bachelet, I. -G. Shin, C. Han, P. Fouqué, A. Gould, J. W. Menzies, J. -P. Beaulieu, D. P. Bennett, I. A. Bond, Subo Dong, D. Heyrovský, J. B. Marquette, J. Marshall, J. Skowron, R. A. Street, T. Sumi, A. Udalski, L. Abe, K. Agabi, M. D. Albrow, W. Allen, E. Bertin, M. Bos, D. M. Bramich, J. Chavez, G. W. Christie, A. A. Cole, N. Crouzet, S. Dieters, M. Dominik, J. Drummond, J. Greenhill, T. Guillot, C. B. Henderson, F. V. Hessman, K. Horne, M. Hundertmark, J. A. Johnson, U. G. Jørgensen, R. Kandori, C. Liebig, D. Mékarnia, J. McCormick, D. Moorhouse, T. Nagayama, D. Nataf, T. Natusch, S. Nishiyama, J. -P. Rivet, K. C. Sahu, Y. Shvartzvald, G. Thornley, A. R. Tomczak, Y. Tsapras, J. C. Yee, V. Batista, C. S. Bennett, S. Brillant, J. A. R. Caldwell, A. Cassan, E. Corrales, C. Coutures, D. Dominis Prester, J. Donatowicz, D. Kubas, R. Martin, A. Williams, M. Zub, L. Andrade de Almeida, D. L. DePoy, B. S. Gaudi, L. -W. Hung, F. Jablonski, S. Kaspi, N. Klein, C. -U. Lee, Y. Lee, J. -R. Koo, D. Maoz, J. A. Muñoz, R. W. Pogge, D. Polishook, A. Shporer, F. Abe, C. S. Botzler, P. Chote, M. Freeman, A. Fukui, K. Furusawa, P. Harris, Y. Itow, S. Kobara, C. H. Ling, K. Masuda, Y. Matsubara, N. Miyake, K. Ohmori, K. Ohnishi, N. J. Rattenbury, To. Saito, D. J. Sullivan, D. Suzuki, W. L. Sweatman, P. J. Tristram, K. Wada, P. C. M. Yock, M. K. Szymański, I. Soszyński, M. Kubiak, R. Poleski, K. Ulaczyk, G. Pietrzyński, Ł. Wyrzykowski, N. Kains, C. Snodgrass, I. A. Steele, K. A. Alsubai, V. Bozza, P. Browne, M. J. Burgdorf, S. Calchi Novati, P. Dodds, S. Dreizler, F. Finet, T. Gerner, S. Hardis, K. Harpsøe, T. C. Hinse, E. Kerins, L. Mancini, M. Mathiasen, M. T. Penny, S. Proft, S. Rahvar, D. Ricci, G. Scarpetta, S. Schäfer, F. Schönebeck, J. Southworth, J. Surdej, J. Wambsganss

Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA-2010-BLG-477. The measured planet-star mass ratio is $q=(2. Read More