OGLE-2016-BLG-0613LABb: A Microlensing Planet in a Binary System

Han, Cheongho; Udalski, A.; Gould, Andrew; Lee, C. U.; Shvartzvald, Yossi; Zang, Weicheng; Mao, Shude; Kozłowski, S.; Albrow, M. D.; Chung, Sun-Ju; Hwang, Kyu-Ha; Jung, Youn Kil; Kim, D.; Kim, H. W.; Ryu, Yoon-Hyun; Shin, In-Gu; Yee, Jennifer C.; Zhu, Wei; M., S.; Kim, S. L.; Kim, D. J.; Lee, Y.; Park, B. G.; Skowron, J.; Mróz, P.; Pietrukowicz, P.; Poleski, R.; Szymański, M. K.; Ulaczyk, K.; Pawlak, M.; Beichman, C. A.; Bryden, G.; Novati, S. Calchi; Gaudi, B. Scott; Henderson, Calen B.; Howell, Steve B.; Jacklin, Savannah; Penny, Matthew T.; Fouqué, P.; Wang, T. S.

doi:10.3847/1538-3881/aa9179

Cited by 53 publications

(14 citation statements)

References 62 publications

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“…The wide-field optical and infra-red telescopes on Mauna Kea (CFHT-MegaCam, CFHT-WIRCAM, Subaru-HyperSuprimeCam, and UKIRT-WFCAM) can therefore add significant value to the existing microlensing survey networks. This has been demonstrated by our data set's contribution to several planet discoveries in 2016 (Koshimoto et al 2017;Ryu et al 2018;Han et al 2017).…”

Section: Discussionsupporting

confidence: 62%

Measurement of Source Star Colors with the K2C9-CFHT Multi-color Microlensing Survey

Zang

Penny

Zhu

et al. 2018

PASP

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K2 Campaign 9 (K2C9) was the first space-based microlensing parallax survey capable of measuring microlensing parallaxes of free-floating planet candidate microlensing events. Simultaneous to K2C9 observations we conducted the K2C9 Canada-France-Hawaii Telescope Multi-Color Microlensing Survey (K2C9-CFHT MCMS) in order to measure the colors of microlensing source stars to improve the accuracy of K2C9's parallax measurements. We describe the difference imaging photometry analysis of the K2C9-CFHT MCMS observations, and present the project's first data release. This includes instrumental difference flux lightcurves of 217 microlensing events identified by other microlensing surveys, reference image photometry calibrated to PanSTARRS data release 1 photometry, and tools to convert between instrumental and calibrated flux scales. We derive accurate analytic transformations between the PanSTARRS bandpasses and the Kepler bandpass, as well as angular diametercolor relations in the PanSTARRS bandpasses. To demonstrate the use of our data set, we analyze ground-based and K2 data of a short timescale microlensing event, OGLE-2016-BLG-0795. We find the event has a timescale t E = 4.5 ± 0.1 days and microlens parallax π E = 0.12 ± 0.03 or 0.97 ± 0.04, subject to the standard satellite parallax degeneracy. We argue that the smaller value of the parallax is more likely, which implies that the lens is likely a stellar-mass object in the Galactic bulge as opposed to a super-Jupiter mass object in the Galactic disk.

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Section: Discussionsupporting

confidence: 62%

Measurement of Source Star Colors with the K2C9-CFHT Multi-color Microlensing Survey

Zang

Penny

Zhu

et al. 2018

PASP

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“…In the analysis of triple microlensing events the configuration is typically parameterized by two side lengths s 2 , s 3 from the first to the two other components and the angle ψ subtended by them (e.g., Han et al 2017b). The right panel of Figure 14 illustrates the geometry in terms of these parameters.…”

Section: A2 Triangular Parametersmentioning

confidence: 99%

“…Two more microlensing events involving a star + two planets lens have been published so far: OGLE-2012-BLG-0026 (Han et al 2013;Beaulieu et al 2016) and OGLE-2014-BLG-1722(Suzuki et al 2018). In addition, four events involving a binary-star lens with a planet have been published: OGLE-2007-BLG-349 with a circumbinary planet , OGLE-2008-BLG-092 (Poleski et al 2014), OGLE-2013-BLG-0341 (Gould et al 2014), and OGLE-2016-BLG-0613 (Han et al 2017b).…”

Section: Introductionmentioning

confidence: 99%

Triple-lens Gravitational Microlensing: Critical Curves for Arbitrary Spatial Configuration

Danek¹,

Heyrovsky²

2019

ApJ

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Since the first observation of triple-lens gravitational microlensing in 2006, analyses of six more events have been published by the end of 2018. In three events the lens was a star with two planets; four involved a binary star with a planet. Other possible triple lenses, such as triple stars or stars with a planet with a moon, are yet to be detected. The analysis of triple-lens events is hindered by the lack of understanding of the diversity of their caustics and critical curves. We present a method for identifying the full range of critical curves for a triple lens with a given combination of masses in an arbitrary spatial configuration. We compute their boundaries in parameter space, identify the critical-curve topologies in the partitioned regions, and evaluate their probabilities of occurrence. We demonstrate the analysis on three triple-lens models. For three equal masses the computed boundaries divide the parameter space into 39 regions yielding nine different critical-curve topologies. The other models include a binary star with a planet, and a hierarchical star-planet-moon combination of masses. Both have the same set of 11 topologies, including new ones with doubly nested critical-curve loops. The number of lensing regimes thus depends on the combination of masses -unlike in the double lens, which has the same three regimes for any mass ratio. The presented approach is suitable for further investigations, such as studies of the changes occurring in nonstatic lens configurations due to orbital motion of the components or other parallax-type effects.

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“…In this case, the resulting anomaly can be approximated by the superposition of the two binary anomalies, in which the individual primary-companion pairs act as independent 2-body systems (Han 2005). This binary-superposition approximation can be applied for two cases of triple-lens systems, in which the lens is composed of multiple planets, as demonstrated in the cases of OGLE-2006-BLG-109 ) OGLE-2012-BLG-0026 , and planets in close or wide binary systems, as demonstrated in the case of OGLE-2016-BLG-0613 (Han et al 2017). The 2L1S modeling of OGLE-2018-BLG-1011 yields two local solutions, with a planetary companion and a close/wide binary companion, respectively.…”

Section: Triple-lens (3l1s) Interpretationmentioning

confidence: 99%

OGLE-2018-BLG-1011Lb,c: Microlensing Planetary System with Two Giant Planets Orbiting a Low-mass Star

Han¹,

Bennett²,

Udalski³

et al. 2019

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We report a multiplanetary system found from the analysis of microlensing event OGLE-2018-BLG-1011, for which the light curve exhibits a double-bump anomaly around the peak. We find that the anomaly cannot be fully explained by the binary-lens or binary-source interpretations and its description requires the introduction of an additional lens component. The 3L1S (3 lens components and a single source) modeling yields three sets of solutions, in which one set of solutions indicates that the lens is a planetary system in a binary, while the other two sets imply that the lens is a multiplanetary system. By investigating the fits of the individual models to the detailed light curve structure, we find that the multiple-planet solution with planet-to-host mass ratios ∼ 9.5 × 10 −3 and ∼ 15 × 10 −3 are favored over the other solutions. From the Bayesian analysis, we find that the lens is composed of two planets with masses 1.8 +3..4 −1.1 M J and 2.8 +5.1 −1.7 M J around a host with a mass 0.18 +0.33 −0.10 M ⊙ and located at a distance 7.1 +1.1 −1.5 kpc. The estimated distance indicates that the lens is the farthest system among the known multiplanetary systems. The projected planet-host separations are a ⊥,2 = 1.8 +2.1 −1.5 au (0.8 +0.9 −0.6 au) and a ⊥,3 = 0.8 +0.9 −0.6 au, where the values of a ⊥,2 in and out the parenthesis are the separations corresponding to the two degenerate solutions, indicating that both planets are located beyond the snow line of the host, as with the other four multiplanetary systems previously found by microlensing.

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OGLE-2016-BLG-0613LABb: A Microlensing Planet in a Binary System

Cited by 53 publications

References 62 publications

Measurement of Source Star Colors with the K2C9-CFHT Multi-color Microlensing Survey

Measurement of Source Star Colors with the K2C9-CFHT Multi-color Microlensing Survey

Triple-lens Gravitational Microlensing: Critical Curves for Arbitrary Spatial Configuration

OGLE-2018-BLG-1011Lb,c: Microlensing Planetary System with Two Giant Planets Orbiting a Low-mass Star

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