A Wide-orbit Exoplanet OGLE-2012-BLG-0838Lb

Poleski, R.; Suzuki, D.; Udalski, A.; Xie, Xiaojia; Yee, Jennifer C.; Koshimoto, Naoki; Gaudi, B. Scott; Gould, Andrew; Skowron, J.; Szymański, M. K.; Soszyński, I.; Kozłowski, S.; Wyrzykowski, Ł.; Ulaczyk, K.; Abe, F.; Barry, Richard; Bennett, D. P.; Bhattacharya, Aparna; Bond, I. A.; Donachie, M.; Fujii, Hirosane; Fukui, A.; Itow, Y.; Hirao, Yuki; Kamei, Y.; Kondo, Iona; Li, Man Cheung Alex; Matsubara, Y.; Miyazaki, Shota; Muraki, Y.; Nagakane, M.; Ranc, Clément; Rattenbury, N. J.; Satoh, Yuki; Shoji, Hikaru; Suematsu, Haruno; Sullivan, D. J.; Sumi, T.; Tristram, P. J.; Yamakawa, T.; Yamawaki, Tsubasa; Yonehara, A.; Han, Cheongho; Dong, Subo; Morzinski, Katie M.; Males, Jared R.; Close, Laird M.; Pogge, Richard W.; Beaulieu, J. P.; Marquette, J. B.

doi:10.3847/1538-3881/ab8a49

2020

DOI: 10.3847/1538-3881/ab8a49

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A Wide-orbit Exoplanet OGLE-2012-BLG-0838Lb

R. Poleski¹,

D. Suzuki²,

A. Udalski³

et al.

Abstract: We present the discovery of a planet on a very wide orbit in the microlensing event OGLE-2012-BLG-0838. The signal of the planet is well separated from the main peak of the event and the planet-star projected separation is found to be twice larger than the Einstein ring radius, which roughly corresponds to a projected separation of ≈ 4 AU. Similar planets around low-mass stars are very hard to find using any technique other than microlensing. We discuss microlensing model fitting in detail and discuss the pros… Show more

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Cited by 4 publications

References 96 publications

(71 reference statements)

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Bayesian Approach for Determining Microlens System Properties with High-angular-resolution Follow-up Imaging

Koshimoto

Bennett

Suzuki

2020

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We present the details of the Bayesian analysis of the planetary microlensing event MOA-2016-BLG-227, whose excess flux is likely due to a source/lens companion or an unrelated ambient star, as well as of the assumed prior distributions. Furthermore, we apply this method to four reported planetary events, MOA-2008-BLG-310, MOA-2011-BLG-293, OGLE-2012-BLG-0527, and OGLE-2012-BLG-0950, where adaptive optics observations have detected excess flux at the source star positions. For events with small angular Einstein radii, our lens mass estimates are more uncertain than those of previous analyses, which assumed that the excess was due to the lens. Our predictions for MOA-2008-BLG-310 and OGLE-2012-BLG-0950 are consistent with recent results on these events obtained via Keck and Hubble Space Telescope observations when the source star is resolvable from the lens star. For events with small angular Einstein radii, we find that it is generally difficult to conclude whether the excess flux comes from the host star. Therefore, it is necessary to identify the lens star by measuring its proper motion relative to the source star to determine whether the excess flux comes from the lens star. Even without such measurements, our method can be used to statistically test the dependence of the planet-hosting probability on the stellar mass.

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Bayesian Approach for Determining Microlens System Properties with High-angular-resolution Follow-up Imaging

Koshimoto

Bennett

Suzuki

2020

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OGLE-2018-BLG-0567Lb and OGLE-2018-BLG-0962Lb: Two Microlensing Planets through the Planetary-caustic Channel

Jung¹,

Han²,

Udalski³

et al. 2021

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We present the analyses of two microlensing events, OGLE-2018-BLG-0567 and OGLE-2018-BLG-0962. In both events, the short-lasting anomalies were densely and continuously covered by two high-cadence surveys. The lightcurve modeling indicates that the anomalies are generated by source crossings over the planetary caustics induced by planetary companions to the hosts. The estimated planet/host separation (scaled to the angular Einstein radius θ E ) and mass ratio are (s, q × 10 3 ) = (1.81 ± 0.02, 1.24 ± 0.07) and (s, q × 10 3 ) = (1.25 ± 0.03, 2.38 ± 0.08), respectively. From Bayesian analyses, we estimate the host and planet masses as = -+ -+

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KMT-2019-BLG-0371 and the Limits of Bayesian Analysis

Kim

Chung

Yee

et al. 2021

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We show that the perturbation at the peak of the light curve of microlensing event KMT-2019-BLG-0371 is explained by a model with a mass ratio between the host star and planet of q ∼ 0.08. Due to the short event duration (t E ∼ 6.5 days), the secondary object in this system could potentially be a massive giant planet. A Bayesian analysis shows that the system most likely consists of a host star with a mass  = -+ M M 0.09 h 0.05 0.14 and a massive giant planet with a mass = -+ M M 7.70 p 3.90 11.34Jup . However, the interpretation of the secondary as a planet (i.e., as having M p < 13M Jup ) rests entirely on the Bayesian analysis. Motivated by this event, we conduct an investigation to determine which constraints meaningfully affect Bayesian analyses for microlensing events. We find that the masses inferred from such a Bayesian analysis are determined almost entirely by the measured value of θ E and are relatively insensitive to other factors such as the direction of the event (ℓ, b), the lens-source relative proper motion μ rel , or the specific Galactic model prior.

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A Wide-orbit Exoplanet OGLE-2012-BLG-0838Lb

Cited by 4 publications

References 96 publications

Bayesian Approach for Determining Microlens System Properties with High-angular-resolution Follow-up Imaging

Bayesian Approach for Determining Microlens System Properties with High-angular-resolution Follow-up Imaging

OGLE-2018-BLG-0567Lb and OGLE-2018-BLG-0962Lb: Two Microlensing Planets through the Planetary-caustic Channel

KMT-2019-BLG-0371 and the Limits of Bayesian Analysis

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