OGLE-2016-BLG-0156: Microlensing Event with Pronounced Microlens-parallax Effects Yielding a Precise Lens Mass Measurement

Jung, Youn Kil; Han, Cheongho; Bond, I. A.; Udalski, A.; Gould, Andrew; Albrow, M. D.; Chung, Sun-Ju; Hwang, Kyu-Ha; Lee, Chung-Uk; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yee, Jennifer C.; Jee, M. James; Kim, Doeon; Cha, Sang-Mok; Kim, Dong-Jin; Lee, Dong-Joo; Lee, Yongseok; Park, Byeong-Gon; Pogge, Richard W.; Abe, F.; Barry, Richard; Bennett, D. P.; Bhattacharya, Aparna; Donachie, M.; Fukui, A.; Hirao, Yuki; Itow, Y.; Kawasaki, Kohei; Kondo, Iona; Koshimoto, Naoki; Li, Man Cheung Alex; Matsubara, Y.; Muraki, Y.; Miyazaki, Shota; Nagakane, M.; Ranc, Clément; Rattenbury, N. J.; Suematsu, Haruno; Sullivan, D. J.; Sumi, T.; Suzuki, D.; Tristram, P. J.; Yonehara, A.; Mróz, P.; Poleski, R.; Skowron, J.; Szymański, M. K.; Soszyński, I.; Ulaczyk, K.; Pawlak, M.

doi:10.3847/1538-4357/ab001f

Cited by 2 publications

(2 citation statements)

References 35 publications

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“…For all the analyzed events, the angular Einstein radii are securely measured from the detections of finite-source effects. The microlens parallax is measurable by detecting deformations in lensing lightcurves caused by the deviation of the source motion from rectilinear due to the change of the observer's position induced by the orbital motion of Earth around the Sun (Gould 1992), e.g., OGLE-2016-BLG-0156 (Jung et al 2019). The microlens parallax cannot be measured through this annual microlens parallax channel for any of the events because the timescales of the events are too short to yield measurable deviations in the lensing lightcurves.…”

Section: Nature Of Lensesmentioning

confidence: 99%

Candidate Brown-dwarf Microlensing Events with Very Short Timescales and Small Angular Einstein Radii

Han

Lee

Udalski

et al. 2020

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Short-timescale microlensing events are likely to be produced by substellar brown dwarfs (BDs), but it is difficult to securely identify BD lenses based on only event timescales t E because short-timescale events can also be produced by stellar lenses with high relative lens-source proper motions. In this paper, we report three strong candidate BD-lens events found from the search for lensing events not only with short timescales (  t 6 days E ) but also with very small angular Einstein radii (q  0.05 mas E ) among the events that have been found in the

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Section: Nature Of Lensesmentioning

confidence: 99%

Candidate Brown-dwarf Microlensing Events with Very Short Timescales and Small Angular Einstein Radii

Han

Lee

Udalski

et al. 2020

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“…However, the measurement of p E in this single accelerating frame is usually difficult because the change of the observer's position during typical microlensing events (t E < yr/2π) is quite minor. As a result, the sample of events with p E measured from the annual parallax effect is relatively small, and they are biased toward events with long timescales (e.g., Jung et al 2019b) and/ or events produced by nearby lenses (e.g., Jung et al 2018a).…”

Section: Introductionmentioning

confidence: 99%

Spitzer Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M Dwarf

Jung

Gould

Udalski

et al. 2019

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We report the discovery of a Spitzer microlensing planet OGLE-2018-BLG-0596Lb, with preferred planet-host mass ratio q∼2×10 −4 . The planetary signal, which is characterized by a short (∼1 day) "bump" on the rising side of the lensing light curve, was densely covered by ground-based surveys. We find that the signal can be explained by a bright source that fully envelops the planetary caustic, i.e., a "Hollywood" geometry. Combined with the source proper motion measured from Gaia, the Spitzer satellite parallax measurement makes it possible to precisely constrain the lens physical parameters. The preferred solution, in which the planet perturbs the minor image due to lensing by the host, yields a Uranus-mass planet with a mass of M p =13.9±1.6M ⊕ orbiting a mid M-dwarf with a mass of M h =0.23±0.03M e . There is also a second possible solution that is substantially disfavored but cannot be ruled out, for which the planet perturbs the major image. The latter solution yields M p =1.2±0.2M ⊕ and M h =0.15±0.02M e . By combining the microlensing and Gaia data together with a Galactic model, we find in either case that the lens lies on the near side of the Galactic bulge at a distance D L ∼6±1 kpc. Future adaptive optics observations may decisively resolve the major image/minor image degeneracy.

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OGLE-2016-BLG-0156: Microlensing Event with Pronounced Microlens-parallax Effects Yielding a Precise Lens Mass Measurement

Cited by 2 publications

References 35 publications

Candidate Brown-dwarf Microlensing Events with Very Short Timescales and Small Angular Einstein Radii

Candidate Brown-dwarf Microlensing Events with Very Short Timescales and Small Angular Einstein Radii

Spitzer Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M Dwarf

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