Ogle-2013-BLG-0102la,b: Microlensing Binary With Components at Star/Brown Dwarf and Brown Dwarf/Planet Boundaries

Jung, Y. K.; Udalski, A.; Sumi, T.; Han, Cheongho; Gould, Andrew; Skowron, J.; Kozłowski, S.; Poleski, R.; Wyrzykowski, Ł.; Szymański, M. K.; Pietrzyński, G.; Soszyński, I.; Ulaczyk, K.; Mróz, P.; Kubiak, M.; Abe, F.; Bennett, D. P.; Bond, I. A.; Botzler, C. S.; Freeman, Matthew; Fukui, A.; Fukunaga, D.; Itow, Y.; Koshimoto, Naoki; Larsen, Patricia; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Namba, Susumu; Ohnishi, Koji; Philpott, L.; Rattenbury, N. J.; Saito, To.; Sullivan, D. J.; Suzuki, D.; Tristram, P. J.; Tsurumi, Naoki; Wada, K.; Yamai, N.; Yock, P. C. M.; Yonehara, A.; Albrow, M. D.; Choi, J.-Y.; DePoy, D. L.; Gaudi, B. Scott; Hwang, Kyu-Ha; Lee, Chung-Uk; Park, H.; Owen, Stephanie J.; Pogge, Richard W.; Shin, In-Gu; Yee, Jennifer C.

doi:10.1088/0004-637x/798/2/123

Cited by 56 publications

(30 citation statements)

References 57 publications

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“…Another candidate super-Jupiter mass planet in the sample orbiting a low mass star is MOA-2012-BLG-006 (Poleski et al 2017), but a mass measurement for this event would be quite difficult, because of its bright giant source star. In addition to these events in the sample, the following events are candidates for super-Jupiter planets orbiting low-mass stars: MOA-2010-BLG-73, OGLE-2013-BLG-0102, OGLE-2013-BLG-1761, OGLE-2015-BLG-0954, MOA-2016-BLG-227, OGLE-2016-BLG-0263, KMT-2016-BLG-1397, and KMT-2017-BLG-1038(Street et al 2013Jung et al 2015;Hirao et al 2017;Shin et al 2016;Bennett et al 2017;Koshimoto et al 2017b;Zang et al 2018;Shin et al 2019). Perhaps the most interesting candidate is OGLE-2018-BLG-1011 (Han et al 2019), which has two super-Jupiter planets with mass ratios of 0.015 and 0.0095 orbiting a star with an estimated mass of ∼ 0.2M .…”

Section: Introductionmentioning

confidence: 99%

Keck Observations Confirm a Super-Jupiter Planet Orbiting M Dwarf OGLE-2005-BLG-071L

Bennett

Bhattacharya

Beaulieu

et al. 2020

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We present adaptive optics imaging from the NIRC2 instrument on the Keck-2 telescope that resolves the exoplanet host (and lens) star as it separates from the brighter source star. These observations yield the K-band brightness of the lens and planetary host star, as well as the lens-source relative proper motion, µ rel,H . in the heliocentric reference frame. The µ rel,H measurement allows determination of the microlensing parallax vector, π E , which had only a single component determined by the microlensing light curve. The combined measurements of µ rel,H and K L provide the masses of the host stat, M host = 0.426 ± 0.037M , and planet, m p = 3.27 ± 0.32M Jupiter with a projected separation of 3.4 ± 0.5 AU. This confirms the tentative conclusion of a previous paper (Dong et al. 2009b) that this super-Jupiter mass planet, OGLE-2005-BLG-071Lb, arXiv:1909.04740v1 [astro-ph.EP] 10 Sep 2019 -2orbits an M-dwarf. Such planets are predicted to be rare by the core accretion theory and have been difficult to find with other methods, but there are two such planets with firm mass measurements from microlensing, and an additional 11 planetary microlens events with host mass estimates < 0.5M and planet mass estimates > 2 Jupiter masses that could be confirmed by high angular follow-up observations. We also point out that OGLE-2005-BLG-071L has separated far enough from its host star that it should be possible to measure the host star metalicity with spectra from a high angular resolution telescope such as Keck, the VLT, the Hubble Space Telescope or the James Webb Space Telescope.

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Section: Introductionmentioning

confidence: 99%

Keck Observations Confirm a Super-Jupiter Planet Orbiting M Dwarf OGLE-2005-BLG-071L

Bennett

Bhattacharya

Beaulieu

et al. 2020

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“…Binary-lens Interpretation Adopting the parametrization of Jung et al (2015) for the description of a standard binary-lens light curve, we search for a binary-lens solution by following the method of Jung et al (2015), one of the well-established modeling procedure developed based on the map-making method (Dong et al 2006). 5 Figure 2 shows the ∆χ 2 surface of (s, q) parameter space derived from the initial grid search.…”

Section: Discussionmentioning

confidence: 99%

Binary Source Microlensing Event OGLE-2016-BLG-0733: Interpretation of a Long-term Asymmetric Perturbation

Jung¹,

Udalski²,

Yee³

et al. 2017

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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. From the detailed modeling of the lensing light curve, however, we find that the perturbation originates from the binarity of the source rather than the lens. This result demonstrates that binary sources with roughly equal-luminosity components can mimic long-term perturbations induced by planets with projected separations near the Einstein ring. The result also represents the importance of the consideration of various interpretations in planet-like perturbations and of high-cadence observations for ensuring the unambiguous detection of the planet.

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“…Because the event was simultaneously observed by ground and space telescopes, we try to find fits for both observed light curves using parameters adopted from the conventional parameterization (Refsdal 1966;Gould 1992Gould , 1994Graff & Gould 2002;Shin et al 2013;Jung et al 2015;Udalski et al 2015b;Zhu et al 2015). We briefly summarize the parameterization to facilitate further description of the modeling.…”

Section: Discussionmentioning

confidence: 99%

OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Microlens Parallax Effect from Space-based Observations

Shin¹,

Udalski²,

Yee³

et al. 2017

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The microlens parallax is a crucial observable for conclusively identifying the nature of lens systems in microlensing events containing or composed of faint (even dark) astronomical objects such as planets, neutron stars, brown dwarfs, and black holes. With the commencement of a new era of microlensing in collaboration with space-based observations, the microlens parallax can be routinely measured. In addition, space-based observations can provide opportunities to verify the microlens parallax measured from ground-only observations and to find a unique solution to the lensing light-curve analysis. Furthermore, since most space-based observations cannot cover the full light curves of lensing events, it is also necessary to verify the reliability of the information extracted from fragmentary space-based light curves. We conduct a test based on the microlensing event OGLE-2016-BLG-0168, created by a binary lens system consisting of almost equal mass M-dwarf stars, to demonstrate that it is possible to verify the microlens parallax and to resolve degeneracies using the space-based light curve even though the observations are fragmentary. Since space-based observatories will frequently produce fragmentary light curves due to their short observing windows, the methodology of this test will be useful for next-generation microlensing experiments that combine space-based and ground-based collaboration.

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Ogle-2013-BLG-0102la,b: Microlensing Binary With Components at Star/Brown Dwarf and Brown Dwarf/Planet Boundaries

Cited by 56 publications

References 57 publications

Keck Observations Confirm a Super-Jupiter Planet Orbiting M Dwarf OGLE-2005-BLG-071L

Keck Observations Confirm a Super-Jupiter Planet Orbiting M Dwarf OGLE-2005-BLG-071L

Binary Source Microlensing Event OGLE-2016-BLG-0733: Interpretation of a Long-term Asymmetric Perturbation

OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Microlens Parallax Effect from Space-based Observations

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