Triple Microlens Ogle-2008-BLG-092l: Binary Stellar System With a Circumprimary Uranus-Type Planet

Poleski, R.; Skowron, J.; Udalski, A.; Han, Cheongho; Kozłowski, S.; Wyrzykowski, Ł.; Dong, Subo; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Ulaczyk, K.; Gould, Andrew

doi:10.1088/0004-637x/795/1/42

Cited by 102 publications

(72 citation statements)

References 59 publications

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“…Circumbinary planets and planets in close binary systems are very difficult to detect with the radial velocity method, but Kepler has proved quite adept at finding such systems (Doyle et al 2011;Orosz et al 2012;Welsh et al 2012Welsh et al , 2015Kostov et al 2013Kostov et al , 2014Kostov et al , 2016. Gravitational microlensing (Bennett 2008;Gaudi 2012) has demonstrated the ability to detect such systems (Bennett et al 1999;Gould et al 2014;Poleski et al 2014;Udalski et al 2015) (either circumbinary planets or planets orbiting one member of a relatively close binary). Two of these claimed microlensing planets in binary systems have turned out to be incorrect, MACHO-97-BLG-41 (Bennett et al 1999;Albrow et al 2000;Jung et al 2013) and OGLE-2013-BLG-0723 (Udalski et al 2015;Han et al 2016), but this is largely an issue that can be addressed by greater care in event modeling.…”

Section: Introductionmentioning

confidence: 99%

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Bennett¹,

Rhie²,

Udalski³

et al. 2016

106

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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≈3.4×10 −4 , but there is an additional signal due to an additional lens mass, either another planet or another star. We find acceptable light-curve fits with two classes of models: two-planet models (with a single host star) and circumbinary planet models. The light curve also reveals a significant microlensing parallax effect, which constrains the mass of the lens system to be M L ≈0.7  M . Hubble Space Telescope (HST) images resolve the lens and source stars from their neighbors and indicate excess flux due to the star(s) in the lens system. This is consistent with the predicted flux from the circumbinary models, where the lens mass is shared between two stars, but there is not enough flux to be consistent with the two-planet, one-star models. So, only the circumbinary models are consistent with the HST data. They indicate a planet of mass m c =80±13 Å M , orbiting a pair of M dwarfs with masses of M A =0.41±0.07 and M B =0.30±0.07, which makes this the lowest-mass circumbinary planet system known. The ratio of the separation between the planet and the center of mass to the separation of the two stars is ∼40, so unlike most of the circumbinary planets found by Kepler, the planet does not orbit near the stability limit.

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Section: Introductionmentioning

confidence: 99%

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Bennett¹,

Rhie²,

Udalski³

et al. 2016

106

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“…For this event, the lensing light curve exhibited little lensing magnification attributable to the host of the planet similar to OGLE-2016-BLG-1227, but the planetary signal was entirely due to a brief caustic feature. The second case is OGLE-2008-BLG-092 (Poleski et al 2014). For this event, the planet was detected through the isolated event channel, but in this case the host of the planet was on the source trajectory, and gave rise to a bump in the lensing light curve.…”

Section: Discussionmentioning

confidence: 99%

OGLE-2016-BLG-1227L: A Wide-separation Planet from a Very Short-timescale Microlensing Event

Han

Udalski²,

Gould³

et al. 2020

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We present the analysis of the microlensing event OGLE-2016-BLG-1227. The light curve of this shortduration event appears to be a single-lens event affected by severe finite-source effects. Analysis of the light curve based on single-lens single-source (1L1S) modeling yields very small values of the event timescale, t E ∼ 3.5 days, and the angular Einstein radius, θ E ∼ 0.009 mas, making the lens a candidate of a free-floating planet. Close inspection reveals that the 1L1S solution leaves small residuals with amplitude ∆I 0.03 mag. We find that the residuals are explained by the existence of an additional widely-separated heavier lens component, indicating that the lens is a wide-separation planetary system rather than a free-floating planet. From Bayesian analysis, it is estimated that the planet has a mass of M p = 0.79 +1.30 −0.39 M J and it is orbiting a low-mass host star with a mass of M host = 0.10 +0.17 −0.05 M ⊙ located with a projected separation of a ⊥ = 3.4 +2.1 −1.0 au. The planetary system is located in the Galactic bulge with a line-of-sight separation from the source star of D LS = 1.21 +0.96 −0.63 kpc. The event shows that there are a range of deviations in the signatures of host stars for apparently isolated planetary lensing events and that it is possible to identify a host even when a deviation is subtle.

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“…We used MCMC implementation by Dong et al (2007) and Poleski et al (2014). Even though we run the MCMC multiple times with a number of settings, MCMC failed to produce a converging chain and hence we could not use it to fit a microlensing model.…”

Section: Discussionmentioning

confidence: 99%

A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

Poleski

Udalski

Bond

et al. 2017

A&A

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We present the discovery of a substellar companion to the primary host lens in the microlensing event MOA-2012-BLG-006. The companion-to-host mass ratio is 0.016, corresponding to a companion mass ofThus, the companion is either a high-mass giant planet or a low-mass brown dwarf, depending on the mass of the primary M * . The companion signal was separated from the peak of the primary event by a time that was as much as four times longer than the event timescale. We therefore infer a relatively large projected separation of the companion from its host of ≈ 10 a.u.(M * /0.5M ) 1/2 for a wide range (3-7 kpc) of host star distances from the Earth. We also challenge a previous claim of a planetary companion to the lens star in microlensing event OGLE-2002-BLG-045.

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Triple Microlens Ogle-2008-BLG-092l: Binary Stellar System With a Circumprimary Uranus-Type Planet

Cited by 102 publications

References 59 publications

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

OGLE-2016-BLG-1227L: A Wide-separation Planet from a Very Short-timescale Microlensing Event

A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

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