Binary Microlensing Event Ogle-2009-BLG-020 Gives Verifiable Mass, Distance, and Orbit Predictions

Skowron, J.; Udalski, A.; Gould, Andrew; Dong, Subo; Monard, L. A. G.; Han, Cheongho; Nelson, C.; McCormick, J.; Moorhouse, D.; Thornley, G.; Maury, A.; Bramich, D. M.; Greenhill, J.; Kozłowski, S.; Bond, I. A.; Poleski, R.; Wyrzykowski, Ł.; Ulaczyk, K.; Kubiak, M.; Szymański, M. K.; Pietrzyński, G.; Gaudi, B. Scott; Yee, Jennifer C.; Hung, L. W.; Pogge, Richard W.; DePoy, D. L.; Lee, Chung-Uk; Park, B.-G.; Allen, William H.; Mallia, F.; Drummond, J.; Bolt, Greg; Allan, A.; Browne, P.; Clay, N.; Dominik, M.; Fraser, S. N.; Horne, K.; Kains, N.; Mottram, Christopher J.; Snodgrass, C.; Steele, I. A.; Street, R. A.; Tsapras, Y.; Abe, F.; Bennett, D. P.; Botzler, C. S.; Douchin, D.; Freeman, Matthew; Fukui, A.; Furusawa, K.; Hayashi, F.; Hearnshaw, John; Hosaka, S.; Itow, Y.; Kamiya, K.; Kilmartin, P. M.; Korpela, A.; Lin, Wei; Ling, C. H.; Makita, S.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nagayama, Takahiro; Miyake, N.; Nishimoto, K.; Ohnishi, Kouhei; Perrott, Y. C.; Rattenbury, N. J.; Saito, To.; Skuljan, L.; Sullivan, D. J.; Sumi, T.; Suzuki, D.; Sweatman, W. L.; Tristram, P. J.; Wada, K.; Yock, P. C. M.; Beaulieu, J. P.; Fouqué, P.; Albrow, M. D.; Batista, V.; Brillant, S.; Caldwell, J. A. R.; Cassan, A.; Cole, A. A.; Cook, K. H.; Coutures, C.; Dieters, S.; Prester, D. Dominis; Donatowicz, J.; Kane, Stephen R.; Kubas, D.; Marquette, J. B.; Martín, Roland; Menzies, John; Sahu, Kailash C.; Wambsganß, J.; Williams, A.; Zub, M.

doi:10.1088/0004-637x/738/1/87

Cited by 146 publications

(187 citation statements)

References 45 publications

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“…Still, it did not seem possible to measure full orbits. Nevertheless, Skowron et al (2011) significantly constrained all seven Kepler parameters for the binary system OGLE-2009-BLG-020L, albeit with huge errors and strong correlations. These measurements were later shown to be consistent with RV follow-up observations by Yee et al (2016).…”

Section: Full Kepler Orbits In Microlensingmentioning

confidence: 99%

“…Of course, if these parameters are specified, together with the total mass of the system, one can determine the full orbit and hence the Kepler parameters. Skowron et al (2011) discusses the transformations from microlensing parameters to Kepler parameters in detail. For each MCMC sample, one determines θ * from the value of f s Figure 8.…”

Section: Full Keplerian Orbital Solutionmentioning

confidence: 99%

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OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

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We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass, M p =13.4±0.9 M J , places it right at the deuteriumburning limit, i.e., the conventional boundary between "planets" and "brown dwarfs." Its existence raises the question of whether such objects are really "planets" (formed within the disks of their hosts) or "failed stars" (lowmass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M host =0.89±0.07 M e , and the planet has a semimajor axis a∼2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period.

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Section: Full Kepler Orbits In Microlensingmentioning

confidence: 99%

Section: Full Keplerian Orbital Solutionmentioning

confidence: 99%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

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“…Kubas et al 2012), or Bayesian analysis are used to derive the physical parameters of the different planetary systems and to proceed further in the analysis. In this context, Skowron et al (2011) showed that the deformation of the microlensing light curve can be used to constrain all the orbital parameters of a binary lens system. Shin et al (2012) presented the microlensing event OGLE-2011-BLG-0417 and modelled it as due to a binary lens system.…”

Section: Based On Observations Made With Eso Telescope At the Paranalmentioning

confidence: 99%

The first radial velocity measurements of a microlensing event: no evidence for the predicted binary

Boisse

Santerne

Beaulieu

et al. 2015

A&A

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The gravitational microlensing technique allows the discovery of exoplanets around stars distributed in the disk of the galaxy towards the bulge. The alignment of two stars that led to the discovery is unique over the timescale of a human life, however, and cannot be re-observed. Moreover, the target host is often very faint and located in a crowded region. These difficulties hamper and often make impossible the follow up of the target and study of its possible companions. A radial-velocity curve was predicted for the binary system, OGLE-2011-BLG-0417, discovered and characterised from a microlensing event. We used the UVES spectrograph mounted at the VLT, ESO to derive precise radial-velocity measurements of OGLE-2011-BLG-0417. To gather high-precision radial velocities on faint targets of microlensing events, we proposed to use the source star as a reference to measure the lens radial velocities. We obtained ten radial velocities on the putative V = 18 lens with a dispersion of ∼100 m s −1 , spread over one year. Our measurements do not confirm the microlensing prediction for this binary system. The most likely scenario is that the putative V = 18 mag lens is actually a blend and not the primary lens which is 2 mag fainter. Further observations and analyses are needed to understand the microlensing observation and infer on the nature and characteristics of the lens itself.

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“…The default binary lens parametrization is not optimal for fitting all the microlensing events because the parameters α, q, and in many cases s are not directly constrained by the light curves, in the sense that the observable properties of the microlensing event are not directly relatable to these parameters (Cassan 2008;Sumi et al 2010;Skowron et al 2011;Kains et al 2012). …”

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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Binary Microlensing Event Ogle-2009-BLG-020 Gives Verifiable Mass, Distance, and Orbit Predictions

Cited by 146 publications

References 45 publications

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

The first radial velocity measurements of a microlensing event: no evidence for the predicted binary

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

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