MOA-2011-BLG-262Lb: A SUB-EARTH-MASS MOON ORBITING A GAS GIANT PRIMARY OR A HIGH VELOCITY PLANETARY SYSTEM IN THE GALACTIC BULGE

Bennett, D. P.; Batista, V.; Bond, I. A.; Bennett, C. S.; Suzuki, D.; Beaulieu, J. P.; Udalski, A.; Donatowicz, J.; Bozza, V.; Abe, F.; Botzler, C. S.; Freeman, Matthew; Fukunaga, D.; Fukui, A.; Itow, Y.; Koshimoto, Naoki; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Namba, Susumu; Ohnishi, Kouhei; Rattenbury, N. J.; Saito, To.; Sullivan, D. J.; Sumi, T.; Sweatman, W. L.; Tristram, P. J.; Tsurumi, Naoki; Wada, K.; Yock, P. C. M.; Albrow, M. D.; Bachelet, E.; Brillant, S.; Caldwell, J.; Cassan, A.; Cole, A. A.; Corrales, E.; Coutures, C.; Dieters, S.; Prester, D. Dominis; Fouqué, P.; Greenhill, J.; Horne, K.; Koo, Jae‐Rim; Kubas, D.; Marquette, J. B.; Martín, Roland; Menzies, John; Sahu, K. C.; Wambsganß, J.; Williams, A.; Zub, M.; Choi, J.-Y.; DePoy, D. L.; Dong, Subo; Gaudi, B. Scott; Gould, Andrew; Han, Cheongho; Henderson, Calen B.; McGregor, D.; Lee, Chung-Uk; Pogge, Richard W.; Shin, In-Gu; Yee, Jennifer C.; Szymański, M. K.; Skowron, J.; Poleski, R.; Kozllowski, S.; Wyrzykowski, Ł.; Kubiak, M.; Pietrukowicz, P.; Pietrzyński, G.; Ulaczyk, K.; Tsapras, Y.; Street, R. A.; Dominik, M.; Bramich, D. M.; Browne, P.; Hundertmark, M.; Kains, N.; Snodgrass, C.; Steele, I. A.; Dékány, I.; Gonzalez, O. A.; Heyrovsky, David; Kandori, Ryo; Kerins, E.; Lucas, P. W.; Minniti, D.; Nagayama, Takahiro; Rejkuba, M.; Robin, A. C.; Saito, R. K.

doi:10.1088/0004-637x/785/2/155

Cited by 167 publications

(106 citation statements)

References 89 publications

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“…If we assume that all stars and brown dwarfs have an equal probability of hosting a planet with the measured properties, then we can perform a Bayesian analysis to estimate the lens system properties using the technique from Bennett et al (2014). We ran an MCMC run with about 180,000 links to obtain the posterior distributions presented in Table 3 and Figure 5.…”

Section: Lens Properties and Discussionmentioning

confidence: 99%

“…These distributions are based on the source-star brightness, color, and the radius calculated in Section 4. It is also assumed that the source star is a main-sequence bulge star distributed across 5-12 kpc following a standard Galactic model (Bennett et al 2014). For each MCMC fit, the source distance is picked randomly from this distribution.…”

Section: Lens Properties and Discussionmentioning

confidence: 99%

“…To determine the uncertainties for the model parameters, it is necessary to have accurate error bars that will give c » dof 1 2 for each data set. We used the method of Bennett et al (2014) . The number of data points used for each telescope and their corresponding k values are listed in Table 1.…”

Section: Data Reductionmentioning

confidence: 99%

“…We calculate the extinction in the direction of the source using the method described by Bennett et al (2014). The position of the centroid of the red clump in the OGLE-III catalog is found to be - 2.20, 15.84).…”

Section: Calibration and Source Propertiesmentioning

confidence: 99%

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Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Bhattacharya

Bennett

Bond

et al. 2016

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We present the analysis of the planetary microlensing event OGLE-2014-BLG-1760, which shows a strong lightcurve signal due to the presence of a Jupiter mass ratio planet. One unusual feature of this event is that the source star is quite blue, with -=  V I 1.48 0.08. This is marginally consistent with a source star in the Galactic bulge, but it could possibly indicate a young source star on the far side of the disk. Assuming a bulge source, we perform a Bayesian analysis assuming a standard Galactic model, and this indicates that the planetary system resides in or near the Galactic bulge at =  D 6.9 1.1 kpc , and a projected star-planet separation of = -+ a 1.75 0.33 0.34 au. The lens-source relative proper motion is m =  6.5 1.1 rel mas yr −1 . The lens (and stellar host star) is estimated to be very faint compared to the source star, so it is most likely that it can be detected only when the lens and source stars start to separate. Due to the relatively high relative proper motion, the lens and source will be resolved to about ∼46 mas in 6-8 yr after the peak magnification. So, by 2020-2022, we can hope to detect the lens star with deep, high-resolution images.

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Section: Lens Properties and Discussionmentioning

confidence: 99%

Section: Lens Properties and Discussionmentioning

confidence: 99%

Section: Data Reductionmentioning

confidence: 99%

Section: Calibration and Source Propertiesmentioning

confidence: 99%

See 2 more Smart Citations

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Bhattacharya

Bennett

Bond

et al. 2016

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“…The values Q p and k 2,p are the tidal quality factor and degree-2 Love number of the planet, which control the energy dissipation rate. Because T ∝ M −1 L a 13/2 * , large moons orbiting planets close to their parent stars have short lifetimes; this may explain why there have been only a few possible detections of exomoons so far [35,138].…”

Section: Dynamical Stabilitymentioning

confidence: 99%

Formation of exomoons: a solar system perspective

Barr

2016

Astronomical Review

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Satellite formation is a natural by-product of planet formation. With the discovery of numerous extrasolar planets, it is likely that moons of extrasolar planets (exomoons) will soon be discovered. Some of the most promising techniques can yield both the mass and radius of the moon. Here, I review recent ideas about the formation of moons in our Solar System, and discuss the prospects of extrapolating these theories to predict the sizes of moons that may be discovered around extrasolar planets. It seems likely that planet-planet collisions could create satellites around rocky or icy planets which are large enough to be detected by currently available techniques. Detectable exomoons around gas giants may be able to form by co-accretion or capture, but determining the upper limit on likely moon masses at gas giant planets requires more detailed, modern simulations of these processes.

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Finding Planets via Gravitational Microlensing

Batista¹

2017

Handbook of Exoplanets

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MOA-2011-BLG-262Lb: A SUB-EARTH-MASS MOON ORBITING A GAS GIANT PRIMARY OR A HIGH VELOCITY PLANETARY SYSTEM IN THE GALACTIC BULGE

Abstract: Bennett et al.

Cited by 167 publications

References 89 publications

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Formation of exomoons: a solar system perspective

Finding Planets via Gravitational Microlensing

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