MASSES AND ORBITAL CONSTRAINTS FOR THE OGLE-2006-BLG-109Lb,c JUPITER/SATURN ANALOG PLANETARY SYSTEM

Bennett, D. P.; Rhie, Sun Hong; Nikolaev, Sergei; Gaudi, B. Scott; Udalski, A.; Gould, Andrew; Christie, Grant; Maoz, Dan; Dong, Subo; McCormick, J.; Szymański, M. K.; Tristram, P. J.; Macintosh, Bruce; Cook, K. H.; Kubiak, M.; Pietrzyński, G.; Soszyński, I.; Szewczyk, O.; Ulaczyk, K.; Wyrzykowski, Ł.; DePoy, D. L.; Han, Cheongho; Kaspi, S.; Lee, Chung-Uk; Mallia, F.; Natusch, T.; Park, B.-G.; Pogge, Richard W.; Polishook, David; Abe, F.; Bond, I. A.; Botzler, C. S.; Fukui, A.; Hearnshaw, John; Itow, Y.; Kamiya, K.; Korpela, A.; Kilmartin, P. M.; Lin, Wei; Ling, J. F.; Masuda, K.; Matsubara, Y.; Motomura, M.; Muraki, Y.; Nakamura, Satoko; Okumura, Teppei; Ohnishi, Kouhei; Perrott, Y. C.; Rattenbury, N. J.; Sako, T.; Saito, To.; Sato, S.; Skuljan, L.; Sullivan, D. J.; Sumi, T.; Sweatman, W. L.; Yock, P. C. M.; Albrow, M. D.; Allan, A.; Beaulieu, J. P.; Bramich, D. M.; Burgdorf, M.; Coutures, C.; Dominik, M.; Dieters, S.; Fouqué, P.; Greenhill, J.; Horne, K.; Snodgrass, C.; Steele, I. A.; Tsapras, Y.; Chaboyer, Brian; Crocker, Alison F.; Frank, and S.

doi:10.1088/0004-637x/713/2/837

Cited by 160 publications

(118 citation statements)

References 91 publications

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“…One might argue that the previously mentioned noisiness of the signals will make it difficult to measure frequency differences accurately, but it should still give us a rough idea of the configuration of the system. In this regard, the situation can be likened to other known cases where planetary properties have not been measured to high accuracy (e.g., OGLE-2006-BLG-109 L c has a semimajor axis of 4.5 ± 2.2 au; Bennett et al 2010), and yet still give great insight into the inner structure of the system.…”

Section: Physical Properties Derived From Multiple Detectionsmentioning

confidence: 99%

On the Radio Detection of Multiple-Exomoon Systems Due to Plasma Torus Sharing

Noyola

Satyal

Musielak³

2016

ApJ

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The idea of single exomoon detection due to the radio emissions caused by its interaction with the host exoplanet is extended to multiple-exomoon systems. The characteristic radio emissions are made possible in part by plasma from the exomoon's own ionosphere. In this work, it is demonstrated that neighboring exomoons and the exoplanetary magnetosphere could also provide enough plasma to generate a detectable signal. In particular, the plasma-torus-sharing phenomenon is found to be particularly well suited to facilitate the radio detection of plasmadeficient exomoons. The efficiency of this process is evaluated, and the predicted power and frequency of the resulting radio signals are presented.

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Section: Physical Properties Derived From Multiple Detectionsmentioning

confidence: 99%

On the Radio Detection of Multiple-Exomoon Systems Due to Plasma Torus Sharing

Noyola

Satyal

Musielak³

2016

ApJ

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“…The exception is OGLE-2006-BLG-109La,b, the first twoplanet system found by microlensing (Gaudi et al 2008;Bennett et al 2010). Due to the very large caustic from one of the planets, together with a data rate that was very high and continuous for that time, Bennett et al (2010) were able to introduce one additional dynamical parameter relative to the standard two-dynamical parameter approach of Albrow et al (2000). This allowed them to make RV predictions for the system that could be tested with future 30 m class telescopes.…”

Section: Full Kepler Orbits In Microlensingmentioning

confidence: 99%

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

Ryu¹,

Yee²,

Udalski³

et al. 2017

Self Cite

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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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“…Yet actual yields of very tight binaries have been small due to the inherent inefficiencies associated with these search programs: RV monitoring programs require large allocations of large telescope time, while searches for overluminous sources need clusters and long-term astrometric programs to confirm object membership. Other signatures of unresolved multiplicity, such as eclipsing (e.g., Stassun et al 2006), astrometric wobble (e.g., Dahn et al 2008), and microlensing (e.g., Bennett et al 2010) have similarly yielded few detections.…”

Section: Introductionmentioning

confidence: 99%

2mass J20261584–2943124: An Unresolved L0.5 + T6 Spectral Binary

Gelino¹,

Burgasser²

2010

The Astronomical Journal

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We identify the L dwarf 2MASS J20261584−2943124 as an unresolved spectral binary, based on low-resolution, near-infrared spectroscopy from IRTF/SpeX. The data reveal a peculiar absorption feature at 1.6 μm, previously noted in the spectra of other very low-mass spectral binaries, which likely arises from overlapping FeH and CH 4 absorption bands in the blended light of an L dwarf/T dwarf pair. Spectral template matching analysis indicates component types of L0.5 and T6, with relative brightness ΔH = 4.2 ± 0.6. Laser guide star adaptive optics imaging observations with Keck/NIRC2 fail to resolve the source, indicating a maximum separation at the observing epoch of 0. 25, or a projected separation of 9 AU assuming a distance of 36 ± 5 pc. With an age that is likely to be relatively older ( 5 Gyr) based on the system's large V tan and mass ratio arguments, the relative motion of the potentially "massive" (0.06-0.08 M ) components of 2MASS J2026−2943 may be detectable through radial velocity variations, like its earlier-type counterpart 2MASS J03202839−0446358 (M8+T5), providing dynamical mass measurements that span the hydrogen burning limit.

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MASSES AND ORBITAL CONSTRAINTS FOR THE OGLE-2006-BLG-109Lb,c JUPITER/SATURN ANALOG PLANETARY SYSTEM

Cited by 160 publications

References 91 publications

On the Radio Detection of Multiple-Exomoon Systems Due to Plasma Torus Sharing

On the Radio Detection of Multiple-Exomoon Systems Due to Plasma Torus Sharing

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

2mass J20261584–2943124: An Unresolved L0.5 + T6 Spectral Binary

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