The Exoplanet Mass-Ratio Function From the Moa-Ii Survey: Discovery of a Break and Likely Peak at a Neptune mass

Suzuki, D.; Bennett, D. P.; Sumi, T.; Bond, I. A.; Rogers, Leslie; Abe, F.; Asakura, Y.; Bhattacharya, Aparna; Donachie, M.; Freeman, Matthew; Fukui, A.; Hirao, Yuki; Itow, Y.; Koshimoto, Naoki; Li, M. C. A.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nagakane, M.; Onishi, Kyoko; Oyokawa, H.; Rattenbury, N. J.; Saito, To.; Sharan, A.; Shibai, Hiroshi; Sullivan, D. J.; Tristram, P. J.; Yonehara, A.

doi:10.3847/1538-4357/833/2/145

Cited by 255 publications

(290 citation statements)

References 139 publications

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“…This then sets the stage for whether its parallax is "adequately measured" according to the Zhu et al (2017b) criteria, or rather whether the corresponding 63 As a result, in microlensing statistical studies, the planet/brown-dwarf boundary is often defined by q. For example, Suzuki et al (2016;following Bond et al 2004) and Shvartzvald et al (2016) use q=0.03 and q=0.04, respectively, which would correspond to the conventional 13 M jup limit for stars of mass M;0.4 M e and M;0.3 M e , respectively. point-lens event would have satisfied them.…”

Section: Construction Of Blind Tests In the Facementioning

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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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: Construction Of Blind Tests In the Facementioning

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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“…Using a 1.8m telescope with a wide-field CCD camera, MOA-II monitors millions of stars simultaneously towards the densely populated regions of the GB. The rewards of collaborative efforts by MOA-II and other microlensing research groups include the discovery of E-mail: mli351@aucklanduni.ac.nz over 50 exoplanets (Suzuki et al 2016) and evidence for free-floating planets, which are not orbiting around any star (Ban et al 2016). The MOA-II project has also resulted in a large amount of photometric data, spanning over 8 years to date for variable objects which are worth categorization for future study.…”

Section: Introductionmentioning

confidence: 99%

The first eclipsing binary catalogue from the MOA-II data base

Rattenbury

Bond

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the first catalogue of eclipsing binaries in two MOA fields towards the Galactic bulge, in which over 8,000 candidates, mostly contact and semi-detached binaries of periods < 1 d, were identified. In this paper, the light curves of a small number of interesting candidates including eccentric binaries, binaries with noteworthy phase modulations and eclipsing RS CVn type stars are shown as examples. In addition, we identified three triple object candidates by detecting the light-travel-time effect in their eclipse time variation curves.

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“…To date, about 50 exoplanets have been found by microlensing thanks to their continuous effort. Several statistical studies have revealed the planet abundances beyond the snow line (Gould et al 2010;Sumi et al 2010;Cassan et al 2012;Shvartzvald et al 2016;Suzuki et al 2016). Suzuki et al (2016) found a possible peak in the mass ratio function and that cold Neptunes are likely to be the most common type of planets beyond the snow line.…”

Section: Introductionmentioning

confidence: 99%

“…Several statistical studies have revealed the planet abundances beyond the snow line (Gould et al 2010;Sumi et al 2010;Cassan et al 2012;Shvartzvald et al 2016;Suzuki et al 2016). Suzuki et al (2016) found a possible peak in the mass ratio function and that cold Neptunes are likely to be the most common type of planets beyond the snow line. Recently, Penny et al (2016) suggested that there exists a possible paucity of planets in the Galactic bulge from the sample of observed microlensing planets, though it appears that they have overestimated the detection efficiency for planets orbiting bulge stars.…”

Section: Introductionmentioning

confidence: 99%

OGLE-2013-BLG-1761Lb: A Massive Planet around an M/K Dwarf

Hirao

Udalski

Sumi

et al. 2017

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We report the discovery and the analysis of the planetary microlensing event, OGLE-2013-BLG-1761. There are some degenerate solutions in this event because the planetary anomaly is only sparsely sampled. However,the detailed lightcurve analysis ruled out all stellar binary models and shows the lens to be a planetary system. There is the so-called close/wide degeneracy in the solutions with the planet/host mass ratio of q∼(7.0±2.0)×10 −3 and q∼(8.1±2.6)×10−3 with the projected separation in Einstein radius units of s=0.95 (close) and s=1.18 (wide), respectively. The microlens parallax effect is not detected, but the finite source effect is detected. Our Bayesian analysis indicates that the lens system is located = . The preference of the large lens distance in the Bayesian analysis is due to the relatively large observed source star radius. The distance and other physical parameters may be constrained by the future high-resolution imaging by large groundtelescopes orHST. If the estimated lens distance is correct, thenthis planet provides another sample for testing the claimed deficit of planets in the Galactic bulge.-

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The Exoplanet Mass-Ratio Function From the Moa-Ii Survey: Discovery of a Break and Likely Peak at a Neptune mass

Cited by 255 publications

References 139 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 eclipsing binary catalogue from the MOA-II data base

OGLE-2013-BLG-1761Lb: A Massive Planet around an M/K Dwarf

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