OGLE-2016-BLG-1093Lb: A Sub-Jupiter-mass Spitzer Planet Located in the Galactic Bulge

Shin, In-Gu; Yee, Jennifer C.; Hwang, Kyu-Ha; Gould, Andrew; Udalski, A.; Bond, I. A.; Albrow, M. D.; Chung, Sun-Ju; Han, Cheongho; Jung, Youn Kil; Kim, Hyoun Woo; Ryu, Yoon-Hyun; Shvartzvald, Yossi; Zang, Weicheng; Cha, Sang-Mok; Kim, Dong-Jin; Lee, Chung-Uk; Lee, Dong-Joo; Lee, Yongseok; Park, Byeong-Gon; Pogge, Richard W.; Mróz, P.; Szymański, M. K.; Skowron, J.; Poleski, R.; Soszyński, I.; Pietrukowicz, P.; Kozłowski, S.; Ulaczyk, K.; Beichman, Charles; Bryden, Geoffery; Novati, S. Calchi; Carey, Sean; Gaudi, B. Scott; Henderson, Calen B.; Zhu, Wei; Abe, F.; Barry, Richard; Bennett, D. P.; Bhattacharya, Aparna; Fujii, Hirosane; Fukui, A.; Hirao, Yuki; Itow, Y.; Kirikawa, Rintaro; Koshimoto, Naoki; Kondo, Iona; Matsubara, Y.; Matsumoto, Sho; Miyazaki, Shota; Muraki, Y.; Olmschenk, Greg; Okamura, Arisa; Ranc, Clément; Rattenbury, N. J.; Satoh, Yuki; Silva, Stela Ishitani; Sumi, T.; Suzuki, D.; Toda, Taiga; Tristram, P. J.; Vandorou, Aikaterini; Yama, Hibiki

doi:10.3847/1538-3881/ac6513

Cited by 4 publications

(1 citation statement)

References 55 publications

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“…When the background star is seen from outside of Earth, it crosses the caustics at different times. This has been observed with the Spitzer space telescope for OGLE-2016-BLG-1093Lb (Figure 6 - [20]). Since from the Moon the microlensing event is seen under an angle different from Earth, it will provide a better 2D characterization of the planet location respective to its parent star.…”

Section: Microlensing Detectionsupporting

confidence: 54%

OWL-Moon: Very high resolution spectropolarimetric interferometry and imaging from the Moon: exoplanets to cosmology

Silk¹,

Vakili

2022

Exp Astron

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We outline a concept for OWL-Moon, a 50-100m aperture telescope located on the surface of the Moon, to address three major areas in astronomy, namely the detection of biosignatures on habitable exoplanets, the geophysics of exoplanets, and cosmology. Such a large lunar telescope, when coupled with large Earth-based telescopes, would allow Intensity Interferometric measurements, leading to picoarcsecond angular resolution. This would have applications in many areas of astronomy and is timely in light of the renewed interest of space agencies in returning to the Moon.

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Section: Microlensing Detectionsupporting

confidence: 54%

OWL-Moon: Very high resolution spectropolarimetric interferometry and imaging from the Moon: exoplanets to cosmology

Silk¹,

Vakili

2022

Exp Astron

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Four sub-Jovian-mass planets detected by high-cadence microlensing surveys

Han

Kim

Gould

et al. 2022

A&A

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Aims. With the aim of finding short-term planetary signals, we investigated the data collected from current high-cadence microlensing surveys. Methods. From this investigation, we found four planetary systems with low planet-to-host mass ratios, including OGLE-2017-BLG-1691L, KMT-2021-BLG-0320L, KMT-2021-BLG-1303L, and KMT-2021-BLG-1554L. Despite the short durations, ranging from a few hours to a couple of days, the planetary signals were clearly detected by the combined data of the lensing surveys. We found that three of the planetary systems have mass ratios on the order of 10−4 and the other has a mass ratio that is slightly greater than 10−3. Results. The estimated masses indicate that all discovered planets have sub-Jovian masses. The planet masses of KMT-2021-BLG-0320Lb, KMT-2021-BLG-1303Lb, and KMT-2021-BLG-1554Lb correspond to ~0.10, ~0.38, and ~0.12 times the mass of the Jupiter, and the mass of OGLE-2017-BLG-1691Lb corresponds to that of the Uranus. The estimated mass of the planet host KMT-2021-BLG-1554L, Mhost ~ 0.08 M⊙, corresponds to the boundary between a star and a brown dwarf. Besides this system, the host stars of the other planetary systems are low-mass stars with masses in the range of ~[0.3–0.6] M⊙. The discoveries of the planets fully demonstrate the capability of the current high-cadence microlensing surveys in detecting low-mass planets.

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Precision measurement of a brown dwarf mass in a binary system in the microlensing event

Herald¹,

Udalski²,

Bozza³

et al. 2022

A&A

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Context. Brown dwarfs are transition objects between stars and planets that are still poorly understood, for which several competing mechanisms have been proposed to describe their formation. Mass measurements are generally difficult to carry out for isolated objects as well as for brown dwarfs orbiting low-mass stars, which are often too faint for a spectroscopic follow-up. Aims. Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here, we present an analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is caused by a binary system composed of a brown dwarf orbiting a red dwarf. Methods. Thanks to extensive ground observations and the availability of space observations from Spitzer, it has been possible to obtain accurate estimates of all microlensing parameters, including the parallax, source radius, and orbital motion of the binary lens. Results. Following an accurate modeling process, we found that the lens is composed of a red dwarf with a mass of M1 = 0.149 ± 0.010 M⊙ and a brown dwarf with a mass of M2 = 0.0463 ± 0.0031 M⊙ at a projected separation of a⊥ = 0.585 au. The system has a peculiar velocity that is typical of old metal-poor populations in the thick disk. A percent-level precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become more common in the future thanks to the Roman space telescope.

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OGLE-2016-BLG-1093Lb: A Sub-Jupiter-mass Spitzer Planet Located in the Galactic Bulge

Cited by 4 publications

References 55 publications

OWL-Moon: Very high resolution spectropolarimetric interferometry and imaging from the Moon: exoplanets to cosmology

OWL-Moon: Very high resolution spectropolarimetric interferometry and imaging from the Moon: exoplanets to cosmology

Four sub-Jovian-mass planets detected by high-cadence microlensing surveys

Precision measurement of a brown dwarf mass in a binary system in the microlensing event

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