Please note that eDoc will be permanently shut down in the first quarter of 2021!      Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 742689.0, MPI für Astronomie / Publikationen_mpia
OGLE-2016-BLG-0263Lb: Microlensing detection of a very low-mass binary companion through a repeating event channel
Authors:Han, C.; Udalski, A.; Gould, A.; Bond, I. A.; Albrow, M. D.; Chung, S. -. J.; Jung, Y. K.; Ryu, Y. -. H.; Shin, I. -. G.; Yee, J. C.; Zhu, W.; Cha, S. -. M.; Kim, S. -. L.; Kim, D. -. J.; Lee, C. -. U.; Lee, Y.; Park, B. -. G.; Skowron, J.; Mróz, P.; Pietrukowicz, P.; Kozłowski, S.; Poleski, R.; Szymański, M. K.; Soszyński, I.; Ulaczyk, K.; Pawlak, M.; Abe, F.; Asakura, Y.; Barry, R.; Bennett, D. P.; Bhattacharya, A.; Donachie, M.; Evans, P.; Fukui, A.; Hirao, Y.; Itow, Y.; Koshimoto, N.; Li, M. C. A.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nagakane, M.; Ohnishi, K.; Ranc, C.; Rattenbury, N. J.; Saito, T.; Sharan, A.; Sullivan, D. J.; Sumi, T.; Suzuki, D.; Tristram, P. J.; Yamada, T.; Yonehara, A.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:The Astronomical Journal
Issue / Number:4
Start Page:id. 133 (9 pp)
Audience:Not Specified
Abstract / Description:We report the discovery of a planet-mass companion to the microlens OGLE-2016-BLG-0263L. Unlike most low-mass companions that were detected through perturbations to the smooth and symmetric light curves produced by the primary, the companion was discovered through the channel of a repeating event, in which the companion itself produced its own single-mass light curve after the event produced by the primary had ended. Thanks to the continuous coverage of the second peak by high-cadence surveys, the possibility of the repeating nature due to source binarity is excluded with a 96% confidence level. The mass of the companion estimated by a Bayesian analysis is {M}{{p}}={4.1}-2.5+6.5 {M}{{J}}. The projected primary-companion separation is {a}\perp ={6.5}-1.9+1.3 au. The ratio of the separation to the snow-line distance of {a}\perp /{a}{sl}∼ 15.4 corresponds to the region beyond Neptune, the outermost planet of the solar system. We discuss the importance of high-cadence surveys in expanding the range of microlensing detections of low-mass companions and future space-based microlensing surveys.
Free Keywords:brown dwarfs; gravitational lensing: micro; planetary systems
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.