Paper

OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting either a Late-Type Star or a Stellar Remnant

Miyazaki, Shota, Hibiki Yama, Fujii, Hirosane, Tristram, Paul J, Ranc, Clément, Pietrukowicz, Paweł, Skowron, Jan, Suzuki, Daisuke, Sumi, Takahiro, Satoh, Yuki K, Mio Tomoyoshi, Stela Ishitani Silva, Udalski, Andrzej, Rattenbury, Nicholas J, Matsubara, Yutaka, Barry, Richard, Yamashita, Kansuke, Abe, Fumio, Olmschenk, Greg, Vandorou, Aikaterini, Koshimoto, Naoki, Mróz, Przemek, Bennett, David P, Bond, Ian A, Kirikawa, Rintaro, Szymański, Michał K, Kozłowski, Szymon, Fukui, Akihiko, Itow, Yoshitaka, Soszyński, Igor, Bhattacharya, Aparna, Hirao, Yuki, Muraki, Yasushi, Hamada, Ryusei, Poleski, Radosław, Ulaczyk, Krzysztof

2023

Overview

We present the analysis of microlensing event OGLE-2014-BLG-0221, a planetary candidate event discovered in 2014. The photometric light curve is best described by a binary-lens single-source model. Our light curve modeling finds two degenerate models, with event timescales of \\(t_\\mathrm{E}\\sim70\\) days and \\(\\sim110\\) days. These timescales are relatively long, indicating that the discovered system would possess a substantial mass. The two models are similar in their planetary parameters with a Jupiter mass ratio of \\(q \\sim 10^{-3}\\) and a separation of \\(s \\sim 1.1\\). While the shorter timescale model shows marginal detection of a microlensing parallax signal, the longer timescale model requires a higher order effect of microlensing parallax, lens orbital motion or xallarap to explain the deviation in the light curve. However, the modeling shows significant correlation between the higher order effects and suffers the ecliptic degeneracy that results in a failure to determine the parallax parameters. Bayesian inference is used to estimate the physical parameters of the lens, revealing the lens to be either a late-type star supported by the shorter timescale model or a stellar remnant supported by the longer timescale model. If the lens is a remnant, this would be the second planet found by microlensing around a stellar remnant. Since the models predict different values for relative proper motion and source flux, future high angular resolution follow-up observations (e.g. Keck adaptive optics) are required to rule out either of the models.

• Publisher: Cornell University Library, arXiv.org
• Subject: Adaptive optics / Angular resolution / Astronomical models / Bayesian analysis / Binary stars / Companion stars / Extrasolar planets / Lenses / Light curve / Microlenses / Parallax / Parameters / Physical properties / Statistical inference / Time