OGLE-2018-BLG-1011L\lowercase{b,c}: Microlensing Planetary System with Two Giant Planets Orbiting a Low-mass Star
Creators: name: Han, Cheongho
name: Bennett, David P.
name: Udalski, Andrzej
name: Gould, Andrew
name: Bond, Ian A.
name: Shvartzvald, Yossi
name: Nikolaus, Kay-Sebastian
name: Hundertmark, Markus
name: Bozza, Valerio
name: Cassan, Arnaud
name: Hirao, Yuki
name: Bachelet, Etienne
name: Albrow, Michael D.
name: Chung, Sun-Ju
name: Hong, Kyeongsoo
name: Hwang, Kyu-Ha
name: Lee, Chung-Uk
name: Ryu, Yoon-Hyun
name: Shin, In-Gu
name: Yee, Jennifer C.
name: Jung, Youn Kil
name: Cha, Sang-Mok
name: Kim, Doeon
name: Kim, Dong-Jin
name: Kim, Hyoun-Woo
name: Kim, Seung-Lee
name: Lee, Dong-Joo
name: Lee, Yongseok
name: Park, Byeong-Gon
name: Mróz, Richard W. Pogge Przemek
name: Szymański, Michał K.
name: Skowron, Jan
name: Poleski, Radek
name: Soszyński, Igor
name: Pietrukowicz, Paweł
name: Kozłowski, Szymon
name: Ulaczyk, Krzysztof
name: Rybicki, Krzysztof A.
name: Iwanek, Patryk
name: Abe, Marcin Wrona Fumio
name: Barry, Richard
name: Bhattacharya, Aparna
name: Donachie, Martin
name: Fukui, Akihiko
name: Itow, Yoshitaka
name: Kawasaki, Kohei
name: Kondo, Iona
name: Koshimoto, Naoki
name: Li, Man Cheung Alex
name: Matsubara, Yutaka
name: Muraki, Yasushi
name: Miyazaki, Shota
name: Nagakane, Masayuki
name: Ranc, Clément
name: Rattenbury, Nicholas J.
name: Suematsu, Haruno
name: Sumi, Denis J. Sullivan Takahiro
name: Suzuki, Daisuke
name: Tristram, Paul J.
name: Yonehara, Atsunori
name: Fouqué, Pascal
name: Mao, Shude
name: Wang, Tianshu
name: Zang, Weicheng
name: Zhu, Wei
name: Penny, Matthew T.
name: Beichman, Charles A.
name: Bryden, Geoffery
name: Novati, Sebastiano Calchi
name: Gaudi, B. Scott
name: Henderson, Calen B.
name: Jacklin, Savannah
name: Stassun, Keivan G.
Publisher: name: arXiv
Year: 2019
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We report a multiplanetary system found from the analysis of microlensing event OGLE-2018-BLG-1011, for which the light curve exhibits a double-bump anomaly around the peak. We find that the anomaly cannot be fully explained by the binary-lens or binary-source interpretations and its description requires the introduction of an additional lens component. The 3L1S (3 lens components and a single source) modeling yields three sets of solutions, in which one set of solutions indicates that the lens is a planetary system in a binary, while the other two sets imply that the lens is a multiplanetary system. By investigating the fits of the individual models to the detailed light curve structure, we find that the multiple-planet solution with planet-to-host mass ratios $\sim 9.5\times 10^{-3}$ and $\sim 15\times 10^{-3}$ are favored over the other solutions. From the Bayesian analysis, we find that the lens is composed of two planets with masses $1.8^{+3..4}_{-1.1}~M_{\rm J}$ and $2.8^{+5.1}_{-1.7}~M_{\rm J}$ around a host with a mass $0.18^{+0.33}_{-0.10}~M_\odot$ and located at a distance $7.1^{+1.1}_{-1.5}~{\rm kpc}$. The estimated distance indicates that the lens is the farthest system among the known multiplanetary systems. The projected planet-host separations are $a_{\perp,2}=1.8^{+2.1}_{-1.5}~{\rm au}$ ($0.8^{+0.9}_{-0.6}~{\rm au}$) and $a_{\perp,3}=0.8^{+0.9}_{-0.6}~{\rm au}$, where the values of $a_{\perp,2}$ in and out the parenthesis are the separations corresponding to the two degenerate solutions, indicating that both planets are located beyond the snow line of the host, as with the other four multiplanetary systems previously found by microlensing.
description: 14 pages, 18 figures, 8 tables