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Spin–Orbit Geometry of AU Mic b and c from Back-to-back Transits Observed Contemporaneously with Magellan PFS, LCOGT, and CHEOPS

  • Authors: Zitao Lin, Gyula M. Szabó, Krzysztof Sz. Zieliński, Zhen Guo, Zoltán Garai, R. Paul Butler, Alexis Brandeker, Johanna K. Teske, Davide Gandolfi, Haochuan Yu, Nicolas Billot, Suzanne Aigrain, Michael Cretignier, Liang Wang, Xuan Mao, Wei M. Yuan, Hongpeng Lu, Jiayin Li, Yann Alibert, Ádám Boldog, Vincent Bourrier, Giovanni Bruno, Jeffrey D. Crane, Fei Dai, Olivier D. S. Demangeon, Alexis Heitzmann, Zhecheng Hu, Pradip Karmakar, Levente Kriskovics, Monika Lendl, He Y. Liu, Pierre F. L. Maxted, Hugh P. Osborn, Gaetano Scandariato, Stephen A. Shectman, Sérgio G. Sousa, Soléne Ulmer-Moll, Mu-Tian Wang, Thomas G. Wilson, Sharon X. Wang

Zitao Lin et al 2026 The Astrophysical Journal Letters 1005 .

  • Provider: AAS Journals

Caption: Figure 3.

Transit fitting results for AU Mic b and c. For AU Mic c, three fits using different flare-masking choices are presented. Blue dots represent the data used in the fit, while red dots indicate masked data points. The solid black lines represent the best-fit transit models using the W23 prior. For the detrended CHEOPS data, additional best-fit models using alternative priors are shown as solid and dashed gray lines; these exhibit only marginal deviations from each other. Priors used: W23: based on J. M. Wittrock et al. (2023); B25-22 and B25-23: based on 2022 and 2023 values of Á. Boldog et al. (2025), respectively.

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