The TESS-Keck Survey. III. A Stellar Obliquity Measurement of TOI-1726 c,The Astronomical Journal

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The TESS-Keck Survey. III. A Stellar Obliquity Measurement of TOI-1726 c
The Astronomical Journal ( IF 5.3 ) Pub Date : 2020-09-30 , DOI: 10.3847/1538-3881/abb3bd
Fei Dai ₁ , Arpita Roy ₂ , Benjamin Fulton ₃ , Paul Robertson ₄ , Lea Hirsch ₅ , Howard Isaacson ₆ , Simon Albrecht ₇ , Andrew W. Mann ₈ , Martti H. Kristiansen _{9,

10} , Natalie M. Batalha ₁₁ , Corey Beard ₄ , Aida Behmard ₁ , Ashley Chontos ₁₂ , Ian J. M. Crossfield ₁₃ , Paul A. Dalba ₁₄ , Courtney Dressing ₆ , Steven Giacalone ₆ , Michelle Hill ₁₄ , Andrew W. Howard ₁₅ , Daniel Huber ₁₂ , Stephen R. Kane ₁₄ , Molly Kosiarek ₁₁ , Jack Lubin ₄ , Andrew Mayo ₆ , Teo Mocnik ₁₆ , Joseph M. Akana Murphy ₁₁ , Erik A. Petigura ₁₇ , Lee Rosenthal ₂ , Ryan A. Rubenzahl ₂ , Nicholas Scarsdale ₁₁ , Lauren M. Weiss ₁₂ , Judah Van Zandt ₁₇ , George R. Ricker ₁₈ , Roland Vanderspek ₁₈ , David W. Latham ₁₉ , Sara Seager _{18,

20,

21} , Joshua N. Winn ₂₂ , Jon M. Jenkins ₂₃ , Douglas A. Caldwell _{23,

24} , David Charbonneau ₁₉ , Tansu Daylan ₂₅ , Maximilian N. Gnther ₂₅ , Edward Morgan ₂₁ , Samuel N. Quinn ₁₉ , Mark E. Rose ₂₃ , Jeffrey C. Smith _{23,

24}

Affiliation

Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA
Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
NASA Exoplanet Science Institute/Caltech-IPAC, MC 314-6, 1200 E. California Blvd., Pasadena, CA 91125, USA
Department of Physics & Astronomy, The University of California, Irvine, Irvine, CA 92697, USA
Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA, USA
501 Campbell Hall, University of California at Berkeley, Berkeley, CA 94720, USA
Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
Department of Physics and Astronomy, The University of North Carolina at Chapel Hill, Chapel Hill, NC 27599, USA
Brorfelde Observatory, Observator Gyldenkernes Vej 7, DK-4340 Tllse, Denmark
DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark
Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95060, USA
Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Dr., Honolulu, HI 96822, USA
Department of Physics and Astronomy, University of Kansas, Lawrence, KS, USA
Department of Earth and Planetary Sciences, University of California, Riverside, CA 92521, USA
California Institute of Technology, Pasadena, CA 91125, USA
Gemini Observatory Northern Operations, 670 N. A’ohoku Pl., Hilo, HI 96720, USA
Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA
Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Center for Astrophysics∣Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA
Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Department of Aeronautics and Astronautics, MIT, 77 Massachusetts Ave., Cambridge, MA 02139, USA
Department of Astrophysical Sciences, Princeton University, 4 Ivy Ln., Princeton, NJ 08544, USA
NASA Ames Research Center, Moffett Field, CA 94035, USA
SETI Institute, Mountain View, CA, USA
Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 70 Vassar St., Cambridge, MA 02139, USA

We report the measurement of a spectroscopic transit of TOI-1726 c, one of two planets transiting a G-type star with $V$ = 6.9 in the Ursa Major Moving Group ($\sim$400 Myr). With a precise age constraint from cluster membership, TOI-1726 provides a great opportunity to test various obliquity excitation scenarios that operate on different timescales. By modeling the Rossiter-McLaughlin (RM) effect, we derived a sky-projected obliquity of $-1^{+35}_{-32}~^{\circ}$. This result rules out a polar/retrograde orbit; and is consistent with an aligned orbit for planet c. Considering the previously reported, similarly prograde RM measurement of planet b and the transiting nature of both planets, TOI-1726 tentatively conforms to the overall picture that compact multi-transiting planetary systems tend to have coplanar, likely aligned orbits. TOI-1726 is also a great atmospheric target for understanding differential atmospheric loss of sub-Neptune planets (planet b 2.2 $R_\oplus$ and c 2.7 $R_\oplus$ both likely underwent photoevaporation). The coplanar geometry points to a dynamically cold history of the system that simplifies any future modeling of atmospheric escape.

中文翻译：

TESS-Keck 调查。三、TOI-1726 c 的恒星倾角测量

我们报告了 TOI-1726 c 光谱凌日的测量结果，这是在大熊座移动群 ($\sim$400 Myr) 中过境 G 型恒星的两颗行星之一，其中 $V$ = 6.9。TOI-1726 具有来自集群成员的精确年龄限制，提供了一个很好的机会来测试在不同时间尺度上运行的各种倾斜激发场景。通过对 Rossiter-McLaughlin (RM) 效应建模，我们推导出了 $-1^{+35}_{-32}~^{\circ}$ 的天空投影倾角。这个结果排除了极地/逆行轨道；并且与行星 c 的对齐轨道一致。考虑到先前报道的行星 b 的类似顺行 RM 测量以及两颗行星的凌日性质，TOI-1726 暂时符合整体图景，即紧凑的多凌日行星系统往往具有共面的、可能对齐的轨道。TOI-1726 也是了解亚海王星行星（行星 b 2.2 $R_\oplus$ 和 c 2.7 $R_\oplus$ 都可能经历了光蒸发）的大气差异损失的重要大气目标。共面几何指向系统的动态冷历史，简化了未来大气逃逸的任何建模。

更新日期：2020-09-30

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