The TESS-Keck Survey. III. A Stellar Obliquity Measurement of TOI-1726 c
- Creators
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Dai, Fei
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Roy, Arpita
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Fulton, Benjamin
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Robertson, Paul
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Hirsch, Lea
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Isaacson, Howard
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Albrecht, Simon
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Mann, Andrew W.
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Kristiansen, Martti H.
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Batalha, Natalie M.
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Beard, Corey
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Behmard, Aida
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Chontos, Ashley
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Crossfield, Ian J. M.
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Dalba, Paul A.
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Dressing, Courtney
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Giacalone, Steven
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Hill, Michelle
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Howard, Andrew W.
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Huber, Daniel
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Kane, Stephen R.
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Kosiarek, Molly R.
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Lubin, Jack
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Mayo, Andrew
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Mocnik, Teo
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Murphy, Joseph M. Akana
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Petigura, Erik A.
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Rosenthal, Lee
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Rubenzahl, Ryan A.
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Scarsdale, Nicholas
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Weiss, Lauren M.
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Van Zandt, Judah
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Ricker, George R.
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Vanderspek, Roland
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Latham, David W.
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Seager, Sara
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Winn, Joshua N.
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Jenkins, Jon M.
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Caldwell, Douglas A.
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Charbonneau, David
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Daylan, Tansu
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Günther, Maximilian N.
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Morgan, Edward
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Quinn, Samuel N.
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Rose, Mark E.
- Smith, Jeffrey C.
Abstract
We report the measurement of a spectroscopic transit of TOI-1726c, one of two planets transiting a G-type star with V = 6.9 in the Ursa Major Moving Group (~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)∘. 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 multitransiting 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⊕ and c 2.7 R⊕ both likely underwent photoevaporation). The coplanar geometry points to a dynamically cold history of the system that simplifies any future modeling of atmospheric escape.
Additional Information
© 2020 The American Astronomical Society. Received 2020 May 6; revised 2020 August 19; accepted 2020 August 27; published 2020 September 30. We thank the time assignment committee of the University of California for observing time on the Automated Planet Finder for the TESS-Keck Survey. We thank NASA for funding associated with our Key Strategic Mission Support project for TESS–Keck–Survey. We thank Ken and Gloria Levy, who supported the construction of the Levy Spectrometer on the Automated Planet Finder. We thank the University of California and Google for supporting Lick Observatory and the UCO staff for their dedicated work scheduling and operating the telescopes of Lick Observatory. This paper is based on data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. T.D. acknowledges support from MIT's Kavli Institute as a Kavli postdoctoral fellow. M.N.G. acknowledges support from MIT's Kavli Institute as a Torres postdoctoral fellow. P.D. acknowledges support from a National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1903811. J.M.A.M. gratefully acknowledges support from the National Science Foundation Graduate Research Fellowship under grant No. DGE-1842400. J.M.A.M. also thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining grant No. 1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. M.H.K. acknowledges Allan R. Schmitt for making his light curve examining software LcTools freely available. D.C. was supported by a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. S.A. acknowledges the support from the Danish Council for Independent Research through the DFF Sapere Aude Starting grant No. 4181-00487B, and the Stellar Astrophysics Centre which funding is provided by The Danish National Research Foundation (grant agreement No.: DNRF106). Facilities: Automated Planet Finder (Levy) - , TESS. - Software: Batman (Kreidberg 2015), Emcee (Foreman-Mackey et al. 2013), EXOFAST (Eastman et al. 2013), Isoclassify (Huber 2017), lmfit(Newville et al. 2014) SpecMatch (Petigura 2015; Yee et al. 2017).Attached Files
Published - Dai_2020_AJ_160_193.pdf
Submitted - 2008.12397.pdf
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Additional details
- Alternative title
- TKS III: A Stellar Obliquity Measurement of TOI-1726 c
- Eprint ID
- 105413
- Resolver ID
- CaltechAUTHORS:20200916-112854779
- NASA/JPL/Caltech
- Ken and Gloria Levy
- University of California
- Massachusetts Institute of Technology (MIT)
- Kavli Foundation
- NSF Astronomy and Astrophysics Fellowship
- AST-1903811
- NSF Graduate Research Fellowship
- DGE-1842400
- LSSTC Institutional Members
- NSF
- OAC-1829740
- Brinson Foundation
- Gordon and Betty Moore Foundation
- John Templeton Foundation
- Danish Council for Independent Research
- 4181-00487B
- Danish National Research Foundation
- DNRF106
- Created
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2020-09-23Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department, Infrared Processing and Analysis Center (IPAC)