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Published June 2022 | Published + Accepted Version
Journal Article Open

An Aligned Orbit for the Young Planet V1298 Tau b

Abstract

The alignment of planetary orbits with respect to the stellar rotation preserves information on their dynamical histories. Measuring this angle for young planets helps illuminate the mechanisms that create misaligned orbits for older planets, as different processes could operate over timescales ranging from a few megayears to a gigayear. We present spectroscopic transit observations of the young exoplanet V1298 Tau b; we update the age of V1298 Tau to be 28 ± 4 Myr based on Gaia EDR3 measurements. We observed a partial transit with Keck/HIRES and LBT/PEPSI, and detected the radial velocity anomaly due to the Rossiter–McLaughlin effect. V1298 Tau b has a prograde, well-aligned orbit, with λ = 4 − 10 + 7 deg. By combining the spectroscopically measured v sin i ⋆ and the photometrically measured rotation period of the host star we also find that the orbit is aligned in 3D, ψ = 8 − 7 + 4 deg. Finally, we combine our obliquity constraints with a previous measurement for the interior planet V1298 Tau c to constrain the mutual inclination between the two planets to be i mut = 0° ± 19°. This measurements adds to the growing number of well-aligned planets at young ages, hinting that misalignments may be generated over timescales of longer than tens of megayears. The number of measurements, however, is still small, and this population may not be representative of the older planets that have been observed to date. We also present the derivation of the relationship between i mut, λ, and i for the two planets.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 October 7; revised 2022 March 10; accepted 2022 March 16; published 2022 May 4. Thanks to Adina Feinstein, Ben Montet, and Elisabeth Newton for useful discussions. We thank the other observers who contributed some of our observations or helped with the planning of the observations: David Latham, Samuel Quinn, and Andrew Howard. Thanks to Josh Walawender for supporting our Keck observations. This work was supported by a NASA Keck PI Data Award through JPL RSA 1634873. P.D. is supported by a National Science Foundation (NSF) Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1903811. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. The LBT is an international collaboration among institutions in the United States, Italy and Germany. The LBT Corporation partners are: The Ohio State University; LBT Beteiligungsgesellschaft, Germany, representing the Max Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota and University of Virginia. This paper includes data collected by the K2 mission. Funding for the K2 mission is provided by the NASA Science Mission directorate. This work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Facility: Keck:I (HIRES), LBT (PEPSI), FLWO1.5 m (TRES), Kepler, Spitzer. Software: astropy (Astropy Collaboration et al. 2013, 2018), celerite2 (Foreman-Mackey et al. 2017; Foreman-Mackey 2018), everest (Luger et al. 2016, 2018), exoplanet (Foreman-Mackey et al. 2019, 2021), jupyter (Kluyver et al. 2016), matplotlib (Hunter 2007), misttborn (Johnson et al. 2017), numpy (van der Walt et al. 2011), pandas (pandas development team 2020; Wes McKinney 2010), pymc3 (Salvatier et al. 2016), seaborn (Waskom et al. 2017), starry (Luger et al. 2019), theano (Theano Development Team 2016).

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Published - Johnson_2022_AJ_163_247.pdf

Accepted Version - 2110.10707.pdf

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Additional details

Created:
August 22, 2023
Modified:
October 24, 2023