The TESS-Keck Survey. XV. Precise Properties of 108 TESS Planets and Their Host Stars

Creators: MacDougall, Mason G.; Petigura, Erik A.; Gilbert, Gregory J.; Angelo, Isabel; Batalha, Natalie M.; Beard, Corey; Behmard, Aida; Blunt, Sarah; Brinkman, Casey; Chontos, Ashley; Crossfield, Ian J. M.; Dai, Fei; Dalba, Paul A.; Dressing, Courtney; Fetherolf, Tara; Fulton, Benjamin; Giacalone, Steven; Hill, Michelle L.; Holcomb, Rae; Howard, Andrew W.; Huber, Daniel; Isaacson, Howard; Kane, Stephen R.; Kosiarek, Molly R.; Lubin, Jack; Mayo, Andrew; Močnik, Teo; Akana Murphy, Joseph M.; Pidhorodetska, Daria; Polanski, Alex S.; Rice, Malena; Robertson, Paul; Rosenthal, Lee J.; Roy, Arpita; Rubenzahl, Ryan A.; Scarsdale, Nicholas; Turtelboom, Emma V.; Tyler, Dakotah; Van Zandt, Judah; Weiss, Lauren M.; Yee, Samuel W.

Abstract

We present the stellar and planetary properties for 85 TESS Objects of Interest (TOIs) hosting 108 planet candidates that compose the TESS-Keck Survey (TKS) sample. We combine photometry, high-resolution spectroscopy, and Gaia parallaxes to measure precise and accurate stellar properties. We then use these parameters as inputs to a light-curve processing pipeline to recover planetary signals and homogeneously fit their transit properties. Among these transit fits, we detect significant transit-timing variations among at least three multiplanet systems (TOI-1136, TOI-1246, TOI-1339) and at least one single-planet system (TOI-1279). We also reduce the uncertainties on planet-to-star radius ratios R_p/R⋆ across our sample, from a median fractional uncertainty of 8.8% among the original TOI Catalog values to 3.0% among our updated results. With this improvement, we are able to recover the Radius Gap among small TKS planets and find that the topology of the Radius Gap among our sample is broadly consistent with that measured among Kepler planets. The stellar and planetary properties presented here will facilitate follow-up investigations of both individual TOIs and broader trends in planet properties, system dynamics, and the evolution of planetary systems.

Additional Information

© 2023. 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. M.M. acknowledges support from the UCLA Cota-Robles Graduate Fellowship. D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC21K0652), and the National Science Foundation (AST-1717000). D.D. acknowledges support from the TESS Guest Investigator Program grant 80NSSC22K0185 and NASA Exoplanet Research Program grant 18-2XRP18_2-0136. T.F. acknowledges support from the University of California President's Postdoctoral Fellowship Program. R.A.R. is supported by the NSF Graduate Research Fellowship, grant No. DGE 1745301. P.D. acknowledges support from a 51 Pegasi b Postdoctoral Fellowship from the Heising-Simons Foundation. J.M.A.M. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1842400. J.M.A.M. acknowledges 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. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the time assignment committees of the University of California, the California Institute of Technology, NASA, and the University of Hawaii for supporting the TESS-Keck Survey with observing time at Keck Observatory. We thank NASA for funding associated with our Key Strategic Mission Support project. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff for support of HIRES and remote observing. We recognize and acknowledge the cultural role and reverence that the summit of Maunakea has within the indigenous Hawaiian community. We are deeply grateful to have the opportunity to conduct observations from this mountain. This paper is based on data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We also acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This paper also includes data that are publicly available from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via 10.17909/t9-nmc8-f686 and 10.17909/fwdt-2x66. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. Facilities: TESS - , Keck/HIRES. - Software: We made use of the following publicly available Python modules: exoplanet (Foreman-Mackey et al. 2021), PyMC3 (Salvatier et al. 2016), theano (The Theano Development Team et al. 2016), celerite2 (Foreman-Mackey 2018), astropy (Astropy Collaboration et al. 2013, 2018), isoclassify (Huber et al. 2017), lightkurve (Lightkurve Collaboration et al. 2018), matplotlib (Hunter 2007), numpy (Harris et al. 2020), scipy (Virtanen et al. 2020), limb-darkening (Espinoza & Jordán 2015), SpecMatch-Synth (Petigura et al. 2017a), SpecMatch-Emp (Yee et al. 2017), and pandas (McKinney 2010).

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