TESS-Keck Survey. XIV. Two Giant Exoplanets from the Distant Giants Survey

Creators: Van Zandt, Judah; Petigura, Erik A.; MacDougall, Mason; Gilbert, Gregory J.; Lubin, Jack; Barclay, Thomas; Batalha, Natalie M.; Crossfield, Ian J. M.; Dressing, Courtney; Fulton, Benjamin; Howard, Andrew W.; Huber, Daniel; Isaacson, Howard; Kane, Stephen R.; Robertson, Paul; Roy, Arpita; Weiss, Lauren M.; Behmard, Aida; Beard, Corey; Chontos, Ashley; Dai, Fei; Dalba, Paul A.; Fetherolf, Tara; Giacalone, Steven; Henze, Christopher E.; Hill, Michelle L.; Hirsch, Lea A.; Holcomb, Rae; Howell, Steve B.; Jenkins, Jon M.; Latham, David W.; Mayo, Andrew; Mireles, Ismael; Močnik, Teo; Murphy, Joseph M. Akana; Pidhorodetska, Daria; Polanski, Alex S.; Ricker, George R.; Rosenthal, Lee J.; Rubenzahl, Ryan A.; Seager, S.; Scarsdale, Nicholas; Turtelboom, Emma V.; Vanderspek, Roland; Winn, Joshua N.

Abstract

We present the Distant Giants Survey, a three-year radial velocity campaign to measure P(DG|CS), the conditional occurrence of distant giant planets (DG; M_p ∼ 0.3–13 M_J, P > 1 yr) in systems hosting a close-in small planet (CS; R_p < 10 R_⊕). For the past two years, we have monitored 47 Sun-like stars hosting small transiting planets detected by TESS. We present the selection criteria used to assemble our sample and report the discovery of two distant giant planets, TOI-1669 b and TOI-1694 c. For TOI-1669 b we find that M sin i = 0.573 ± 0.074 M_J, P = 502 ± 16 days, and e < 0.27, while for TOI-1694 c, M sin i = 1.05 ± 0.05 M_J, P = 389.2 ± 3.9 days, and e = 0.18 ± 0.05. We also confirmed the 3.8 days transiting planet TOI-1694 b by measuring a true mass of M = 26.1 ± 2.2 M_⊕. At the end of the Distant Giants Survey, we will incorporate TOI-1669 b and TOI-1694 c into our calculation of P(DG|CS), a crucial statistic for understanding the relationship between outer giants and small inner companions.

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. J.V.Z. acknowledges support from the Future Investigators in NASA Earth and Space Science and Technology (FINESST) grant 80NSSC22K1606. 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. T.F. acknowledges support from the University of California President's Postdoctoral Fellowship Program. 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 and on the Automated Planet Finder. 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. 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 for supporting Lick Observatory and the UCO staff for their dedicated work scheduling and operating the telescopes of Lick Observatory. Funding for the TESS mission is provided by NASA's Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center at NASA Ames Research Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Facilities: Automated Planet Finder (Levy) - , Keck I (HIRES) - , Gemini-North ('Alopeke) - , TESS. - Software: radvel (Fulton et al. 2018), emcee (Foreman-Mackey et al. 2013), SpecMatch (Petigura et al. 2017).

Attached Files

Published - Van_Zandt_2023_AJ_165_60.pdf

Files

Van_Zandt_2023_AJ_165_60.pdf

Files (1.9 MB)

Name	Size	Download all
Van_Zandt_2023_AJ_165_60.pdf md5:8feafa5aa8989bc41a1744094bf2e4e0	1.9 MB	Preview Download

Additional details

	All versions	This version
Views	0	0
Downloads	0	0
Data volume	0 Bytes	0 Bytes