The Astronomical Journal (Jan 2025)

The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets

  • Judah Van Zandt,
  • Erik A. Petigura,
  • Jack Lubin,
  • Lauren M. Weiss,
  • Emma V. Turtelboom,
  • Tara Fetherolf,
  • Joseph M. Akana Murphy,
  • Ian J. M. Crossfield,
  • Gregory J. Gilbert,
  • Teo Močnik,
  • Natalie M. Batalha,
  • Courtney Dressing,
  • Benjamin Fulton,
  • Andrew W. Howard,
  • Daniel Huber,
  • Howard Isaacson,
  • Stephen R. Kane,
  • Paul Robertson,
  • Arpita Roy,
  • Isabel Angelo,
  • Aida Behmard,
  • Corey Beard,
  • Ashley Chontos,
  • Fei Dai,
  • Steven Giacalone,
  • Michelle L. Hill,
  • Rae Holcomb,
  • Steve B. Howell,
  • Andrew W. Mayo,
  • Daria Pidhorodetska,
  • Alex S. Polanski,
  • James Rogers,
  • Lee J. Rosenthal,
  • Ryan A. Rubenzahl,
  • Nicholas Scarsdale,
  • Dakotah Tyler,
  • Samuel W. Yee,
  • Jon Zink

DOI
https://doi.org/10.3847/1538-3881/adbbed
Journal volume & issue
Vol. 169, no. 5
p. 235

Abstract

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We present the results of the Distant Giants Survey, a 3 yr radial velocity (RV) campaign to search for wide-separation giant planets orbiting Sun-like stars known to host an inner transiting planet. We defined a distant giant (DG) to have a = 1–10 au and ${M}_{p}\sin i=$ 70–4000 M _⊕ = 0.2–12.5 M _J , and required transiting planets to have a < 1 au and R _p = 1–4 R _⊕ . We assembled our sample of 47 stars using a single selection function and observed each star at monthly intervals to obtain ≈30 RV observations per target. The final catalog includes a total of 12 distant companions: four giant planets detected during our survey, two previously known giant planets, and six objects of uncertain disposition identified through RV/astrometric accelerations. Statistically, half of the uncertain objects are planets and the remainder are stars/brown dwarfs. We calculated target-by-target completeness maps to account for missed planets. We found evidence for a moderate enhancement of DGs in the presence of close-in small planets (CSs), P(DG∣CS) = ${31}_{-11}^{+12}$ %, over the field rate of P(DG) = $1{6}_{-2}^{+2} \% $ . No enhancement is disfavored ( p ∼ 8%). In contrast to a previous study, we found no evidence that stellar metallicity raises the enhancement of P(DG∣CS) over P(DG). We found evidence that DG companions preferentially accompany shorter-period CS planets and have lower eccentricities than randomly selected giant planets. This points toward a nuanced picture of dynamically cool formation in which giants interact with, but do not disrupt, their inner systems.

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