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

Abstract 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>p</mml:mi> </mml:mrow> </mml:msub> <mml:mi>sin</mml:mi> <mml:mi>i</mml:mi> <mml:mo>=</mml:mo> </mml:math> 70–4000 M ⊕ = 0.2–12.5 M J , and required transiting planets to have a &lt; 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) = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mn>31</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>11</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>12</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> %, over the field rate of P(DG) = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>1</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>%</mml:mo> </mml:math> . 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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Journal
The Astronomical Journal
Published
2025-04-01
DOI
https://doi.org/10.3847/1538-3881/adbbed
Citations
8
Primary Topic
Stellar, planetary, and galactic studies
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article
Field-Weighted Citation Impact
9.24

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article

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

Howard Isaacson, Jack Lubin, Andrew W. Mayo, Stephen R. Kane et al.
8 citations
The Astronomical Journal
Stellar, planetary, and galactic studies
9.24
article

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

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

Abstract

Abstract 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>p</mml:mi> </mml:mrow> </mml:msub> <mml:mi>sin</mml:mi> <mml:mi>i</mml:mi> <mml:mo>=</mml:mo> </mml:math> 70–4000 M ⊕ = 0.2–12.5 M J , and required transiting planets to have a &lt; 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) = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mn>31</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>11</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>12</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> %, over the field rate of P(DG) = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>1</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>6</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>%</mml:mo> </mml:math> . 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.

The Astronomical JournalVol. 169(5)
University of California, Riverside (US), University of Notre Dame (US), California Institute of Technology (US), Ames Research Center (US), The University of Sydney (AU), Space Telescope Science Institute (US), University of Hawaii System (US), American Museum of Natural History (US), Johns Hopkins University (US), University of Kansas (US), University of California, Los Angeles (US), University of California, Santa Cruz (US), University of Toronto (CA), University of Southern Queensland (AU), Princeton University (US), University of California, Irvine (US), NASA Exoplanet Science Institute (US), Gemini North Observatory (US), Université Bourgogne Franche-Comté (FR), Flatiron Health (United States) (US), Flatiron Institute (US), University of California, Berkeley (US)
NASA Exoplanet Science Institute
Openalex Percentile: Top 2%
Stellar, planetary, and galactic studies
9.24
DOIOpen Access PDFOpenAlex
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