May
2025
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2025AJ....169..235V
Authors
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Van Zandt, Judah
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Petigura, Erik A.
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Lubin, Jack
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Weiss, Lauren M.
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Turtelboom, Emma V.
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Fetherolf, Tara
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Murphy, Joseph M. Akana
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Crossfield, Ian J. M.
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Gilbert, Gregory J.
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Močnik, Teo
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Batalha, Natalie M.
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Dressing, Courtney
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Fulton, Benjamin
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Howard, Andrew W.
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Huber, Daniel
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Isaacson, Howard
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Kane, Stephen R.
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Robertson, Paul
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Roy, Arpita
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Angelo, Isabel
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Behmard, Aida
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Beard, Corey
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Chontos, Ashley
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Dai, Fei
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Giacalone, Steven
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Hill, Michelle L.
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Holcomb, Rae
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Howell, Steve B.
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Mayo, Andrew W.
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Pidhorodetska, Daria
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Polanski, Alex S.
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Rogers, James
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Rosenthal, Lee J.
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Rubenzahl, Ryan A.
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Scarsdale, Nicholas
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Tyler, Dakotah
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Yee, Samuel W.
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Zink, Jon
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 70–4000 M⊕ = 0.2–12.5 MJ, and required transiting planets to have a < 1 au and Rp = 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) = %, over the field rate of P(DG) = . 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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