The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
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 _...
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| author | 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 |
| author_facet | 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 |
| author_sort | Judah Van Zandt |
| collection | DOAJ |
| description | 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. |
| format | Article |
| id | doaj-art-effd081d4dcf4dd89bf2e23d89c44066 |
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| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-effd081d4dcf4dd89bf2e23d89c440662025-08-20T02:18:55ZengIOP PublishingThe Astronomical Journal1538-38812025-01-01169523510.3847/1538-3881/adbbedThe TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small PlanetsJudah Van Zandt0https://orcid.org/0000-0002-4290-6826Erik A. Petigura1https://orcid.org/0000-0003-0967-2893Jack Lubin2https://orcid.org/0000-0001-8342-7736Lauren M. Weiss3https://orcid.org/0000-0002-3725-3058Emma V. Turtelboom4https://orcid.org/0000-0002-1845-2617Tara Fetherolf5https://orcid.org/0000-0002-3551-279XJoseph M. Akana Murphy6https://orcid.org/0000-0001-8898-8284Ian J. M. Crossfield7Gregory J. Gilbert8https://orcid.org/0000-0003-0742-1660Teo Močnik9https://orcid.org/0000-0003-4603-556XNatalie M. Batalha10https://orcid.org/0000-0002-7030-9519Courtney Dressing11https://orcid.org/0000-0001-8189-0233Benjamin Fulton12https://orcid.org/0000-0003-3504-5316Andrew W. Howard13https://orcid.org/0000-0001-8638-0320Daniel Huber14https://orcid.org/0000-0001-8832-4488Howard Isaacson15https://orcid.org/0000-0002-0531-1073Stephen R. Kane16https://orcid.org/0000-0002-7084-0529Paul Robertson17https://orcid.org/0000-0003-0149-9678Arpita Roy18https://orcid.org/0000-0001-8127-5775Isabel Angelo19https://orcid.org/0000-0002-9751-2664Aida Behmard20https://orcid.org/0000-0003-0012-9093Corey Beard21https://orcid.org/0000-0001-7708-2364Ashley Chontos22https://orcid.org/0000-0003-1125-2564Fei Dai23https://orcid.org/0000-0002-8958-0683Steven Giacalone24https://orcid.org/0000-0002-8965-3969Michelle L. Hill25https://orcid.org/0000-0002-0139-4756Rae Holcomb26https://orcid.org/0000-0002-5034-9476Steve B. Howell27https://orcid.org/0000-0002-2532-2853Andrew W. Mayo28https://orcid.org/0000-0002-7216-2135Daria Pidhorodetska29https://orcid.org/0000-0001-9771-7953Alex S. Polanski30https://orcid.org/0000-0001-7047-8681James Rogers31https://orcid.org/0000-0001-7615-6798Lee J. Rosenthal32https://orcid.org/0000-0001-8391-5182Ryan A. Rubenzahl33https://orcid.org/0000-0003-3856-3143Nicholas Scarsdale34https://orcid.org/0000-0003-3623-7280Dakotah Tyler35https://orcid.org/0000-0003-0298-4667Samuel W. Yee36https://orcid.org/0000-0001-7961-3907Jon Zink37https://orcid.org/0000-0003-1848-2063Department of Physics & Astronomy, University of California Los Angeles , Los Angeles, CA 90095, USA ; judahvz@astro.ucla.eduDepartment of Physics & Astronomy, University of California Los Angeles , Los Angeles, CA 90095, USA ; judahvz@astro.ucla.eduDepartment of Physics & Astronomy, University of California Los Angeles , Los Angeles, CA 90095, USA ; judahvz@astro.ucla.eduDepartment of Physics and Astronomy, University of Notre Dame , Notre Dame, IN 46556, USADepartment of Astronomy, University of California Berkeley , Berkeley, CA 94720, USADepartment of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USADepartment of Astronomy and Astrophysics, University of California , Santa Cruz, CA 95064, USADepartment of Physics & Astronomy, University of Kansas , 1082 Malott, 1251 Wescoe Hall Drive, Lawrence, KS 66045, USADepartment of Physics & Astronomy, University of California Los Angeles , Los Angeles, CA 90095, USA ; judahvz@astro.ucla.eduGemini Observatory/NSF NOIRLab , 670 N. A’ohoku Place, Hilo, HI 96720, USADepartment of Astronomy and Astrophysics, University of California , Santa Cruz, CA 95060, USADepartment of Astronomy, University of California Berkeley , Berkeley, CA 94720, USANASA Exoplanet Science Institute/Caltech-IPAC , MC 314-6, 1200 E. California Boulevard, Pasadena, CA 91125, USADepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USAInstitute for Astronomy, University of Hawai‘i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA; Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney , NSW 2006, AustraliaDepartment of Astronomy, University of California Berkeley , Berkeley, CA 94720, USA; Centre for Astrophysics, University of Southern Queensland , Toowoomba, QLD 4350, AustraliaDepartment of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USADepartment of Physics & Astronomy, University of California , Irvine, Irvine, CA 92697, USASpace Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USA; Department of Physics and Astronomy, Johns Hopkins University , 3400 N Charles Street, Baltimore, MD 21218, USADepartment of Physics & Astronomy, University of California Los Angeles , Los Angeles, CA 90095, USA ; judahvz@astro.ucla.eduAmerican Museum of Natural History , 200 Central Park West, Manhattan, NY 10024, USADepartment of Physics & Astronomy, University of California , Irvine, Irvine, CA 92697, USAInstitute for Astronomy, University of Hawai‘i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA; Department of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08540, USADepartment of Astronomy and Astrophysics, University of California , Santa Cruz, CA 95064, USA; Institute for Astronomy, University of Hawai‘i , 2680 Woodlawn Drive, Honolulu, HI 96822, USADepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USADepartment of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USADepartment of Physics & Astronomy, University of California , Irvine, Irvine, CA 92697, USACenter for Computational Astrophysics, Flatiron Institute , 162 Fifth Avenue, New York, NY 10010, USADepartment of Physics & Astronomy, University of California Los Angeles , Los Angeles, CA 90095, USA ; judahvz@astro.ucla.edu; Department of Astronomy, University of California Berkeley , Berkeley, CA 94720, USADepartment of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USAUniversity of Toronto Mississauga , 3359 Mississauga Road, Mississauga, ON L5L 1C6, CanadaUniversity of Toronto Mississauga , 3359 Mississauga Road, Mississauga, ON L5L 1C6, CanadaDepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USANASA Ames Research Center , Moffett Field, CA 94035, USADepartment of Astronomy and Astrophysics, University of California , Santa Cruz, CA 95060, USADepartment of Physics & Astronomy, University of California Los Angeles , Los Angeles, CA 90095, USA ; judahvz@astro.ucla.eduDepartment of Physics and Astronomy, University of Kansas , Lawrence, KS 66045, USADepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USAWe 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.https://doi.org/10.3847/1538-3881/adbbedExoplanet astronomyExoplanet detection methodsRadial velocityBayesian statistics |
| spellingShingle | 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 The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets The Astronomical Journal Exoplanet astronomy Exoplanet detection methods Radial velocity Bayesian statistics |
| title | The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets |
| title_full | The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets |
| title_fullStr | The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets |
| title_full_unstemmed | The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets |
| title_short | The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets |
| title_sort | tess keck survey xxiv outer giants may be more prevalent in the presence of inner small planets |
| topic | Exoplanet astronomy Exoplanet detection methods Radial velocity Bayesian statistics |
| url | https://doi.org/10.3847/1538-3881/adbbed |
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