@article{ad19f79d69984a679ddeba5ab8c044fa,
title = "Revising Properties of Planet-Host Binary Systems. III. There Is No Observed Radius Gap for Kepler Planets in Binary Star Systems",
abstract = "Binary stars are ubiquitous; the majority of solar-type stars exist in binaries. Exoplanet occurrence rate is suppressed in binaries, but some multiples do still host planets. Binaries cause observational biases in planet parameters, with undetected multiplicity causing transiting planets to appear smaller than they truly are. We have analyzed the properties of a sample of 119 planet-host binary stars from the Kepler mission to study the underlying population of planets in binaries that fall in and around the radius valley, which is a demographic feature in period-radius space that marks the transition from predominantly rocky to predominantly gaseous planets. We found no statistically significant evidence for a radius gap for our sample of 122 planets in binaries when assuming that the primary stars are the planet hosts, with a low probability (p < 0.05) of the binary planet sample radius distribution being consistent with the single-star population of small planets via an Anderson-Darling test. These results reveal demographic differences in the planet size distribution between planets in binary and single stars for the first time, showing that stellar multiplicity may fundamentally alter the planet formation process. A larger sample and further assessment of circumprimary versus circumsecondary transits is needed to either validate this nondetection or explore other scenarios, such as a radius gap with a location that is dependent on binary separation.",
keywords = "LOW-MAS STARS, STELLAR PROPERTIES, FUNDAMENTAL PROPERTIES, EFFECTIVE TEMPERATURE, FORMATION HISTORY, MESA ISOCHRONES, UPPER SCORPIUS, SURVEY.111, SUPER-EARTHS",
author = "Kendall Sullivan and Kraus, {Adam L.} and Daniel Huber and Petigura, {Erik A.} and Elise Evans and Trent Dupuy and Jingwen Zhang and Berger, {Travis A.} and Eric Gaidos and Mann, {Andrew W.}",
note = "Funding Information: Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Funding Information: The authors thank the referee for their thoughtful comments, which improved this paper. K.S. acknowledges that this material is based on work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1610403. D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC19K0597). E.P. acknowledges support from the Alfred P. Sloan Foundation. T.A.B.'s research was supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities under contract with NASA. The authors sincerely thank the observing staff and resident astronomers at the Hobby–Eberly Telescope for obtaining the observations presented in this work. The authors acknowledge the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing high-performance computing resources that have contributed to the research results reported within this paper. Funding Information: This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the SVO Filter Profile Service ( http://svo2.cab.inta-csic.es/theory/fps/ ) supported by the Spanish MINECO through grant AYA2017-84089. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France (DOI: 10.26093/cds/vizier). The original description of the VizieR service was published in 2000, A&AS, 143, 23. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. 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. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding Information: The authors thank the referee for their thoughtful comments, which improved this paper. K.S. acknowledges that this material is based on work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1610403. D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC19K0597). E.P. acknowledges support from the Alfred P. Sloan Foundation. T.A.B.'s research was supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities under contract with NASA. The authors sincerely thank the observing staff and resident astronomers at the Hobby-Eberly Telescope for obtaining the observations presented in this work. The authors acknowledge the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing high-performance computing resources that have contributed to the research results reported within this paper. Funding Information: The Hobby–Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universit{\"a}t M{\"u}nchen, and Georg-August-Universit{\"a}t G{\"o}ttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Low-Resolution Spectrograph 2 (LRS2) was developed and funded by the University of Texas at Austin McDonald Observatory and Department of Astronomy and by Pennsylvania State University. We thank the Leibniz-Institut f{\"u}r Astrophysik Potsdam (AIP) and the Institut f{\"u}r Astrophysik G{\"o}ttingen (IAG) for their contributions to the construction of the integral field units. Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",
year = "2023",
month = mar,
day = "27",
doi = "10.3847/1538-3881/acbdf9",
language = "English",
volume = "165",
pages = "1--13",
journal = "Astronomical Journal",
issn = "0004-6256",
publisher = "IOP Publishing",
number = "4",
}