Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
M dwarfs have become increasingly important in the detection of exoplanets and the study of Earth-sized planets and their habitability. However, 20%–30% of M dwarfs have companions that can impact the formation and evolution of planetary systems. We use high-resolution imaging and Gaia astrometry to...
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| Language: | English |
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IOP Publishing
2025-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/ad9923 |
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| author | Rachel A. Matson Rebecca Gore Steve B. Howell David R. Ciardi Jessie L. Christiansen Catherine A. Clark Ian J. M. Crossfield Sergio B. Fajardo-Acosta Rachel B. Fernandes Elise Furlan Emily A. Gilbert Erica Gonzales Kathryn V. Lester Michael B. Lund Elisabeth C. Matthews Alex S. Polanski Joshua E. Schlieder Carl Ziegler |
| author_facet | Rachel A. Matson Rebecca Gore Steve B. Howell David R. Ciardi Jessie L. Christiansen Catherine A. Clark Ian J. M. Crossfield Sergio B. Fajardo-Acosta Rachel B. Fernandes Elise Furlan Emily A. Gilbert Erica Gonzales Kathryn V. Lester Michael B. Lund Elisabeth C. Matthews Alex S. Polanski Joshua E. Schlieder Carl Ziegler |
| author_sort | Rachel A. Matson |
| collection | DOAJ |
| description | M dwarfs have become increasingly important in the detection of exoplanets and the study of Earth-sized planets and their habitability. However, 20%–30% of M dwarfs have companions that can impact the formation and evolution of planetary systems. We use high-resolution imaging and Gaia astrometry to detect stellar companions around M dwarf exoplanet hosts discovered by TESS and determine the projected separation and estimated stellar masses for each system. We find 47 companions around 216 M dwarfs and a multiplicity rate of 19.4% ± 2.7% that is consistent with field M dwarfs. The binary projected separation distribution is shifted to larger separations, confirming the lack of close binaries hosting transiting exoplanets seen in previous studies. We correct the radii of planets with nearby companions and examine the properties of planets in M dwarf multistar systems. We also note three multiplanet systems that occur in close binaries (≲50 au) where planet formation is expected to be suppressed. |
| format | Article |
| id | doaj-art-574dd608d7574c91879e5b1dba627e46 |
| institution | Kabale University |
| issn | 1538-3881 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj-art-574dd608d7574c91879e5b1dba627e462025-01-17T06:53:30ZengIOP PublishingThe Astronomical Journal1538-38812025-01-0116927610.3847/1538-3881/ad9923Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESSRachel A. Matson0https://orcid.org/0000-0001-7233-7508Rebecca Gore1https://orcid.org/0009-0000-7274-7523Steve B. Howell2https://orcid.org/0000-0002-2532-2853David R. Ciardi3https://orcid.org/0000-0002-5741-3047Jessie L. Christiansen4https://orcid.org/0000-0002-8035-4778Catherine A. Clark5https://orcid.org/0000-0002-2361-5812Ian J. M. Crossfield6Sergio B. Fajardo-Acosta7https://orcid.org/0000-0001-9309-0102Rachel B. Fernandes8https://orcid.org/0000-0002-3853-7327Elise Furlan9https://orcid.org/0000-0001-9800-6248Emily A. Gilbert10https://orcid.org/0000-0002-0388-8004Erica Gonzales11Kathryn V. Lester12https://orcid.org/0000-0002-9903-9911Michael B. Lund13https://orcid.org/0000-0003-2527-1598Elisabeth C. Matthews14https://orcid.org/0000-0003-0593-1560Alex S. Polanski15https://orcid.org/0000-0001-7047-8681Joshua E. Schlieder16https://orcid.org/0000-0001-5347-7062Carl Ziegler17https://orcid.org/0000-0002-0619-7639U.S. Naval Observatory , 3450 Massachusetts Avenue NW, Washington, D.C. 20392, USABay Area Environmental Research Institute , Moffett Field, CA 94035, USANASA Ames Research Center , Moffett Field, CA 94035, USANASA Exoplanet Science Institute, California Institute of Technology , IPAC, 1200 E. California Boulevard, Pasadena, CA 91125, USANASA Exoplanet Science Institute, California Institute of Technology , IPAC, 1200 E. California Boulevard, Pasadena, CA 91125, USANASA Exoplanet Science Institute, California Institute of Technology , IPAC, 1200 E. California Boulevard, Pasadena, CA 91125, USADepartment of Physics and Astronomy, University of Kansas , Lawrence, KS 66045, USANASA Exoplanet Science Institute, California Institute of Technology , IPAC, 1200 E. California Boulevard, Pasadena, CA 91125, USADepartment of Astronomy & Astrophysics, 525 Davey Laboratory, The Pennsylvania State University , University Park, PA 16802, USA; Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, The Pennsylvania State University , University Park, PA 16802, USANASA Exoplanet Science Institute, California Institute of Technology , IPAC, 1200 E. California Boulevard, Pasadena, CA 91125, USAJet Propulsion Laboratory, California Institute of Technology , 4800 Oak Grove Drive, Pasadena, CA 91109, USADepartment of Astronomy and Astrophysics, University of California , Santa Cruz, CA 95064, USAMount Holyoke College , South Hadley, MA 01075, USANASA Exoplanet Science Institute, California Institute of Technology , IPAC, 1200 E. California Boulevard, Pasadena, CA 91125, USAMax-Planck-Institut für Astronomie , Königstuhl 17, 69117 Heidelberg, GermanyDepartment of Physics and Astronomy, University of Kansas , Lawrence, KS 66045, USANASA Goddard Space Flight Center , Greenbelt, MD 20771, USADepartment of Physics, Engineering and Astronomy, Stephen F. Austin State University , 1936 North Street, Nacogdoches, TX 75962, USAM dwarfs have become increasingly important in the detection of exoplanets and the study of Earth-sized planets and their habitability. However, 20%–30% of M dwarfs have companions that can impact the formation and evolution of planetary systems. We use high-resolution imaging and Gaia astrometry to detect stellar companions around M dwarf exoplanet hosts discovered by TESS and determine the projected separation and estimated stellar masses for each system. We find 47 companions around 216 M dwarfs and a multiplicity rate of 19.4% ± 2.7% that is consistent with field M dwarfs. The binary projected separation distribution is shifted to larger separations, confirming the lack of close binaries hosting transiting exoplanets seen in previous studies. We correct the radii of planets with nearby companions and examine the properties of planets in M dwarf multistar systems. We also note three multiplanet systems that occur in close binaries (≲50 au) where planet formation is expected to be suppressed.https://doi.org/10.3847/1538-3881/ad9923Binary starsExoplanet systemsLow mass starsM dwarf stars |
| spellingShingle | Rachel A. Matson Rebecca Gore Steve B. Howell David R. Ciardi Jessie L. Christiansen Catherine A. Clark Ian J. M. Crossfield Sergio B. Fajardo-Acosta Rachel B. Fernandes Elise Furlan Emily A. Gilbert Erica Gonzales Kathryn V. Lester Michael B. Lund Elisabeth C. Matthews Alex S. Polanski Joshua E. Schlieder Carl Ziegler Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS The Astronomical Journal Binary stars Exoplanet systems Low mass stars M dwarf stars |
| title | Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS |
| title_full | Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS |
| title_fullStr | Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS |
| title_full_unstemmed | Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS |
| title_short | Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS |
| title_sort | demographics of m dwarf binary exoplanet hosts discovered by tess |
| topic | Binary stars Exoplanet systems Low mass stars M dwarf stars |
| url | https://doi.org/10.3847/1538-3881/ad9923 |
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