A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS
We report the discovery of a super-Jovian 2:1 mean-motion resonance (MMR) pair around the G-type star TIC 279401253, whose dynamical architecture is a prospective benchmark for planet formation and orbital evolution analysis. The system was discovered thanks to a single-transit event recorded by the...
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/acbd4f |
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| author | Vladimir Bozhilov Desislava Antonova Melissa J. Hobson Rafael Brahm Andrés Jordán Thomas Henning Jan Eberhardt Felipe I. Rojas Konstantin Batygin Pascal Torres-Miranda Keivan G. Stassun Sarah C. Millholland Denitza Stoeva Milen Minev Nestor Espinoza George R. Ricker David W. Latham Diana Dragomir Michelle Kunimoto Jon M. Jenkins Eric B. Ting Sara Seager Joshua N. Winn Jesus Noel Villasenor Luke G. Bouma Jennifer Medina Trifon Trifonov |
| author_facet | Vladimir Bozhilov Desislava Antonova Melissa J. Hobson Rafael Brahm Andrés Jordán Thomas Henning Jan Eberhardt Felipe I. Rojas Konstantin Batygin Pascal Torres-Miranda Keivan G. Stassun Sarah C. Millholland Denitza Stoeva Milen Minev Nestor Espinoza George R. Ricker David W. Latham Diana Dragomir Michelle Kunimoto Jon M. Jenkins Eric B. Ting Sara Seager Joshua N. Winn Jesus Noel Villasenor Luke G. Bouma Jennifer Medina Trifon Trifonov |
| author_sort | Vladimir Bozhilov |
| collection | DOAJ |
| description | We report the discovery of a super-Jovian 2:1 mean-motion resonance (MMR) pair around the G-type star TIC 279401253, whose dynamical architecture is a prospective benchmark for planet formation and orbital evolution analysis. The system was discovered thanks to a single-transit event recorded by the Transiting Exoplanet Survey Satellite mission, which pointed to a Jupiter-sized companion with poorly constrained orbital parameters. We began ground-based precise radial velocity (RV) monitoring with HARPS and FEROS within the Warm gIaNts with tEss survey to constrain the transiting body’s period, mass, and eccentricity. The RV measurements revealed not one but two massive planets with periods of ${76.80}_{-0.06}^{+0.06}$ and ${155.3}_{-0.7}^{+0.7}$ days, respectively. A combined analysis of transit and RV data yields an inner transiting planet with a mass of ${6.14}_{-0.42}^{+0.39}$ M _Jup and a radius of ${1.00}_{-0.04}^{+0.04}$ R _Jup , and an outer planet with a minimum mass of ${8.02}_{-0.18}^{+0.18}$ M _Jup , indicating a massive giant pair. A detailed dynamical analysis of the system reveals that the planets are locked in a strong first-order, eccentricity-type 2:1 MMR, which makes TIC 279401253 one of the rare examples of truly resonant architectures supporting disk-induced planet migration. The bright host star, V ≈ 11.9 mag, the relatively short orbital period ( P _b = ${76.80}_{-0.06}^{+0.06}$ days), and pronounced eccentricity ( e = 0.448 ${}_{-0.029}^{+0.028}$ ) make the transiting planet a valuable target for atmospheric investigation with the James Webb Space Telescope and ground-based extremely large telescopes. |
| first_indexed | 2024-03-12T04:36:28Z |
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| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-12T04:36:28Z |
| publishDate | 2023-01-01 |
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| spelling | doaj.art-d95488f4b2d341198d87867e29d3a1542023-09-03T09:55:29ZengIOP PublishingThe Astrophysical Journal Letters2041-82052023-01-019462L3610.3847/2041-8213/acbd4fA 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPSVladimir Bozhilov0https://orcid.org/0000-0002-3117-7197Desislava Antonova1https://orcid.org/0000-0003-1507-7230Melissa J. Hobson2https://orcid.org/0000-0002-5945-7975Rafael Brahm3https://orcid.org/0000-0002-9158-7315Andrés Jordán4https://orcid.org/0000-0002-5389-3944Thomas Henning5https://orcid.org/0000-0002-1493-300XJan Eberhardt6https://orcid.org/0000-0003-3130-2768Felipe I. Rojas7https://orcid.org/0000-0003-3047-6272Konstantin Batygin8https://orcid.org/0000-0002-7094-7908Pascal Torres-Miranda9https://orcid.org/0000-0003-0974-210XKeivan G. Stassun10https://orcid.org/0000-0002-3481-9052Sarah C. Millholland11https://orcid.org/0000-0003-3130-2282Denitza Stoeva12https://orcid.org/0000-0001-6277-9644Milen Minev13https://orcid.org/0000-0002-5702-5095Nestor Espinoza14https://orcid.org/0000-0001-9513-1449George R. Ricker15https://orcid.org/0000-0003-2058-6662David W. Latham16https://orcid.org/0000-0001-9911-7388Diana Dragomir17https://orcid.org/0000-0003-2313-467XMichelle Kunimoto18https://orcid.org/0000-0001-9269-8060Jon M. Jenkins19https://orcid.org/0000-0002-4715-9460Eric B. Ting20https://orcid.org/0000-0002-8219-9505Sara Seager21https://orcid.org/0000-0002-6892-6948Joshua N. Winn22https://orcid.org/0000-0002-4265-047XJesus Noel Villasenor23https://orcid.org/0000-0002-4625-8264Luke G. Bouma24https://orcid.org/0000-0002-0514-5538Jennifer Medina25https://orcid.org/0000-0002-3284-4713Trifon Trifonov26https://orcid.org/0000-0002-0236-775XDepartment of Astronomy, Faculty of Physics, Sofia University “St Kliment Ohridski,” 5 James Bourchier Blvd., BG-1164 Sofia, Bulgaria vbozhilov@phys.uni-sofia.bgDepartment of Astronomy, Faculty of Physics, Sofia University “St Kliment Ohridski,” 5 James Bourchier Blvd., BG-1164 Sofia, Bulgaria vbozhilov@phys.uni-sofia.bgMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, Germany; Millennium Institute for Astrophysics, ChileMillennium Institute for Astrophysics, Chile; Facultad de Ingeniera y Ciencias, Universidad Adolfo Ibáñez , Av. Diagonal las Torres 2640, Peñalolén, Santiago, Chile; Data Observatory Foundation , ChileMillennium Institute for Astrophysics, Chile; Facultad de Ingeniera y Ciencias, Universidad Adolfo Ibáñez , Av. Diagonal las Torres 2640, Peñalolén, Santiago, Chile; Data Observatory Foundation , ChileMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, GermanyMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, GermanyMillennium Institute for Astrophysics, Chile; Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile , ChileDivision of Geological and Planetary Sciences, California Institute of Technology , Pasadena, CA 91125, USAMillennium Institute for Astrophysics, Chile; Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile , ChileDepartment of Physics and Astronomy, Vanderbilt University , Nashville, TN 37235, USAMIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139, USADepartment of Astronomy, Faculty of Physics, Sofia University “St Kliment Ohridski,” 5 James Bourchier Blvd., BG-1164 Sofia, Bulgaria vbozhilov@phys.uni-sofia.bgDepartment of Astronomy, Faculty of Physics, Sofia University “St Kliment Ohridski,” 5 James Bourchier Blvd., BG-1164 Sofia, Bulgaria vbozhilov@phys.uni-sofia.bg; Institute of Astronomy and National Astronomical Observatory , Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Blvd., 1784 Sofia, BulgariaSpace Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USADepartment of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139, USACenter for Astrophysics , Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USADepartment of Physics and Astronomy, University of New Mexico , Albuquerque, NM, USADepartment of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139, USANASA Ames Research Center , Moffett Field, CA 94035, USANASA Ames Research Center , Moffett Field, CA 94035, USADepartment of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139, USA; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology , Cambridge, MA 02139, USA; Department of Aeronautics and Astronautics, MIT, 77 Massachusetts Avenue, Cambridge, MA 02139, USADepartment of Astrophysical Sciences, Princeton University , NJ 08544, USADepartment of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139, USACahill Center for Astrophysics, California Institute of Technology , Pasadena, CA 91125, USASpace Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USADepartment of Astronomy, Faculty of Physics, Sofia University “St Kliment Ohridski,” 5 James Bourchier Blvd., BG-1164 Sofia, Bulgaria vbozhilov@phys.uni-sofia.bg; Max-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, GermanyWe report the discovery of a super-Jovian 2:1 mean-motion resonance (MMR) pair around the G-type star TIC 279401253, whose dynamical architecture is a prospective benchmark for planet formation and orbital evolution analysis. The system was discovered thanks to a single-transit event recorded by the Transiting Exoplanet Survey Satellite mission, which pointed to a Jupiter-sized companion with poorly constrained orbital parameters. We began ground-based precise radial velocity (RV) monitoring with HARPS and FEROS within the Warm gIaNts with tEss survey to constrain the transiting body’s period, mass, and eccentricity. The RV measurements revealed not one but two massive planets with periods of ${76.80}_{-0.06}^{+0.06}$ and ${155.3}_{-0.7}^{+0.7}$ days, respectively. A combined analysis of transit and RV data yields an inner transiting planet with a mass of ${6.14}_{-0.42}^{+0.39}$ M _Jup and a radius of ${1.00}_{-0.04}^{+0.04}$ R _Jup , and an outer planet with a minimum mass of ${8.02}_{-0.18}^{+0.18}$ M _Jup , indicating a massive giant pair. A detailed dynamical analysis of the system reveals that the planets are locked in a strong first-order, eccentricity-type 2:1 MMR, which makes TIC 279401253 one of the rare examples of truly resonant architectures supporting disk-induced planet migration. The bright host star, V ≈ 11.9 mag, the relatively short orbital period ( P _b = ${76.80}_{-0.06}^{+0.06}$ days), and pronounced eccentricity ( e = 0.448 ${}_{-0.029}^{+0.028}$ ) make the transiting planet a valuable target for atmospheric investigation with the James Webb Space Telescope and ground-based extremely large telescopes.https://doi.org/10.3847/2041-8213/acbd4fRadial velocityTransit photometryExoplanetsExoplanet systemsExoplanet dynamicsExoplanet evolution |
| spellingShingle | Vladimir Bozhilov Desislava Antonova Melissa J. Hobson Rafael Brahm Andrés Jordán Thomas Henning Jan Eberhardt Felipe I. Rojas Konstantin Batygin Pascal Torres-Miranda Keivan G. Stassun Sarah C. Millholland Denitza Stoeva Milen Minev Nestor Espinoza George R. Ricker David W. Latham Diana Dragomir Michelle Kunimoto Jon M. Jenkins Eric B. Ting Sara Seager Joshua N. Winn Jesus Noel Villasenor Luke G. Bouma Jennifer Medina Trifon Trifonov A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS The Astrophysical Journal Letters Radial velocity Transit photometry Exoplanets Exoplanet systems Exoplanet dynamics Exoplanet evolution |
| title | A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS |
| title_full | A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS |
| title_fullStr | A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS |
| title_full_unstemmed | A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS |
| title_short | A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS |
| title_sort | 2 1 mean motion resonance super jovian pair revealed by tess feros and harps |
| topic | Radial velocity Transit photometry Exoplanets Exoplanet systems Exoplanet dynamics Exoplanet evolution |
| url | https://doi.org/10.3847/2041-8213/acbd4f |
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