Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
The early K-type T-Tauri star, V1298 Tau ( V = 10 mag, age ≈ 20–30 Myr) hosts four transiting planets with radii ranging from 4.9 to 9.6 R _⊕ . The three inner planets have orbital periods of ≈8–24 days while the outer planet’s period is poorly constrained by single transits observed with K2 and the...
| Main Authors: | , , , , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/acc865 |
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| author | James Sikora Jason Rowe Saugata Barat Jacob L. Bean Madison Brady Jean-Michel Désert Adina D. Feinstein Emily A. Gilbert Gregory Henry David Kasper Déreck-Alexandre Lizotte Michael R. B. Matesic Vatsal Panwar Andreas Seifahrt Hinna Shivkumar Gudmundur Stefánsson Julian Stürmer |
| author_facet | James Sikora Jason Rowe Saugata Barat Jacob L. Bean Madison Brady Jean-Michel Désert Adina D. Feinstein Emily A. Gilbert Gregory Henry David Kasper Déreck-Alexandre Lizotte Michael R. B. Matesic Vatsal Panwar Andreas Seifahrt Hinna Shivkumar Gudmundur Stefánsson Julian Stürmer |
| author_sort | James Sikora |
| collection | DOAJ |
| description | The early K-type T-Tauri star, V1298 Tau ( V = 10 mag, age ≈ 20–30 Myr) hosts four transiting planets with radii ranging from 4.9 to 9.6 R _⊕ . The three inner planets have orbital periods of ≈8–24 days while the outer planet’s period is poorly constrained by single transits observed with K2 and the Transiting Exoplanet Survey Satellite (TESS). Planets b, c, and d are proto–sub-Neptunes that may be undergoing significant mass loss. Depending on the stellar activity and planet masses, they are expected to evolve into super-Earths/sub-Neptunes that bound the radius valley. Here we present results of a joint transit and radial velocity (RV) modeling analysis, which includes recently obtained TESS photometry and MAROON-X RV measurements. Assuming circular orbits, we obtain a low-significance (≈2 σ ) RV detection of planet c, implying a mass of ${19.8}_{-8.9}^{+9.3}\,{M}_{\oplus }$ and a conservative 2 σ upper limit of <39 M _⊕ . For planets b and d, we derive 2 σ upper limits of M _b < 159 M _⊕ and M _d < 41 M _⊕ , respectively. For planet e, plausible discrete periods of P _e > 55.4 days are ruled out at the 3 σ level while seven solutions with 43.3 < P _e / d < 55.4 are consistent with the most probable 46.768131 ± 000076 days solution within 3 σ . Adopting the most probable solution yields a 2.6 σ RV detection with a mass of 0.66 ± 0.26 M _Jup . Comparing the updated mass and radius constraints with planetary evolution and interior structure models shows that planets b, d, and e are consistent with predictions for young gas-rich planets and that planet c is consistent with having a water-rich core with a substantial (∼5% by mass) H _2 envelope. |
| first_indexed | 2024-03-12T04:00:36Z |
| format | Article |
| id | doaj.art-5d4afbba92dd4d16b8b508e1c3f1ccf2 |
| institution | Directory Open Access Journal |
| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-03-12T04:00:36Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-5d4afbba92dd4d16b8b508e1c3f1ccf22023-09-03T11:41:24ZengIOP PublishingThe Astronomical Journal1538-38812023-01-01165625010.3847/1538-3881/acc865Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-XJames Sikora0https://orcid.org/0000-0002-3522-5846Jason Rowe1https://orcid.org/0000-0002-5904-1865Saugata Barat2Jacob L. Bean3https://orcid.org/0000-0003-4733-6532Madison Brady4https://orcid.org/0000-0003-2404-2427Jean-Michel Désert5https://orcid.org/0000-0002-0875-8401Adina D. Feinstein6https://orcid.org/0000-0002-9464-8101Emily A. Gilbert7https://orcid.org/0000-0002-0388-8004Gregory Henry8https://orcid.org/0000-0003-4155-8513David Kasper9https://orcid.org/0000-0003-0534-6388Déreck-Alexandre Lizotte10Michael R. B. Matesic11https://orcid.org/0000-0002-1119-7473Vatsal Panwar12https://orcid.org/0000-0002-2513-4465Andreas Seifahrt13https://orcid.org/0000-0003-4526-3747Hinna Shivkumar14https://orcid.org/0000-0001-9289-0570Gudmundur Stefánsson15https://orcid.org/0000-0001-7409-5688Julian Stürmer16https://orcid.org/0000-0002-4410-4712Anton Pannekoek Institute for Astronomy, University of Amsterdam , 1098 XH Amsterdam, The Netherlands ; james.t.sikora@gmail.com; Department of Physics & Astronomy, Bishop’s University , 2600 Rue College, Sherbrooke, QC J1M 1Z7, CanadaDepartment of Physics & Astronomy, Bishop’s University , 2600 Rue College, Sherbrooke, QC J1M 1Z7, CanadaAnton Pannekoek Institute for Astronomy, University of Amsterdam , 1098 XH Amsterdam, The Netherlands ; james.t.sikora@gmail.comDepartment of Astronomy & Astrophysics, University of Chicago , Chicago, IL 60637, USADepartment of Astronomy & Astrophysics, University of Chicago , Chicago, IL 60637, USAAnton Pannekoek Institute for Astronomy, University of Amsterdam , 1098 XH Amsterdam, The Netherlands ; james.t.sikora@gmail.comDepartment of Astronomy & Astrophysics, University of Chicago , Chicago, IL 60637, USAJet Propulsion Laboratory, California Institute of Technology , 4800 Oak Grove Drive, Pasadena, CA 91109, USACenter of Excellence in Information Systems, Tennessee State University , Nashville, TN 37209, USADepartment of Astronomy & Astrophysics, University of Chicago , Chicago, IL 60637, USADepartment of Physics & Astronomy, Bishop’s University , 2600 Rue College, Sherbrooke, QC J1M 1Z7, CanadaDepartment of Physics & Astronomy, Bishop’s University , 2600 Rue College, Sherbrooke, QC J1M 1Z7, Canada; Département de Physique, Université de Montréal , 2900 Bd Édouard-Montpetit, Montréal, QC H3T 1J4, Canada; Trottier Institute for Research on Exoplanets, Département de Physique, Université de Montréal , 2900 Bd Édouard-Montpetit, Montréal, QC H3T 1J4, CanadaAnton Pannekoek Institute for Astronomy, University of Amsterdam , 1098 XH Amsterdam, The Netherlands ; james.t.sikora@gmail.com; Department of Physics, University of Warwick , Coventry, West Midlands CV4 7AL, UKDepartment of Astronomy & Astrophysics, University of Chicago , Chicago, IL 60637, USAAnton Pannekoek Institute for Astronomy, University of Amsterdam , 1098 XH Amsterdam, The Netherlands ; james.t.sikora@gmail.comDepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08540, USALandessternwarte, Zentrum für Astronomie der Universität Heidelberg , Königstuhl 12, D-69117 Heidelberg, GermanyThe early K-type T-Tauri star, V1298 Tau ( V = 10 mag, age ≈ 20–30 Myr) hosts four transiting planets with radii ranging from 4.9 to 9.6 R _⊕ . The three inner planets have orbital periods of ≈8–24 days while the outer planet’s period is poorly constrained by single transits observed with K2 and the Transiting Exoplanet Survey Satellite (TESS). Planets b, c, and d are proto–sub-Neptunes that may be undergoing significant mass loss. Depending on the stellar activity and planet masses, they are expected to evolve into super-Earths/sub-Neptunes that bound the radius valley. Here we present results of a joint transit and radial velocity (RV) modeling analysis, which includes recently obtained TESS photometry and MAROON-X RV measurements. Assuming circular orbits, we obtain a low-significance (≈2 σ ) RV detection of planet c, implying a mass of ${19.8}_{-8.9}^{+9.3}\,{M}_{\oplus }$ and a conservative 2 σ upper limit of <39 M _⊕ . For planets b and d, we derive 2 σ upper limits of M _b < 159 M _⊕ and M _d < 41 M _⊕ , respectively. For planet e, plausible discrete periods of P _e > 55.4 days are ruled out at the 3 σ level while seven solutions with 43.3 < P _e / d < 55.4 are consistent with the most probable 46.768131 ± 000076 days solution within 3 σ . Adopting the most probable solution yields a 2.6 σ RV detection with a mass of 0.66 ± 0.26 M _Jup . Comparing the updated mass and radius constraints with planetary evolution and interior structure models shows that planets b, d, and e are consistent with predictions for young gas-rich planets and that planet c is consistent with having a water-rich core with a substantial (∼5% by mass) H _2 envelope.https://doi.org/10.3847/1538-3881/acc865Exoplanet astronomyExoplanetsMini NeptunesTransitsRadial velocityExoplanet systems |
| spellingShingle | James Sikora Jason Rowe Saugata Barat Jacob L. Bean Madison Brady Jean-Michel Désert Adina D. Feinstein Emily A. Gilbert Gregory Henry David Kasper Déreck-Alexandre Lizotte Michael R. B. Matesic Vatsal Panwar Andreas Seifahrt Hinna Shivkumar Gudmundur Stefánsson Julian Stürmer Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X The Astronomical Journal Exoplanet astronomy Exoplanets Mini Neptunes Transits Radial velocity Exoplanet systems |
| title | Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X |
| title_full | Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X |
| title_fullStr | Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X |
| title_full_unstemmed | Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X |
| title_short | Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X |
| title_sort | updated planetary mass constraints of the young v1298 tau system using maroon x |
| topic | Exoplanet astronomy Exoplanets Mini Neptunes Transits Radial velocity Exoplanet systems |
| url | https://doi.org/10.3847/1538-3881/acc865 |
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