Updated planetary mass constraints of the young V1298 tau system using MAROON-X

• Verfasst von: Sikora, James [VerfasserIn]
• Verfasst von: Rowe, Jason [VerfasserIn]
• Verfasst von: Barat, Saugata [VerfasserIn]
• Verfasst von: Bean, Jacob L. [VerfasserIn]
• Verfasst von: Brady, Madison [VerfasserIn]
• Verfasst von: Désert, Jean-Michel [VerfasserIn]
• Verfasst von: Feinstein, Adina D. [VerfasserIn]
• Verfasst von: Gilbert, Emily A. [VerfasserIn]
• Verfasst von: Henry, Gregory [VerfasserIn]
• Verfasst von: Kasper, David [VerfasserIn]
• Verfasst von: Lizotte, Déreck-Alexandre [VerfasserIn]
• Verfasst von: Matesic, Michael R. B. [VerfasserIn]
• Verfasst von: Panwar, Vatsal [VerfasserIn]
• Verfasst von: Seifahrt, Andreas [VerfasserIn]
• Verfasst von: Shivkumar, Hinna [VerfasserIn]
• Verfasst von: Stefánsson, Gudmundur [VerfasserIn]
• Verfasst von: Stürmer, Julian [VerfasserIn]
• Titel: Updated planetary mass constraints of the young V1298 tau system using MAROON-X
• Verf.angabe: 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, and Julian Stürmer
• Jahr: 2023
• Umfang: 15 S.
• Illustrationen: Illustrationen
• Fussnoten: Veröffentlicht: 24. Mai 2023 ; Gesehen am 26.07.2023
• Titel Quelle: Enthalten in: The astronomical journal
• Ort Quelle: Washington, DC : AAS Publishing, American Astronomical Society, 1998
• Jahr Quelle: 2023
• Band/Heft Quelle: 165(2023), 6, Artikel-ID 250, Seite 1-15
• ISSN Quelle: 1538-3881
• DOI: doi:10.3847/1538-3881/acc865
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1853672904

Abstract

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 (≈2σ) RV detection of planet c, implying a mass of and a conservative 2σ upper limit of <39 M ⊕. For planets b and d, we derive 2σ 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 3σ level while seven solutions with 43.3 < P e/d < 55.4 are consistent with the most probable 46.768131 ± 000076 days solution within 3σ. Adopting the most probable solution yields a 2.6σ 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) H2 envelope.