TOI-2119: a transiting brown dwarf orbiting an active M-dwarf from NASA's TESS mission. Issue 4 (16th June 2022)

• Record Type: Journal Article
• Authors: Carmichael, Theron W; Irwin, Jonathan M; Murgas, Felipe; Pallé, Enric; Stassun, Keivan G; Bartnik, Matthew; Collins, Karen A; de Leon, Jerome; Esparza-Borges, Emma; Fedewa, Jeremy; Fong, William; Fukui, Akihiko; Jenkins, Jon M; Kagetani, Taiki; Latham, David W; Lund, Michael B; Mann, Andrew W; Moldovan, Dan; Morgan, Edward H; Narita, Norio; Painter, Shane; Parviainen, Hannu; Quintana, Elisa V; Ricker, George R; Schulte, Jack; Schwarz, Richard P; Seager, Sara; Sokolovsky, Kirill; Twicken, Joseph D; Winn, Joshua N
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 514:Issue 4(2022)
• Page Start: 4944
• Page End: 4957
• Publication Date: 2022-06-16
• Subjects: techniques: photometric -- techniques: radial velocities -- techniques: spectroscopic -- (stars:) brown dwarfs -- stars: low-mass; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac1666
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We report the discovery of TOI-2119b, a transiting brown dwarf (BD) that orbits and is completely eclipsed by an active M -dwarf star. Using light-curve data from the Transiting Exoplanet Survey Satellite mission and follow-up high-resolution Doppler spectroscopic observations, we find the BD has a radius of Rb = 1.08 ± 0.03 R J, a mass of Mb = 64.4 ± 2.3 M J, an orbital period of P = 7.200865 ± 0.00002 d, and an eccentricity of e = 0.337 ± 0.002. The host star has a mass of M ⋆ = 0.53 ± 0.02M⊙, a radius of R ⋆ = 0.50 ± 0.01R⊙, an effective temperature of T eff = 3621 ± 48K, and a metallicity of $\rm [Fe/H]=+0.06\pm 0.08$ . TOI-2119b joins an emerging population of transiting BDs around M-dwarf host stars, with TOI-2119 being the ninth such system. These M-dwarf–brown dwarf systems typically occupy mass ratios near q = Mb / M ⋆ ≈ 0.1−0.2, which separates them from the typical mass ratios for systems with transiting substellar objects and giant exoplanets that orbit more massive stars. The nature of the secondary eclipse of the BD by the star enables us to estimate the effective temperature of the substellar object to be 2030 ± 84K, which is consistent with predictions by substellar evolutionary models.