HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star

Vowell, Noah; Rodriguez, Joseph E.; Quinn, Samuel N.; Zhou, George; Vanderburg, Andrew; Mann, Andrew W.; Hooton, Matthew J.; Stassun, Keivan G.; Howard, Saburo; Bieryla, Allyson; Latham, David W.; Howell, Steve B.; Guillot, T.; Ziegler, Carl; Collins, Karen A.; Carmichael, Theron W.; Jenkins, Jon M.; Shporer, Avi; ABE, Lyu; Bendjoya, Philippe; Bush, Jonathan L.; Buttu, Marco; Collins, Kevin I.; Eastman, Jason D.; Fields, Matthew J.; Gasparetto, Thomas; Günther, Maximilian N.; Kostov, Veselin B.; Kraus, Adam L.; Lester, Kathryn V.; Levine, Alan M.; Marie-Sainte, Wenceslas; Mékarnia, D.; Osborn, H.; Rapetti, David; Ricker, G.; Winn, Joshua N.; Sefako, Ramotholo; Srdoč, Gregor; Suárez, Olga; Torres, Guillermo; Triaud, A. H. M. J.; Vanderspek, R.; Winn, Joshua N.

doi:10.3847/1538-3881/acd197

Cited by 6 publications

(3 citation statements)

References 136 publications

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“…Specifically, we used the unpopular package 33 to build a model of systematics (Hattori et al 2021). The details of the unpopular extraction used here are reported in Barber et al (2022), Vowell et al (2023), andWood et al (2023), each of which were applied to measuring rotation periods in young associations.…”

Section: Tess Photometrymentioning

confidence: 99%

TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association

Thao,

Mann,

Barber

et al. 2024

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Young (<500 Myr) planets are critical to studying how planets form and evolve. Among these young planetary systems, multiplanet configurations are particularly useful, as they provide a means to control for variables within a system. Here, we report the discovery and characterization of a young planetary system, TOI-1224. We show that the planet host resides within a young population we denote as MELANGE-5. By employing a range of age-dating methods—isochrone fitting, lithium abundance analysis, gyrochronology, and Gaia excess variability—we estimate the age of MELANGE-5 to be 210 ± 27 Myr. MELANGE-5 is situated in close proximity to previously identified younger (80–110 Myr) associations, Crius 221 and Theia 424/Volans-Carina, motivating further work to map out the group boundaries. In addition to a planet candidate detected by the TESS pipeline and alerted as a TESS object of interest, TOI-1224 b, we identify a second planet, TOI-1224 c, using custom search tools optimized for young stars (Notch and LOCoR). We find that the planets are 2.10 ± 0.09 R ⊕ and 2.88 ± 0.10 R ⊕ and orbit their host star every 4.18 and 17.95 days, respectively. With their bright (K = 9.1 mag), small (R * = 0.44 R ⊙), and cool (T eff = 3326 K) host star, these planets represent excellent candidates for atmospheric characterization with JWST.

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Section: Tess Photometrymentioning

confidence: 99%

TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association

Thao,

Mann,

Barber

et al. 2024

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“…In addition to planets, TESS is able to detect transiting brown dwarf companions. Out of the 39 confirmed transiting brown dwarf companions currently known, TESS has discovered almost half (Grieves et al 2021;Cañas et al 2022;Carmichael et al 2022;Lin et al 2023;Psaridi et al 2022;Sebastian et al 2022;Vowell et al 2023). The use of TESS to detect transiting brown dwarf companions enables the determination of precise radii, and may therefore illuminate the brown dwarf desert and associated formation mechanisms.…”

Section: Introductionmentioning

confidence: 99%

TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star

Page,

Pepper,

Wright

et al. 2024

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We present the discovery of TOI-1994b, a low-mass brown dwarf transiting a hot subgiant star on a moderately eccentric orbit. TOI-1994 has an effective temperature of 7700 − 410 + 720 K, V magnitude of 10.51 mag and log(g) of 3.982 − 0.065 + 0.067 . The brown dwarf has a mass of 22.1 − 2.5 + 2.6 M J, a period of 4.034 days, an eccentricity of 0.341 − 0.059 + 0.054 , and a radius of 1.220 − 0.071 + 0.082 R J. TOI-1994b is more eccentric than other transiting brown dwarfs with similar masses and periods. The population of low-mass brown dwarfs may have properties similar to planetary systems if they were formed in the same way, but the short orbital period and high eccentricity of TOI-1994b may contrast this theory. An evolved host provides a valuable opportunity to understand the influence stellar evolution has on the substellar companion’s fundamental properties. With precise age, mass, and radius, the global analysis and characterization of TOI-1994b augments the small number of transiting brown dwarfs and allows the testing of substellar evolution models.

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“…TESS light curves have been exhaustively searched for candidate transiting planets (Guerrero et al 2021). Now in its Second Extended Mission, TESS data has led to the discovery of thousands of eclipsing binaries (Prša et al 2022) and over a dozen transiting very-low-mass stars and brown dwarfs (e.g., Grieves et al 2021;Carmichael et al 2022;Psaridi et al 2022;Lin et al 2023;Vowell et al 2023). The population of TESS-discovered eclipsing or transiting systems is biased toward periods shorter than about 10 days due to TESS's observing strategy and the smaller transit probabilities of systems with longer periods.…”

Section: Introductionmentioning

confidence: 99%

Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries

Schmidt,

Schlaufman,

Ding 丁

et al. 2023

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While secondary mass inferences based on single-lined spectroscopic binary (SB1) solutions are subject to sin i degeneracies, this degeneracy can be lifted through the observations of eclipses. We combine the subset of Gaia Data Release 3 SB1 solutions consistent with brown dwarf-mass secondaries with the Transiting Exoplanet Survey Satellite (TESS) Object of Interest (TOI) list to identify three candidate transiting brown dwarf systems. Ground-based precision radial velocity follow-up observations confirm that TOI-2533.01 is a transiting brown dwarf with M = 72 − 3 + 3 M Jup = 0.069 − 0.003 + 0.003 M ⊙ orbiting TYC 2010-124-1 and that TOI-5427.01 is a transiting very low-mass star with M = 93 − 2 + 2 M Jup = 0.088 − 0.002 + 0.002 M ⊙ orbiting UCAC4 515-012898. We validate TOI-1712.01 as a very low-mass star with M = 82 − 7 + 7 M Jup = 0.079 − 0.007 + 0.007 M ⊙ transiting the primary in the hierarchical triple system BD+45 1593. Even after accounting for third light, TOI-1712.01 has a radius nearly a factor of 2 larger than predicted for isolated stars with similar properties. We propose that the intense instellation experienced by TOI-1712.01 diminishes the temperature gradient near its surface, suppresses convection, and leads to its inflated radius. Our analyses verify Gaia DR3 SB1 solutions in the low Doppler semiamplitude limit, thereby providing the foundation for future joint analyses of Gaia radial velocities and Kepler, K2, TESS, and PLAnetary Transits and Oscillations light curves for the characterization of transiting massive brown dwarfs and very low-mass stars.

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HIP 33609 b: An Eccentric Brown Dwarf Transiting a V = 7.3 Rapidly Rotating B Star

Abstract: We present the discovery and characterization of HIP 33609 b, a transiting warm brown dwarf orbiting a late B star, discovered by NASA's Transiting Exoplanet Survey Satellite as TOI-588 b. HIP 33609 b is a large (R b = 1.580 − 0.070 … Show more

Cited by 6 publications

References 136 publications

TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association

TESS Hunt for Young and Maturing Exoplanets (THYME). X. A Two-planet System in the 210 Myr MELANGE-5 Association

TOI-1994b: A Low-mass Eccentric Brown Dwarf Transiting A Subgiant Star

Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries

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