TOI-811b and TOI-852b: New transiting brown dwarfs with similar masses and very different radii and ages from the TESS mission

Theron W. Carmichael, Samuel N. Quinn, George Zhou, Nolan Grieves, Jonathan M. Irwin, Keivan G. Stassun, Andrew M. Vanderburg, Joshua N. Winn, Francois Bouchy, Clara E. Brasseur, César Briceño, Douglas A. Caldwell, David Charbonneau, Karen A. Collins, Knicole D. Colon, Jason D. Eastman, Michael Fausnaugh, William Fong, Gábor Furész, Chelsea HuangJon M. Jenkins, John F. Kielkopf, David W. Latham, Nicholas Law, Michael B. Lund, Andrew W. Mann, George R. Ricker, Joseph E. Rodriguez, Richard P. Schwarz, Avi Shporer, Peter Tenenbaum, MacKenna L. Wood, Carl Ziegler

Research output: Contribution to journalArticlepeer-review

Abstract

We report the discovery of two transiting brown dwarfs (BDs), TOI-811b and TOI-852b, from NASA's Transiting Exoplanet Survey Satellite mission. These two transiting BDs have similar masses but very different radii and ages. Their host stars have similar masses, effective temperatures, and metallicities. The younger and larger transiting BD is TOI-811b at a mass of Mb = 59.9 ± 13.0MJ and radius of Rb = 1.26 ± 0.06RJ, and it orbits its host star in a period of P = 25.16551 ± 0.00004 days. We derive the host star's age of 93+61-29 Myr from an application of gyrochronology. The youth of this system, rather than external heating from its host star, is why this BD's radius is relatively large. This constraint on the youth of TOI-811b allows us to test substellar mass-radius evolutionary models at young ages where the radius of BDs changes rapidly. TOI-852b has a similar mass at Mb = 53.7 ± 1.4MJ but is much older (4 or 8 Gyr, based on bimodal isochrone results of the host star) and is also smaller with a radius of Rb = 0.83 ± 0.04RJ. TOI-852b's orbital period is P = 4.94561 ± 0.00008 days. TOI-852b joins the likes of other old transiting BDs that trace out the oldest substellar mass-radius evolutionary models where contraction of the BD's radius slows and approaches a constant value. Both host stars have a mass of M∗ = 1.32M⊙ ± 0.05 and differ in their radii, Teff, and [Fe/H], with TOI-811 having R∗ = 1.27 ± 0.09R⊙, Teff = 6107 ± 77 K, and [Fe/ H]=+0.40 ± 0.09 and TOI-852 having R∗ = 1.71 ± 0.04R⊙, Teff = 5768 ± 84 K, and [Fe/H]=+0.33 ± 0.09. We take this opportunity to examine how TOI-811b and TOI-852b serve as test points for young and old substellar isochrones, respectively.

Original languageEnglish (US)
Article numberabd4e1
JournalAstronomical Journal
Volume161
Issue number2
DOIs
StatePublished - Feb 1 2021

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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