HATS-6b: A warm saturn transiting an early m dwarf star, and a set of empirical relations for characterizing k and m dwarf planet hosts

J. D. Hartman, D. Bayliss, R. Brahm, G. Bakos, L. Mancini, A. Jordàn, K. Penev, M. Rabus, G. Zhou, R. P. Butler, N. Espinoza, M. De Val-Borro, W. Bhatti, Z. Csubry, S. Ciceri, T. Henning, B. Schmidt, P. Arriagada, S. Shectman, J. CraneI. Thompson, V. Suc, B. Csàk, T. G. Tan, R. W. Noyes, J. Làzàr, I. Papp, P. Sàri

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We report the discovery by the HATSouth survey of HATS-6b, an extrasolar planet transiting a V = 15.2 mag, i = 13.7 mag M1V star with a mass of 0.57 and a radius of 0.57 . HATS-6b has a period of P = 3.3253 d, mass of = 0.32 , radius of = 1.00 , and zero-albedo equilibrium temperature of = 712.8 ±5.1 K. HATS-6 is one of the lowest mass stars known to host a close-in gas giant planet, and its transits are among the deepest of any known transiting planet system. We discuss the follow-up opportunities afforded by this system, noting that despite the faintness of the host star, it is expected to have the highest K-band S/N transmission spectrum among known gas giant planets with K. In order to characterize the star we present a new set of empirical relations between the density, radius, mass, bolometric magnitude, and V-, J-, H- and K-band bolometric corrections for main sequence stars with , or spectral types later than K5. These relations are calibrated using eclipsing binary components as well as members of resolved binary systems. We account for intrinsic scatter in the relations in a self-consistent manner. We show that from the transit-based stellar density alone it is possible to measure the mass and radius of a ∼0.6 star to ∼7 and ∼2% precision, respectively. Incorporating additional information, such as the color, or an absolute magnitude, allows the precision to be improved by up to a factor of two.

Original languageEnglish
Article number166
JournalAstronomical Journal
Issue number5
StatePublished - 1 May 2015
Externally publishedYes


  • machine-readable and VO tables
  • planetary systems
  • stars: individual (HATS-6)
  • techniques: photometric
  • techniques: spectroscopic Supporting material


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