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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 730220.0, MPI für Astronomie / Publikationen_mpia
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
Authors:Hartman, J. D.; Bayliss, D.; Brahm, R.; Bakos, G. Á.; Mancini, L.; Jordán, A.; Penev, K.; Rabus, M.; Zhou, G.; Butler, R. P.; Espinoza, N.; de Val-Borro, M.; Bhatti, W.; Csubry, Z.; Ciceri, S.; Henning, T.; Schmidt, B.; Arriagada, P.; Shectman, S.; Crane, J.; Thompson, I.; Suc, V.; Csák, B.; Tan, T. G.; Noyes, R. W.; Lázár, J.; Papp, I.; Sári, P.
Date of Publication (YYYY-MM-DD):2015
Title of Journal:The Astronomical Journal
Issue / Number:5
Start Page:id. 166 (20 pp)
Audience:Not Specified
Abstract / Description: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 {{M}ȯ } and a radius of 0.57 {{R}ȯ }. HATS-6b has a period of P = 3.3253 d, mass of {{M}p} = 0.32 {{M}J}, radius of {{R}p} = 1.00 {{R}J}, and zero-albedo equilibrium temperature of {{T}eq} = 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 {{T}eq}\lt 750 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 M\lt 0.80 {{M}ȯ }, 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 {{M}ȯ } star to ∼7 and ∼2% precision, respectively. Incorporating additional information, such as the V-K color, or an absolute magnitude, allows the precision to be improved by up to a factor of two. The HATSouth network is operated by a collaboration consisting of Princeton University (PU), the Max Planck Institute für Astronomie (MPIA), the Australian National University (ANU), and the Pontificia Universidad Católica de Chile (PUC). The station at Las Campanas Observatory (LCO) of the Carnegie Institute is operated by PU in conjunction with PUC, the station at the High Energy Spectroscopic Survey (H.E.S.S.) site is operated in conjunction with MPIA, and the station at Siding Spring Observatory (SSO) is operated jointly with ANU. This paper includes data gathered with the 6.5 m Magellan Telescopes located as Las Campanas Observatory, Chile. Based in part on observations made with the MPG 2.2 m Telescope and the ESO 3.6 m Telescope at the ESO Observatory in La Silla. This paper uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope.
Free Keywords:planetary systems; stars: individual: HATS-6; techniques: photometric; techniques: spectroscopic
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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