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

Hartman, J. D. and Bayliss, D. and Brahm, R. and Bakos, G. A. and Mancini, L. and Jordan, A. and Penev, K. and Rabus, M. and Zhou, G. ORCID: https://orcid.org/0000-0002-4891-3517 and Butler, R. P. and Espinoza, N. and de Val-Borro, M. and Bhatti, W. and Csubry, Z. and Ciceri, S. and Henning, T. and Schmidt, B. and Arriagada, P. and Shectman, S. and Crane, J. and Thompson, I. and Suc, V. and Csak, B. and Tan, T. G. and Noyes, R. W. and Lazar, J. and Papp, I. and Sari, P. (2015) 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. The Astronomical Journal, 149 (5):166. pp. 1-20. ISSN 0004-6256

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Abstract

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.


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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Faculty/School / Institute/Centre: No Faculty
Faculty/School / Institute/Centre: No Faculty
Date Deposited: 31 Jan 2022 22:27
Last Modified: 31 Jan 2022 22:27
Uncontrolled Keywords: planetary systems; stars: individual: HATS-6; techniques: photometric; techniques: spectroscopic; Astrophysics - Earth; Planetary Astrophysics; Astrophysics - Solar and Stellar Astrophysics
Fields of Research (2008): 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
Fields of Research (2020): 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems
Socio-Economic Objectives (2008): E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences
Socio-Economic Objectives (2020): 28 EXPANDING KNOWLEDGE > 2801 Expanding knowledge > 280120 Expanding knowledge in the physical sciences
Identification Number or DOI: https://doi.org/10.1088/0004-6256/149/5/166
URI: http://eprints.usq.edu.au/id/eprint/44991

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