HATS-34b and HATS-46b: Re-characterisation Using TESS and Gaia

Abstract

We present a revised characterisation of the previously discovered transiting planet systems HATS-34 and HATS-46. We make use of the newly available space-based light curves from the NASA TESS mission and high-precision parallax and absolute photometry measurements from the ESA Gaia mission to determine the mass and radius of the planets and host stars with dramatically increased precision and accuracy compared to published values, with the uncertainties in some parameters reduced by as much as a factor of seven. Using an isochrone based fit, for HATS-34 we measure a revised host star mass and radius of $0.952_{-0.02}^{+0.04}{M}_S$ and of $0.9381\pm 0.0080R_S$, respectively, and a revised mass and radius for the transiting planet of $0.951\pm 0.050M_J$ and $1.282\pm 0.064R_J$ respectively. Similarly, for HATS-46 we measure a revised mass and radius for the host star of $0.869\pm 0.023M_S$, and $0.894\pm 0.010R_S$, respectively, and a revised mass and radius for the planet of $0.158\pm 0.042M_J$, and $0.951\pm 0.029R_J$, respectively. The uncertainties that we determine on the stellar and planetary masses and radii are also substantially lower than re-determinations that incorporate the Gaia results without performing a full re-analysis of the light curves and other observational data. We argue that, in light of Gaia and TESS, a full re-analysis of previously discovered transiting planets is warranted.

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Cited by in corpus (2)

• TESS Transit Timing of Hundreds of Hot Jupiters
• LRG-BEASTS: Evidence for clouds in the transmission spectrum of HATS-46 b