We present a revised characterization 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 7. Using an isochrone-based fit, for HATS-34 we measure a revised host star mass and radius of |$0.952_{-0.020}^{+0.040}$| |$\, \mathrm{M}_\odot$| and 0.9381 ± 0.0080 |$\, \mathrm{R}_\odot$|⁠, respectively, and a revised mass and radius for the transiting planet of 0.951 ± 0.050 M_J and 1.282 ± 0.064 R_J, respectively. Similarly, for HATS-46 we measure a revised mass and radius for the host star of 0.869 ± 0.023 |$\, \mathrm{M}_\odot$| and 0.894 ± 0.010 |$\, \mathrm{R}_\odot$|⁠, respectively, and a revised mass and radius for the planet of 0.158 ± 0.042 M_J and 0.951 ± 0.029 R_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.

中文翻译：

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HATS-34b和HATS-46b：使用TESS和Gaia进行重新表征

我们介绍了先前发现的过境行星系统HATS-34和HATS-46的修订版特性。我们利用NASA TESS任务中新近可用的天基光曲线以及ESA Gaia任务中的高精度视差和绝对光度法测量来确定行星和主恒星的质量和半径，与之相比，精确度和准确性大大提高了。到公布的数值，某些参数的不确定性减少了多达7倍。使用基于等时线的拟合，对于HATS-34，我们测量的修正主星质量和半径为| $ 0.952 _ {-0.020} ^ { +0.040} $ |  | $ \，\ mathrm {M} _ \ odot $ | 和0.9381±0.0080  | $ \，\ mathrm {R} _ \ odot $ |⁠分别和修订的质量和半径0.951±0.050的过境行星 中号_Ĵ和1.282±0.064  [R _Ĵ分别。同样，对于HATS-46，我们测量的主星修正质量和半径为0.869±0.023  | $ \，\ mathrm {M} _ \ odot $ | 和0.894±0.010  | $ \，\ mathrm {R} _ \ ODOT $ |⁠，分别和修订的质量和半径0.158±0.042的行星 中号_Ĵ和0.951±0.029  [R _Ĵ分别。我们在恒星，行星质量和半径上确定的不确定性也大大低于包含盖亚（Gaia）的重新确定无需完全重新分析光曲线和其他观测数据即可获得结果。我们认为，根据盖亚（Gaia）和泰斯（TESS），有必要对先前发现的过境行星进行全面的重新分析。