Araucaria 项目：双星的高精度轨道视差与质量。I. 对十个双线光谱双星的 VLTI/GRAVITY 观测
The Araucaria project: High-precision orbital parallaxes and masses of binary stars. I. VLTI/GRAVITY observations of ten double-lined spectroscopic binaries
AI总结：
本研究结合视向速度与 VLTI/GRAVITY 干涉观测，对十个双线光谱双星系统进行高精度动力学质量和轨道视差测量，精度最高达 0.03%，并证明这些分离双星可作为校准恒星演化模型和检验 Gaia 视差的基准星。
摘要：
我们旨在测量分离双星的高精度、高准确度且不依赖模型的质量和距离。低于 1% 水平的高精度质量对于检验和校准恒星内部结构与演化模型是必要的，而高精度且独立的轨道视差对于检验未来 Gaia 数据发布也至关重要。我们将视向速度测量与干涉观测相结合，以确定十个双线光谱系统的轨道参数和物理参数。我们报告了来自 VLTI/GRAVITY 的新相对天体测量结果，并对其中一些系统报告了新的 VLT/UVES 光谱，以确定每个子星的视向速度。我们测量了十个双星系统的距离及其子星质量，精度最高可达 0.03%（平均水平为 0.2%）。这些结果与其他恒星参数（有效温度、半径、流量比等）结合，用于拟合恒星等龄线并确定其演化阶段和年龄。我们还将我们的轨道视差与 Gaia 进行了比较，结果表明，尽管这些恒星的 RUWE 低于常用的可靠 Gaia 天体测量截断值 1.4，但其中一半恒星与我们的轨道视差相比超过 1σ。通过拟合 GRAVITY 光谱中的地球大气特征，我们还估计在高和中等光谱分辨率模式下波长定标的准确度约为 0.02%。我们证明，将双星的光谱观测与干涉观测相结合，可以提供极高精度和高准确度的动力学质量与轨道视差。由于它们是分离双星，因此可以作为基准星来校准恒星演化模型并检验 Gaia 视差。
英文摘要：
We aim to measure very precise and accurate model-independent masses and distances of detached binary stars. Precise masses at the $< 1$% level are necessary to test and calibrate stellar interior and evolution models, while precise and independent orbital parallaxes are essential to check for the next Gaia data releases. We combined RV measurements with interferometric observations to determine orbital and physical parameters of ten double-lined spectroscopic systems. We report new relative astrometry from VLTI/GRAVITY and, for some systems, new VLT/UVES spectra to determine the radial velocities of each component. We measured the distance of ten binary systems and the mass of their components with a precision as high as 0.03% (average level 0.2%). They are combined with other stellar parameters (effective temperatures, radii, flux ratios, etc.) to fit stellar isochrones and determine their evolution stage and age. We also compared our orbital parallaxes with Gaia and showed that half of the stars are beyond $1σ$ with our orbital parallaxes; although, their RUWE is below the frequently used cutoff of 1.4 for reliable Gaia astrometry. By fitting the telluric features in the GRAVITY spectra, we also estimated the accuracy of the wavelength calibration to be $\sim 0.02$% in high and medium spectral resolution modes. We demonstrate that combining spectroscopic and interferometric observations of binary stars provides extremely precise and accurate dynamical masses and orbital parallaxes. As they are detached binaries, they can be used as benchmark stars to calibrate stellar evolution models and test the Gaia parallaxes.
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