Previous analyses of various standard candles observed by the Gaia satellite have reported statistically significant systematics in the parallaxes that have improved from ∼250 μas in the first data release (DR1) to 50–80 μas in the second data release (DR2). Here we examine the parallaxes newly reported in the Gaia early third data release (EDR3) using the same sample of benchmark eclipsing binaries (EBs) we used to assess the DR1 and DR2 parallaxes. We find a mean offset of −37 20 μas (Gaia − EB), which decreases to −15 18 μas after applying the corrections recommended by the Gaia Mission team; global systematics in the Gaia parallaxes have clearly improved and are no longer statistically significant for the EB sample, which spans 5 ≲ G ≲ 12 in brightness and 0.03–3 kpc in distance. We also find that the Renormalized Unit Weight Error (RUWE) goodness-of-fit statistic reported in Gaia DR3 is highly sensitive to unresolved companions (tertiaries in the case of our EB sample) as well as to photocenter motion of the binaries themselves. RUWE is nearly perfectly correlated (r ² = 0.82) with photocenter motions down to ≲0.1 mas, and surprisingly this correlation exists entirely within the nominal “good” RUWE range of 1.0–1.4. This suggests that RUWE values even slightly greater than 1.0 may signify unresolved binaries in Gaia, and that the RUWE value can serve as a quantitative predictor of the photocenter motion.

先前对盖亚卫星观测到的各种标准烛光的分析报告了视差的统计显着系统性，视差从第一个数据发布 (DR1) 中的 ~ 250 μ改善到第二个数据发布 (DR2) 中的50-80 μ。在这里，我们使用我们用来评估 DR1 和 DR2 视差的基准日食双星 (EB) 的相同样本来检查 Gaia 早期第三次数据发布 (EDR3) 中新报告的视差。我们发现 -37 20 μ作为 (Gaia - EB)的平均偏移量，它降低到 -15 18 μ在应用盖亚任务团队推荐的更正后；Gaia 视差中的全局系统性明显改善，对于 EB 样本不再具有统计意义，EB 样本的亮度跨度为 5 ≲ G ≲ 12，距离为 0.03-3 kpc。我们还发现，Gaia DR3 中报告的重新归一化单位权重误差 (RUWE) 拟合优度统计对未解析的伴星（在我们的 EB 样本中为三级）以及双星本身的光心运动高度敏感。RUWE 几乎完全相关 ( r ²= 0.82），光心运动低至≲0.1 mas，令人惊讶的是，这种相关性完全存在于标称“好” RUWE 范围 1.0–1.4 内。这表明 RUWE 值甚至略大于 1.0 可能意味着盖亚中未解析的双星，并且 RUWE 值可以作为光心运动的定量预测器。