We have re-analyzed the data used by Bessel, von Struve, and Henderson in the 1830s to measure the first parallax distances to stars. We can generally reproduce their results, although we find that von Struve and Henderson have underestimated some of their measurement errors, leading to optimistic parallax uncertainties. We find that temperature corrections for Bessel's measured positions are larger than anticipated, explaining some systematics apparent in his data. It has long been a mystery as to why von Struve first announced a parallax for Vega of 0.125 arcsec, only later with more data to revise it to double that value. We resolve this mystery by finding that von Struve's early result used two dimensions of position data, which independently give significantly different parallaxes, but when combined only fortuitously give the correct result. With later data, von Struve excluded the "problematic" dimension, leading to the larger parallax value. Allowing for likely temperature corrections, and using his data from both dimensions, reduces von Struve's parallax for Vega to a value consistent with the correct value.

中文翻译：

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重新审视第一个恒星视差

我们重新分析了 Bessel、von Struve 和 Henderson 在 1830 年代用来测量到恒星的第一视差距离的数据。我们通常可以重现他们的结果，尽管我们发现 von Struve 和 Henderson 低估了他们的一些测量误差，导致乐观的视差不确定性。我们发现贝塞尔测量位置的温度修正比预期的要大，这解释了他的数据中明显的一些系统性。长期以来，von Struve 为何首先宣布 Vega 的视差为 0.125 弧秒，但后来有更多数据将其修正为该值的两倍，这一直是个谜。我们通过发现 von Struve 的早期结果使用二维位置数据来解开这个谜团，它们独立地给出了显着不同的视差，但是当组合起来只是偶然地给出正确的结果时。有了后来的数据，von Struve 排除了“有问题”的维度，导致了更大的视差值。考虑到可能的温度修正，并使用他来自两个维度的数据，将 von Struve 对 Vega 的视差降低到与正确值一致的值。