论文标题
重新审视的第一个恒星视差
The First Stellar Parallaxes Revisited
论文作者
论文摘要
我们在1830年代重新分析了Bessel，Von Struve和Henderson使用的数据，以测量恒星的第一个视差距离。我们通常可以重现他们的结果，尽管我们发现冯·斯特鲁夫（Von Struve）和亨德森（Henderson）低估了他们的一些测量错误，从而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校正比预期的要大，这解释了他的数据中明显的系统。长期以来，冯·斯特鲁夫（Von Struve）为何首先宣布Vega的差异为0.125 ARCSEC，这一直是一个谜，直到稍后再提供更多数据以将其修改为两倍。我们通过发现冯·斯特鲁夫（Von Struve）的早期结果使用两个维度数据来解决这个谜团，从而独立地产生了明显不同的视差，但是当合并时，只有幸运地给出了正确的结果。借助以后的数据，von Struve排除了“有问题的”维度，从而导致更大的视差值。允许进行可能的温度校正，并使用他的数据从两个维度校正，将Vega的Von Struve的视差降低到与正确值一致的值。
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.
