重新分析半人马座和KBO的可见颜色：那里有什么，我们可能会错过什么
Reanalyzing the visible colors of Centaurs and KBOs: what is there and what we might be missing
摘要：
可见光颜色（BVRI）是半人马座和柯伊伯带天体真实光谱的合理替代，它们在这个范围内是相当线性的。颜色提供的信息有限，但仍然是研究本体表面性质的最佳工具。我们在可见颜色的研究中探索了反复出现的效应：i）由于数据误差条，相关性如何可能被遗漏或削弱，ii）由于低采样而遗漏现有趋势的“风险”，以及对在给定显著性水平下检测趋势所需的样本量进行量化预测的可能性，iii）使用偏相关来区分两个或多个参数的相互影响，以及iv）“红化线”工具对所使用的滤波器的中心波长的灵敏度。我们已经编制了约370个对象在文献中的可见颜色，并进行了分析，每个动态家庭。我们的研究结果表明：a）数据误差棒对可检测的相关性施加了限制，而不管样本大小如何，因此，一旦达到该限制，重要的是减小误差棒，但在相同或更大的误差下扩大采样是毫无意义的; b）几乎所有的动力学家族仍然需要更大的采样以确保检测到大于0.5的相关性; c）（V-R）与（R-I）之间的相关强度系统地低于（B-V）与（V-R）之间的相关强度，并且与这些颜色之间的误差条差异无关; d）使用关于颜色的轨道激发或碰撞速度参数的任何不同风格在统计学上是等效的，经典KBO的倾角相关，而倾角和Tisserand参数相对于海王星不能彼此分开;和e）经典KBO是唯一的动力学家族，既没有显示（B-V）与（V-R），也没有显示（V-R）与（R-I）相关。
英文摘要：
Visible colors (BVRI) are a reasonable proxy for real spectra of Centaurs and Kuiper Belt Objects, which are rather linear in this range. Colors provide limited information but remain the best tool to study the bulk surface properties. We explore recurrent effects in the study of visible colors: i) how a correlation could be missed or weakened as a result of the data error bars, ii) the "risk" of missing an existing trend because of low sampling, and the possibility of making quantified predictions on the sample size needed to detect a trend at a given significance level, iii) the use of partial correlations to distinguish the mutual effect of two or more parameters, and iv) the sensitivity of the "reddening line" tool to the central wavelength of the filters used. We have compiled the visible colors of about 370 objects available in the literature and carried out an analysis per dynamical family. Our results show how a) data error bars impose a limit on the detectable correlations regardless of sample size and that therefore, once that limit is achieved, it is important to diminish the error bars, but it is pointless to enlarge the sampling with the same or larger errors; b) almost all dynamical families still require larger samplings to ensure the detection of correlations stronger than 0.5; c) the correlation strength between (V-R) vs. (R-I) is systematically lower than the one between (B-V) vs. (V-R) and is not related with error-bar differences between these colors; d) it is statistically equivalent to use any of the different flavors of orbital excitation or collisional velocity parameters regarding the color-inclination correlation of classical KBOs whereas the inclination and Tisserand parameter relative to Neptune cannot be separated from one another; and e) classical KBOs are the only dynamical family that shows neither (B-V) vs. (V-R) nor (V-R) vs. (R-I) correlations.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
