木星特洛伊中小行星家族的分类：光谱数据和斯隆数字巡天颜色之间的比较
Taxonomy of asteroid families among the Jupiter Trojans: Comparison between spectroscopic data and the Sloan Digital Sky Survey colors
摘要：
我们提出了一个比较分析的光谱斜率和颜色分布的木星特洛伊，特别注意小行星家族。我们使用的数据样本从斯隆数字巡天的移动物体目录，以及从几个调查获得的光谱。第一个样本的349观测，对应于250特洛伊小行星，从斯隆数字巡天，我们还从文献中提取了第二个样本的91光谱，对应于71特洛伊。光谱斜率的计算是通过一个最小二乘拟合的一条直线的通量从斯隆观测在第一个样品中，和第二个样品中的重组光谱。在这两种情况下，在6230 $\textrmÅ$处将反射通量/光谱重新归一化为1。我们发现特洛伊小行星的光谱斜率分布呈现双峰性。大约三分之二的天体具有与D型小行星相一致的红色斜坡，而其余的天体则显示出与P型和C型分类相一致的较少的红色。小行星家族的成员也呈双峰分布，D型小行星略占优势，但背景显然以D型为主。L4和L5群表现出不同的光谱斜率分布，双峰性仅在L4中观察到。这些差异可以归因于小行星家族，因为背景小行星在两个群中显示出相同的斜率分布。对单个科的分析表明，L5中的科在分类学上是同质的，但在L4中，它们显示出分类学类型的混合。我们讨论了几个方案，可能有助于解释这些结果。
英文摘要：
We present a comparative analysis of the spectral slope and color distributions of Jupiter Trojans, with particular attention to asteroid families. We use a sample of data from the Moving Object Catalogue of the Sloan Digital Sky Survey, together with spectra obtained from several surveys. A first sample of 349 observations, corresponding to 250 Trojan asteroids, were extracted from the Sloan Digital Sky Survey, and we also extracted from the literature a second sample of 91 spectra, corresponding to 71 Trojans. The spectral slopes were computed by means of a least-squares fit to a straight line of the fluxes obtained from the Sloan observations in the first sample, and of the rebinned spectra in the second sample. In both cases the reflectance fluxes/spectra were renormalized to 1 at 6230 $\textrmÅ$. We found that the distribution of spectral slopes among Trojan asteroids shows a bimodality. About 2/3 of the objects have reddish slopes compatible with D-type asteroids, while the remaining bodies show less reddish colors compatible with the P-type and C-type classifications. The members of asteroid families also show a bimodal distribution with a very slight predominance of D-type asteroids, but the background is clearly dominated by the D-types. The L4 and L5 swarms show different distributions of spectral slopes, and bimodality is only observed in L4. These differences can be attributed to the asteroid families since the backgraound asteroids show the same slope distribtuions in both swarms. The analysis of individual families indicates that the families in L5 are taxonomically homogeneous, but in L4 they show a mixture of taxonomic types. We discuss a few scenarios that might help to interpret these results.
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