用HST观测穿海王星天体的光学和红外色
Optical and Infrared Colors of Transneptunian Objects Observed with HST
摘要：
我们目前的光学颜色的72 transneptunian对象（TNOs），和红外颜色的80 TNOs获得的WFPC 2和NICMOS仪器，分别在哈勃太空望远镜（HST）。光学和红外颜色都可用于数据集之间重叠的32个对象。该数据集为整个颜色样本增加了特别均匀，一致和巨大的贡献，特别是在红外线中。我们测量的颜色范围与文献中报道的光学和红外波长的其他颜色一致。我们发现我们和其他人测量的对象一般都很好的协议; 88.1%有超过2西格玛协议。我们的光学样本的Hv星等中位数为7.2，比以前的样本略小（约0.5等）。在我们的红外样本中，中值绝对星等Hv为6.7。我们没有发现新的颜色和动力学性质（半长轴，偏心率，倾角和近日点）之间的相关性。我们确实发现，经典物体的颜色与i<6°来自不同的分布，无论是共振或激发的人口在可见光在>99.99%的水平与K-S测试。同样的结论在红外中发现，显著性水平略低，为99.72%。两个妊神星碰撞碎片与强大的近红外冰带很容易识别广泛的HST红外滤波器，并指出一个有效的搜索策略，以确定更多的这样的对象。我们在（19255）1999 VK 8、1999 OE 4、2000 CE 105、1998 KG 62和1998 WX 31中发现了变异性的证据。
英文摘要：
We present optical colors of 72 transneptunian objects (TNOs), and infrared colors of 80 TNOs obtained with the WFPC2 and NICMOS instruments, respectively, on the Hubble Space Telescope (HST). Both optical and infrared colors are available for 32 objects that overlap between the datasets. This dataset adds an especially uniform, consistent and large contribution to the overall sample of colors, particularly in the infrared. The range of our measured colors is consistent with other colors reported in the literature at both optical and infrared wavelengths. We find generally good agreement for objects measured by both us and others; 88.1% have better than 2 sigma agreement. The median Hv magnitude of our optical sample is 7.2, modestly smaller (~0.5 mag) than for previous samples. The median absolute magnitude, Hv, in our infrared sample is 6.7. We find no new correlations between color and dynamical properties (semi-major axis, eccentricity, inclination and perihelion). We do find that colors of Classical objects with i<6° come from a different distribution than either the Resonant or excited populations in the visible at the >99.99% level with a K-S test. The same conclusion is found in the infrared at a slightly lower significance level, 99.72%. Two Haumea collision fragments with strong near infrared ice bands are easily identified with broad HST infrared filters and point to an efficient search strategy for identifying more such objects. We find evidence for variability in (19255) 1999 VK8, 1999 OE4, 2000 CE105, 1998 KG62 and 1998 WX31.
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