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Shape size and multiplicity of main-belt asteroids I. Keck Adaptive Optics survey

机译：主带小行星的形状大小和多样性I.凯克自适应光学测量

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This paper presents results from a high spatial resolution survey of 33 main-belt asteroids with diameters >40 km using the Keck II Adaptive Optics (AO) facility. Five of these (45 Eugenia, 87 Sylvia, 107 Camilla, 121 Hermione, 130 Elektra) were confirmed to have satellite. Assuming the same albedo as the primary, these moonlets are relatively small (∼5% of the primary size) suggesting that they are fragments captured after a disruptive collision of a parent body or captured ejecta due to an impact. For each asteroid, we have estimated the minimum size of a moonlet that can positively detected within the Hill sphere of the system by estimating and modeling a 2-σ detection profile: in average on the data set, a moonlet located at 2/100 × RHill (1/4 × RHill) with a diameter larger than 6 km (4 km) would have been unambiguously seen. The apparent size and shape of each asteroid was estimated after deconvolution using a new algorithm called AIDA. The mean diameter for the majority of asteroids is in good agreement with IRAS radiometric measurements, though for asteroids with a D < 200 km, it is underestimated on average by 6–8%. Most asteroids had a size ratio that was very close to those determined by lightcurve measurements. One observation of 104 Klymene suggests it has a bifurcated shape. The bi-lobed shape of 121 Hermione described in Marchis et al. [Marchis, F., Hestroffer, D., Descamps, P., Berthier, J., Laver, C., de Pater, I., 2005c. Icarus 178, 450–464] was confirmed after deconvolution. The ratio of contact binaries in our survey, which is limited to asteroids larger than 40 km, is surprisingly high (∼6%), suggesting that a non-single configuration is common in the main-belt. Several asteroids have been analyzed with lightcurve inversions. We compared lightcurve inversion models for plane-of-sky predictions with the observed images (9 Metis, 52 Europa, 87 Sylvia, 130 Elektra, 192 Nausikaa, and 423 Diotima, 511 Davida). The AO images allowed us to determine a unique photometric mirror pole solution, which is normally ambiguous for asteroids moving close to the plane of the ecliptic (e.g., 192 Nausikaa and 52 Europa). The photometric inversion models agree well with the AO images, thus confirming the validity of both the lightcurve inversion method and the AO image reduction technique.
机译：本文介绍了使用Keck II自适应光学（AO）设施对33个直径大于40 km的主带小行星进行的高空间分辨率调查的结果。这些中的五个（45个Eugenia，87个Sylvia，107个Camilla，121个Hermione，130个Elektra）被确认拥有卫星。假设与原初的反射率相同，则这些小卫星相对较小（约为原初大小的5％），表明它们是在母体破裂碰撞或由于撞击而捕获的弹射物之后捕获的碎片。对于每个小行星，我们通过估计和建模2-σ检测剖面来估计可以在系统的Hill球内可靠检测到的卫星的最小尺寸：在数据集上，平均而言，卫星位于2/100×可以清楚地看到直径大于6 km（4 km）的RHill（1/4×RHill）。反卷积后，使用一种称为AIDA的新算法来估算每个小行星的表观大小和形状。大多数小行星的平均直径与IRAS辐射测量结果非常吻合，尽管对于D <200 km的小行星，平均直径被低估了6–8％。大多数小行星的尺寸比与通过光曲线测量确定的尺寸比非常接近。对104个Klymene的一项观察表明，它具有分叉的形状。 Marchis等人描述的121 Hermione的双瓣形状。 [Marchis，F.，Hestroffer，D.，Descamps，P.，Berthier，J.，Laver，C.，de Pater，I.，2005c。反卷积后确认为“伊卡洛斯178，450–464”。在我们的调查中，仅限于大于40 km的小行星的接触二元比率非常高（〜6％），这表明在主带中非单一配置是常见的。已经对几个小行星进行了光曲线反演分析。我们将用于天空平面预测的光曲线反演模型与观测到的图像进行了比较（9梅蒂斯，52欧罗巴，87西尔维亚，130 Elektra，192瑙西卡和423 Diotima，511大卫达）。 AO图像使我们能够确定唯一的光度镜极解，这通常对于小行星接近黄道平面（例如192 Nausikaa和52 Europa）的小行星来说是模棱两可的。光度反演模型与AO图像吻合良好，从而证实了光曲线反演方法和AO图像缩小技术的有效性。

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