LEADER：根据稀少的photometry快速估算小行星形状伸长和自旋纬度分布
LEADER: fast estimates of asteroid shape elongation and spin latitude distributions from scarce photometry
摘要：
许多具有光变曲线亮度测量的小行星数据库（如WISE、Pan-STARRS 1）包含了大量的小行星形状和自旋建模数据。虽然光变曲线反演对于数据稀少的单个目标来说是不合理的，但对于拥有数千颗小行星的大群体来说是可能的，在那里可以获得群体的形状和自旋特征的分布。我们的目标是介绍一个软件实现的方法，计算人口的联合形状伸长率p和自旋纬度β分布，在小行星数据库中的亮度观测。其他主要目标是包括一种方法，用于执行算法的有效性检查，和一个工具，用于人口的统计比较。LEADER软件包从给定的数据库中读取用户定义的亚群的亮度测量数据。观测结果被用来计算种群成员亮度变化的估计值。一个累积分布函数（CDF）的这些估计构建。已知的分析基函数的叠加产生了这个CDF作为（形状，自旋）分布的函数。联合分布可以通过求解线性约束反问题来重构。为了测试该方法的有效性，该算法可以运行与合成小行星模型，其中的形状和自旋特性是已知的，并通过使用从检查数据库中获取的几何形状。LEADER是一个快速而强大的软件包，用于求解大种群的形状和自旋分布。根据所使用的数据库，测量的质量和覆盖范围存在重大差异，因此在可靠地使用数据库之前，总是需要进行综合模拟。我们展示了切换到另一个数据库时结果的差异。
英文摘要：
Many asteroid databases with lightcurve brightness measurements (e.g. WISE, Pan-STARRS1) contain enormous amounts of data for asteroid shape and spin modelling. While lightcurve inversion is not plausible for individual targets with scarce data, it is possible for large populations with thousands of asteroids, where the distributions of the shape and spin characteristics of the populations are obtainable. We aim to introduce a software implementation of a method that computes the joint shape elongation p and spin latitude beta distributions for a population, with the brightness observations given in an asteroid database. Other main goals are to include a method for performing validity checks of the algorithm, and a tool for a statistical comparison of populations. The LEADER software package read the brightness measurement data for a user-defined subpopulation from a given database. The observations were used to compute estimates of the brightness variations of the population members. A cumulative distribution function (CDF) was constructed of these estimates. A superposition of known analytical basis functions yielded this CDF as a function of the (shape, spin) distribution. The joint distribution can be reconstructed by solving a linear constrained inverse problem. To test the validity of the method, the algorithm can be run with synthetic asteroid models, where the shape and spin characteristics are known, and by using the geometries taken from the examined database. LEADER is a fast and robust software package for solving shape and spin distributions for large populations. There are major differences in the quality and coverage of measurements depending on the database used, so synthetic simulations are always necessary before a database can be reliably used. We show examples of differences in the results when switching to another database.
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