nProFit：动力学模型拟合工具
nProFit: a tool for dynamical models fitting
摘要：
星团的表面亮度轮廓（SBPs）包含了有关星团动力学状态的宝贵信息。观察到的恒星星团，特别是球状星团的SBPs，是在良好的协议与预期的SBPs的等温球包含恒星的减少动能。然而，满足这些理论判据的组态的SBPs不能用解析公式唯一地表示，这阻碍了对观测到的星系团动力学状态的分析。为了克服这一缺点，使用最能代表理论模型的核心和晕特征的经验拟合公式已成为一种惯例。我们在这里提出了一个通用的代码，命名为nProFit，它允许拟合河外星团的表面亮度轮廓的理论星团，由King（1966）和Wilson（1975）的动力学模型定义。此外，我们还纳入了理论模型，导致在幂律表面亮度曲线所代表的埃尔森等。1987年。该代码返回基本的尺寸参数，如核心半径，半光半径和潮汐半径，以及动态相关的参数，如体积和表面密度分布，速度色散分布，总质量和结合能为用户固定的质光比。该代码在河外星系团动力学研究中的有用性已经在Cuevas-Otahola et al. 2020中得到了说明。该代码在用户端基于Python，但可以调用Pyraf和Fortran中的高级例程，现在可供公众使用。我们在安装包中提供了示例脚本和模拟集群作为用户指南。
英文摘要：
The surface brightness profiles (SBPs) of star clusters hold invaluable information on the dynamical state of clusters. The observed SBPs of star clusters, especially that of globular clusters, are in good agreement with the SBPs expected for isothermal spheres containing stars of reduced kinetic energies. However, the SBPs of configurations that satisfy these theoretical criteria cannot be uniquely expressed by analytical formulae, which had hindered the analysis of dynamical state of observed clusters in external galaxies. To counter this shortcoming, it has become a practice to use empirical fitting formulae that best represent the core and halo characteristics of theoretical models. We here present a general purpose code, named nProFit, that allows fitting of the surface brightness profiles of extragalactic star clusters to theoretical star clusters, defined by dynamical models of King (1966) and Wilson (1975). In addition, we also incorporated theoretical models that result in power-law surface brightness profiles represented by Elson et al. 1987. The code returns the basic size parameters such as core radius, half-light radius and tidal radius, as well as dynamically relevant parameters, such as the volume and surface density profiles, velocity dispersion profile, total mass and the binding energy for a user-fixed mass-to-light ratio. The usefulness of the code in the dynamical study of extragalactic clusters has been already illustrated in Cuevas-Otahola et al. 2020. The code, which is python-based at the user end, but makes calls to advanced routines in Pyraf and Fortran, is now available for public use. We provide example scripts and mock clusters in the installation package as guide to users.
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