致密星暴星系团的图像建模：I。R136
Image modeling of compact starburst clusters: I. R136
摘要：
HST数据质量的不断进步，最近的多波长高分辨率光谱学和大型望远镜地面自适应光学的高对比度成像需要R136的建模，以了解其性质和演变阶段。为了得到R136的最佳合成多波长图像，我们需要模拟动力学和恒星演化、质量分离和双星分数对年轻大质量星系团生存的影响，并将R136在LMC中的初始参数设置为这个著名星系团的现有知识。我们使用NBODY 6代码产生了一系列32个年轻的大质量星系团。每个集群跟踪足够的时间样本，以遵循R136在其早期阶段的演变。为了将NBODY 6模拟与观测数据进行比较，我们根据代码的输出创建了合成图像。我们使用TLUSTY和KURUCZ模式大气产生HST/WFPC 2过滤器中的通量。日内瓦等时线被用来追踪恒星的演化。然后，我们从合成场景中获得了在F814 W滤波器（790.48nm）中HST/WFPC 2空间分辨率下的可观测参数。利用团簇的表面亮度分布、半光半径、质量函数和近邻半径等参数对R136进行了表征。我们通过在HST的相同分辨率、像素尺度和FOV下创建合成场景，将R136的模拟与其HST图像进行了比较。我们对图像进行了与真实图像相同的光度分析。在提取了恒星源后，我们估算了R136的质量函数、表面亮度剖面、半光半径和近邻半径。对这些标准的解释表明，最初的非隔离群集情景更能代表R136。这一结果支持了大质量恒星是通过吸积而不是碰撞形成的。
英文摘要：
Continuous progress in data quality from HST, recent multiwavelength high resolution spectroscopy and high contrast imaging from ground adaptive optics on large telescopes need modeling of R136 to understand its nature and evolutionary stage. To produce the best synthesized multiwavelength images of R136 we need to simulate the effect of dynamical and stellar evolution, mass segregation and binary stars fraction on the survival of young massive clusters with the initial parameters of R136 in the LMC, being set to the present knowledge of this famous cluster. We produced a series of 32 young massive clusters using the NBODY6 code. Each cluster was tracked with adequate temporal samples to follow the evolution of R136 during its early stages. To compare the NBODY6 simulations with observational data, we created the synthetic images from the output of the code. We used the TLUSTY and KURUCZ model atmospheres to produce the fluxes in HST/ WFPC2 filters. GENEVA isochrones were used to track the evolution of stars. Then, we derived the observable parameters from synthetic scenes at the spatial resolution of HST/WFPC2 in the F814W filter (790.48nm). Surface brightness profile of the cluster, half-light radius, mass function and neighbor radius were used to select the best representation of R136. We compared the simulations of R136 to its HST imagery by creating synthetic scenes at the same resolution, pixel scale and FOV of the HST. We applied the same photometric analysis of the images as of the real ones. Having extracted the stellar sources, we estimated the mass-function, the surface brightness profile, the half-light radius and the neighbor radius across R136. The interpretation of these criteria point to the fact that an initially non-segregated cluster scenario is more representative of R136. This result pleads for the formation of massive stars by accretion instead of collision.
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