局部体积的形态
Morphology of the Local Volume
摘要：
为了研究全球形态的星系分布在我们当地的邻居，我们计算的闵可夫斯基泛函的一个序列的体积有限的样本内的一个球体的8兆秒差距集中在我们的星系。在闵可夫斯基泛函中，我们可以清楚地看到星系的强聚集性以及大尺度上空洞和相干结构的优势。星系分布的形态随着极限绝对星等的变化而变化。这些样本包含了更明亮的星系，显示出更空的空洞和更明显的相干结构。事实上，有一个突出的峰值孤立星系的光度函数MB约。-14，这至少部分地解释了这些形态变化。我们比较从LambdaCDM模拟晕样品。特别注意再现所观察到的局部邻域以及在这些模拟样本中观察到的光度函数。总而言之，模拟样本很好地呈现了星系分布的全球形态。然而，详细的形态分析表明，真正的星系团更强大，观察到的空隙更空，结构更明显的模拟样品相比，从LambdaCDM模拟。
英文摘要：
To study the global morphology of the galaxy distribution in our local neighbourhood we calculate the Minkowski functionals for a sequence of volume limited samples within a sphere of 8 Mpc centred on our galaxy. The well known strong clustering of the galaxies and the dominance of voids and coherent structures on larger scales is clearly visible in the Minkowski functionals. The morphology of the galaxy distribution changes with the limiting absolute magnitude. The samples, encompassing the more luminous galaxies, show emptier voids and more pronounced coherent structures. Indeed there is a prominent peak in the luminosity function of isolated galaxies for MB approx. -14, which at least partly explains these morphological changes. We compare with halo samples from a LambdaCDM simulation. Special care was taken to reproduce the observed local neighbourhood as well as the observed luminosity function in these mock samples. All in all the mock samples render the global morphology of the galaxy distribution quite well. However the detailed morphological analysis reveals that real galaxies cluster stronger, the observed voids are emptier and the structures are more pronounced compared to the mock samples from the LambdaCDM simulation.
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