Advanced morphological galaxy classification: a comparison of observed and simulated galaxies
Advanced morphological galaxy classification: a comparison of observed and simulated galaxies
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高级形态星系分类：观测星系和模拟星系的比较
DOI：
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发表时间：
2011
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通讯作者：
J. Wadsley
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作者：
K. Hambleton;B. Gibson;C. Brook;G. Stinson;C. Conselice;J. Bailin;H. Couchman;J. Wadsley
星系的形态结构中编码了与其形成和演化历史相关的线索。有关星系形态统计的最新进展包括对浓度 (C)、不对称性 (A) 和团块度 (S) 的复杂测量。在这项研究中，这三个参数（CAS）已应用于一组模拟星系，并与从附近星系样本推断的观测结果进行比较。模拟涵盖了一系列质量在 10 10 M⊙ 和 10 12 M⊙ 之间的晚期系统，并采用了 0.1 cm -3 和 100 cm -3 之间的恒星形成密度阈值。我们发现模拟星系的浓度与真实星系的浓度相当。然而，CAS 分析的结果表明，模拟的星系通常更加不对称，并且团块度值的范围超出了观测到的范围。三个 CAS 参数和颜色 (BV) 之间存在很强的相关性，与观测到的星系一致。此外，模拟星系的 CAS 参数和哈勃类型之间具有很强的联系，大部分与真实星系一致。
Encoded within the morphological structure of galaxies are clues related to their formation and evolutionary history. Recent advances pertaining to the statistics of galaxy morphology include sophisticated measures of concentration (C), asymmetry (A), and clumpiness (S). In this study, these three parameters (CAS) have been applied to a suite of simulated galaxies and compared with observational results inferred from a sample of nearby galaxies. The simulations span a range of late-type systems, with masses between �10 10 M⊙ and �10 12 M⊙, and employ star formation density thresholds between 0.1 cm −3 and 100 cm −3 . We have found that the simulated galaxies possess comparable concentrations to their real counterparts. However, the results of the CAS analysis revealed that the simulated galaxies are generally more asymmetric, and that the range of clumpiness values extends beyond the range of those observed. Strong correlations were obtained between the three CAS parameters and colour (BV), consistent with observed galaxies. Furthermore, the simulated galaxies possess strong links between their CAS parameters and Hubble type, mostly in-line with their real counterparts.