arXiv 1104.45382011-04-23astro-ph.SR

年轻星群和星团中恒星和核心的质量分布

Mass distributions of stars and cores in young groups and clusters

Manon Michel, Helen Kirk, Philip C. Myers

备注：: 48 pages, 17 figures, accepted for publication in Astrophysical Journal
发表信息：: 2011 ApJ ,735, 51
DOI：: 10.1088/0004-637X/735/1/51

摘要：

利用14个年轻恒星群的恒星质量和位置，研究了恒星初始质量函数（IMF）和致密核质量函数（CMF）之间的关系。初始柱密度图是通过用具有相同恒星形成效率（SFE）的模型初始核心替换每个恒星来计算的。对于每一组的SFE，核心模型，观测分辨率不同，以产生一个现实的范围内的初始地图。一个clumpfinding算法解析每个初始地图到导出的核心，导出的核心质量，和导出的CMF。主要的结果是，预计混合的初始核心导致衍生核心太少，太大。导出核的数量比初始核的数量少平均因子1.4在稀疏组和5在拥挤组。导出的CMF峰值处的质量超过初始CMF峰值处的质量，在稀疏组中平均因子为1.0，在拥挤组中平均因子为12.1。这些结果意味着，在拥挤的年轻集团和星团中，观测到的核心的质量分布可能无法可靠地预测将在这些核心中形成的原恒星的质量分布。

英文摘要：

We investigate the relation of the stellar initial mass function (IMF) and the dense core mass function (CMF), using stellar masses and positions in 14 well-studied young groups. Initial column density maps are computed by replacing each star with a model initial core having the same star formation efficiency (SFE). For each group the SFE, core model, and observational resolution are varied to produce a realistic range of initial maps. A clumpfinding algorithm parses each initial map into derived cores, derived core masses, and a derived CMF. The main result is that projected blending of initial cores causes derived cores to be too few and too massive. The number of derived cores is fewer than the number of initial cores by a mean factor 1.4 in sparse groups and 5 in crowded groups. The mass at the peak of the derived CMF exceeds the mass at the peak of the initial CMF by a mean factor 1.0 in sparse groups and 12.1 in crowded groups. These results imply that in crowded young groups and clusters, the mass distribution of observed cores may not reliably predict the mass distribution of protostars which will form in those cores.

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