标题： 猎户座星云聚集体中的核质量函数：什么决定了最终的恒星质量？ 显示英文标题

标题： The Core Mass Function in the Orion Nebula Cluster Region: What Determines the Final Stellar Masses?

摘要： 将树状图分析方法应用于CARMA-NRO C$^{18}$O ($J$=1--0)数据（角分辨率约为$\sim$8"），我们在猎户座星云团（ONC）区域识别出了692个密集核。 利用这一核样本，我们比较了同一区域内的核质量和初始恒星质量函数，以量化从核到恒星的转变过程。大约22%的被识别出的核是引力束缚的。 对于无星核推导出的核心质量函数(CMF)在质量范围大于1$M_\odot$时具有与Salpeter的初始恒星质量函数(IMF)相似的斜率，这与先前的研究一致。 我们的CMF在亚太阳质量0.1$\sim$$M_\odot$处有一个峰值，这与在同一区域推导出的IMF的峰值质量相当。 我们还发现当前的恒星形成率与只有自引力的无星核能产生恒星的图像是一致的。 然而，由于核心质量不能以100%的效率吸积到恒星上，这些核心必须从周围环境中获得额外的气体来重现当前的IMF（例如，其斜率和峰值质量）。因此，来自周围的质量吸积可能在决定恒星最终质量方面起着关键作用。 显示英文摘要

摘要： Applying dendrogram analysis to the CARMA-NRO C$^{18}$O ($J$=1--0) data having an angular resolution of $\sim$ 8", we identified 692 dense cores in the Orion Nebula Cluster (ONC) region. Using this core sample, we compare the core and initial stellar mass functions in the same area to quantify the step from cores to stars. About 22 \% of the identified cores are gravitationally bound. The derived core mass function (CMF) for starless cores has a slope similar to Salpeter's stellar initial mass function (IMF) for the mass range above 1 $M_\odot$, consistent with previous studies. Our CMF has a peak at a subsolar mass of $\sim$ 0.1 $M_\odot$, which is comparable to the peak mass of the IMF derived in the same area. We also find that the current star formation rate is consistent with the picture in which stars are born only from self-gravitating starless cores. However, the cores must gain additional gas from the surroundings to reproduce the current IMF (e.g., its slope and peak mass), because the core mass cannot be accreted onto the star with a 100\% efficiency. Thus, the mass accretion from the surroundings may play a crucial role in determining the final stellar masses of stars.