色觉星等图、概率综合模型和初始质量函数的质量上限
Colour-magnitude diagrams, probabilistic synthesis models and the upper mass limit of the initial mass function
摘要：
本文利用恒星光度分布函数，给出了色星等图（CMD）与综合模型之间的内在联系。CMD研究直接使用恒星光度分布函数，而一般来说，合成模型只使用其平均值，即使高阶矩也可以获得。在概率综合模型的形式下，我们证明了恒星系综的平均、高阶矩和积分光度分布函数与恒星光度分布函数有关。更多的细节已经在Cervin ~ o和Luridiana（2006）以及其中的参考文献中提出。作为这种形式主义的直接应用，我们讨论两个关键问题。第一，初始质量函数的质量上限是团簇总质量的函数。第二，我们应用极值理论表明，从归一化的IMF之间的最大和最大值的集群质量不提供集群质量的情况下，只有一个明星在这个质量范围内是本，在IGIMF理论假设。相反，它提供了一个60%的概率有一个质量大于mmax的恒星的集群质量，我们认为，根据这一结果的基本公式的IGIMF理论必须修改。
英文摘要：
We present the underlying relations between colour-magnitude diagrams (CMDs) and synthesis models through the use of stellar luminosity distribution func- tions. CMDs studies make a direct use of the stellar luminosity distribution function while, in general, synthesis models only use its mean value, even though high-order moments can also be obtained. We show that the mean, high-order moments and in- tegrated luminosity distribution functions of stellar ensembles are related to the stellar luminosity distribution function, within the formalism of probabilistic synthesis mod- els. More details have been yet presented in Cervin ~ o & Luridiana (2006) and references therein. As a direct application of this formalism, we discuss two key issues. First, in- ferences on the upper mass limit of the initial mass function as a function of the total mass of clusters. Second, we apply extreme value theory to show that that the cluster mass obtained from normalising the IMF between mmax and mup does not provide the cluster mass in the case where only one star in this mass range is present, as assumed in the IGIMF theory. It provides instead the cluster mass with a 60% probability to have a star with mass larger than mmax, and we argue that in light of this result the basic formulation ofthe IGIMF theory must be revised.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
