论文标题
分子团块伪装他们的恒星形成效率，每个自由落体时间：我们不能愚弄什么
Molecular clumps disguising their star formation efficiency per freefall time: What we can do not to be fooled
论文作者
论文摘要
与他们所经历的气体均匀密度相比，分子团块中体积密度梯度的存在使它们能够提高恒星的形成速率。这种较高的恒星形成速率又产生了我们测量的每个自由落体时间的恒星形成效率的较高值。因此，测得的星形形成效率每次自由度时间$ε_{\ rm ff，meas} $的团块受到困扰。 坡度。本文提出了一种方法，允许人们恢复中心浓缩团块的固有效率。它取决于从团块中心到团块边缘的恒星和气体中表面密度之间的关系。不需要了解团块气体的初始密度曲线。该方法的分步描述是为观察者提供的工具。一旦估算了$ε_ {\ rm ff，int} $，它可以与其测量的，结块平均，对应物$ε_ {\ rm ff，meas} $进行比较，以量化团块的初始气体密度对其星形形成历史的影响。
The presence of a volume density gradient in molecular clumps allow them to raise their star formation rate compared to what they would experience were their gas uniform in density. This higher star formation rate yields in turn a higher value for the star formation efficiency per freefall time that we measure. The measured star formation efficiency per freefall time $ε_{\rm ff, meas}$ of clumps is therefore plagued by a degeneracy, as two factors contribute to it: one is the density gradient of the clump gas, the other is the intrinsic star formation efficiency per freefall time $ε_{\rm ff, int}$ with which the clump would form stars should there be no gas density gradient. This paper presents a method allowing one to recover the intrinsic efficiency of a centrally-concentrated clump. It hinges on the relation between the surface densities in stars and gas measured locally from clump center to clump edge. Knowledge of the initial density profile of the clump gas is not required. A step-by-step description of the method is provided as a tool in hand for observers. Once $ε_{\rm ff, int}$ has been estimated, it can be compared with its measured, clump-averaged, counterpart $ε_{\rm ff, meas}$ to quantify the impact that the initial gas density profile of a clump has had on its star formation history.
