Variations in the initial mass function across the galaxy population

初始质量函数描述了在巨型分子云中恒星形成过程中形成的恒星的质量分布，它是无数天文努力的核心。国际货币基金组织本身是恒星形成物理学的直接标志，但它也是将可观测到的(恒星或星系光)转化为物理量(如总质量)的必要组成部分。虽然有证据表明IMF的形状在不同的环境中有所不同，但我们大多仍然假设IMF在所有环境和所有宇宙尺度上都是恒定的。利用来自暗能量光谱分析仪器(DESI)的数据，这个博士项目将寻找整个银河系人口中IMF形状的系统变化，并作为红移的函数，将迄今观察到的各种“轶事”结果纳入一张连贯的图片，然后提供给恒星形成模型和实际实施。

The initial mass function, which describe the distribution of masses of the stars formed through the process of star formation in giant molecular clouds, is at the core of countless astronomical endeavours. The IMF in itself is of interest as a direct signpost of the physics of star formation, but it also a necessary ingredient when converting observables (star- or galaxy light) into physical quantities (such as total masses). While there is evidence for variations in the shape of the IMF in different environments, we mostly still assume that the IMF is constant in all environments and at all cosmic scales. Using data from the Dark Energy Spectroscopic Instrument (DESI), this PhD project will look for systematic changes in the shape of the IMF across the galaxy population and as a function of redshift, to bring various "anecdotal" results observed so far into a cohesive picture that can then feed into models of star formation and practical implementations.