Variations in the initial mass function across the galaxy population

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.