Cosmic rays in galaxies: a probe of star formation

TL;DR

This paper investigates cosmic-ray energy densities in starburst galaxies, linking them to supernova rates and suggesting a truncated stellar initial mass function in starburst nuclei compared to normal galaxies.

Contribution

It provides evidence connecting cosmic-ray levels to supernova activity and proposes a low-mass cutoff in the stellar IMF specific to starburst environments.

Findings

Cosmic-ray energy densities are higher in starburst galaxy centers.

Supernova rates correlate with cosmic-ray energy densities.

Starburst nuclei may have a truncated stellar IMF at ~2 solar masses.

Abstract

Cosmic-ray energy densities in central regions of starburst galaxies, as inferred from radio and gamma-ray measurements of, respectively, non-thermal synchrotron and neutral pion decay emission, are typically U_p = O(100)eV/cm3, i.e. typically at least an order of magnitude larger than near the Galactic center and in other non-very-actively star-forming galaxies. We first show that these very different energy-density levels reflect a similar disparity in the respective supernova rates in the two environments, which is not unexpected given the supernova origin of (Galactic) energetic particles. As a consequence of this correspondence, we then demonstrate that there is partial quantitative evidence that the stellar initial mass function (IMF) in starburst nuclei has a low-mass truncation at ~2M_sun, as predicted by theoretical models of turbulent media, in contrast with the much smaller value of 0.1M_sun that characterizes the low-mass cutoff of the stellar IMF in `normal' galactic environments.