Emisión \gamma de supervientos galácticos

Star-forming galaxies are the first extragalactic $\gamma$-ray sources whose emission comes mostly from phenomena linked to their stellar populations. The strongest evidence suppoting this interpretation is the quasi-linear correlation between their $\gamma$-ray luminosities and their star formation rates, observed by the Fermi mission. Recently, it has been proposed that the $\gamma$-ray emission of one of these galaxies (NGC 253) could be explained by the interaction of relativistic particles, accelerated in its galactic superwind, with radiation fields and surrounding matter. In this work we extend this model to galaxies with different star formation rates, and explore its ability to explain the aforementioned correlation. We find that the model pedicts a change in the slope of the correlation, contrary to those in which the emission comes from the disk. Although the model describes the observed luminosities in order of magnitude, the trend is at most marginally consistent with observations.