Unveiling the role of galactic rotation on star formation
  We study the star formation process at galactic scales and the role of
rotation through numerical simulations of spiral and starburst galaxies using
the adaptive mesh refinement code Enzo. We focus on the study of three
integrated star formation laws found in the literature: the Kennicutt-Schmidt
(KS) and Silk-Elmegreen (SE) laws, and the dimensionally homogeneous equation
proposed by Escala (2015) $\Sigma_{\rm SFR} \propto \sqrt{G/L}\Sigma_{\rm
gas}^{1.5}$. We show that using the last we take into account the effects of
the integration along the line of sight and find a unique regime of star
formation for both types of galaxies, suppressing the observed bi-modality of
the KS law. We find that the efficiencies displayed by our simulations are
anti-correlated with the angular velocity of the disk $\Omega$ for the three
laws studied in this work. Finally, we show that the dimensionless efficiency
of star formation is well represented by an exponentially decreasing function
of $-1.9\Omega t_{\rm ff}^{\rm ini}$, where $t_{\rm ff}^{\rm ini}$ is the
initial free-fall time. This leads to a unique galactic star formation relation
which reduces the scatter of the bi-modal KS, SE, and Escala (2015) relations
by 43%, 43%, and 35% respectively.
