What can machine learning tell us about the background expansion of the Universe?

Machine learning (ML) algorithms have revolutionized the way we interpret data in astronomy, particle physics, biology, and even economics, since they can remove biases due to a priori chosen models. Here we apply a particular ML method, the genetic algorithms (GA), to cosmological data that describes the background expansion of the Universe, namely the pantheon Type Ia supernovae and the Hubble expansion history $H(z)$ datasets. We obtain model independent and nonparametric reconstructions of the luminosity distance ${d}_{L}(z)$ and Hubble parameter $H(z)$ without assuming any dark energy model or a flat Universe. We then estimate the deceleration parameter $q(z)$, a measure of the acceleration of the Universe, and we make a $\ensuremath{\sim}4.5\ensuremath{\sigma}$ model independent detection of the accelerated expansion, but we also place constraints on the transition redshift of the acceleration phase $({z}_{\mathrm{tr}}=0.662\ifmmode\pm\else\textpm\fi{}0.027)$. We also find a deviation from $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ at high redshifts, albeit within the errors, hinting toward the recently alleged tension between the SnIa/quasar data and the cosmological constant $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model at high redshifts ($z\ensuremath{\gtrsim}1.5$). Finally, we show the GA can be used in complementary null tests of the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ via reconstructions of the Hubble parameter and the luminosity distance.