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The Star Formation Rate Density (SFRD) history of the Universe is wellconstrained up to redshift $z \sim 2$. At earlier cosmic epochs, the picturehas been largely inferred from UV-selected galaxies (e.g. Lyman-break galaxies,LBGs). However, LBGs' inferred SFRs strongly depend on the assumed dustextinction correction, which is not well-constrained at high-$z$, whileobservations in the radio domain are not affected by this issue. In this workwe measure the SFRD from a 1.4 GHz-selected sample of $\sim$600 galaxies in theGOODS-N field up to redshift $\sim 3.5$. We take into account the contributionof Active Galactic Nuclei from the Infrared-Radio correlation. We measure theradio luminosity function, fitted with a modified Schechter function, andderive the SFRD. The cosmic SFRD shows a rise up to $z \sim 2$ and then analmost flat plateau up to $z \sim 3.5$. Our SFRD is in agreement with the onesfrom other FIR/radio surveys and a factor 2 higher than those from LBG samples.We also estimate that galaxies lacking a counterpart in the HST/WFC3 H-band($H$-dark) make up $\sim 25\%$ of the $\phi$-integrated SFRD relative to thefull sample at z $\sim 3.2$, and up to $58\%$ relative to LBG samples.

A new estimate of the cosmic star formation density from a radio-selected sample, and the contribution of $H$-dark galaxies at $z \geq 3$