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We establish a robust statistical description of the star-forming galaxypopulation at the end of cosmic HI reionization ($5.0\le{}z\le6.6$) from alarge sample of 52 galaxies with spectroscopically confirmed redshifts from theVIMOS UltraDeep Survey. We identify galaxies with Ly$\alpha$ either inabsorption or in emission, at variance with most spectroscopic samples in theliterature where Ly$\alpha$ emitters dominate. We find that star-forminggalaxies at these redshifts are distributed along a main sequence in thestellar mass vs. SFR plane. We report a flat evolution of the sSFR(z) in 3<z<6compared to lower redshift measurements. UV-continuum slopes vary withluminosity, with a large dispersion. We determing UV and Ly$\alpha$ luminosityfunctions using V$_{max}$ method and use them to derive star formation ratedensities (SFRD). We find that both UV-derived and Ly$\alpha$-derived SFRDs arein excellent agreement after correcting Ly$\alpha$ luminosity density for IGMabsorption. Our new SFRD measurements at a mean redshift z=5.6 confirm thesteep decline of the SFRD at z>2. The bright end of the Ly$\alpha$ luminosityfunction has a high number density, indicating a significant star formationactivity concentrated in the brightest Ly$\alpha$ emitters (LAE) at theseredshifts. LAE with EW>25\AA ~contribute to about 75\% of the total UV-derivedSFRD. While our analysis favors a low dust content in 5.0<z<6.6, uncertaintieson the dust extinction correction and associated degeneracies in spectralfitting will remain an issue to estimate the total SFRD until future surveyextending spectroscopy to the NIR rest-frame spectral domain, e.g. with JWST.

astronomy and astrophysics

The UV and Ly$\alpha$ Luminosity Functions of galaxies and the Star  Formation Rate Density at the end of HI reionization from the VIMOS  Ultra-Deep Survey (VUDS)