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The aim of this paper is to investigate spectral and photometric propertiesof 854 faint ($i_{AB}$<~25 mag) star-forming galaxies (SFGs) at 2<z<2.5 usingthe VIMOS Ultra-Deep Survey (VUDS) spectroscopic data and deep multi-wavelengthphotometric data in three extensively studied extragalactic fields (ECDFS,VVDS, COSMOS). These SFGs were targeted for spectroscopy based on theirphotometric redshifts. The VUDS spectra are used to measure the UV spectralslopes ($\beta$) as well as Ly$\alpha$ equivalent widths (EW). On average, thespectroscopically measured $\beta$ (-1.36$\pm$0.02), is comparable to thephotometrically measured $\beta$ (-1.32$\pm$0.02), and has smaller measurementuncertainties. The positive correlation of $\beta$ with the Spectral EnergyDistribution (SED)-based measurement of dust extinction, E$_{\rm s}$(B-V),emphasizes the importance of $\beta$ as an alternative dust indicator at highredshifts. To make a proper comparison, we divide these SFGs into threesubgroups based on their rest-frame Ly$\alpha$ EW: SFGs with no Ly$\alpha$emission (SFG$_{\rm N}$; EW$\le$0\AA), SFGs with Ly$\alpha$ emission (SFG$_{\rmL}$; EW$>$0\AA), and Ly$\alpha$ emitters (LAEs; EW$\ge$20\AA). The fraction ofLAEs at these redshifts is $\sim$10%, which is consistent with previousobservations. We compared best-fit SED-estimated stellar parameters of theSFG$_{\rm N}$, SFG$_{\rm L}$ and LAE samples. For the luminosities probed here($\sim$L$^*$), we find that galaxies with and without Ly$\alpha$ in emissionhave small but significant differences in their SED-based properties. We findthat LAEs have less dust, and lower star-formation rates (SFR) compared tonon-LAEs. We also find that LAEs are less massive compared to non-LAEs, thoughthe difference is smaller and less significant compared to the SFR and E$_{\rms}$(B-V). [abridged]

The VIMOS Ultra Deep Survey: Ly$\alpha$ Emission and Stellar Populations of Star-Forming Galaxies at 2