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Gaseous flows inside and outside galaxies are key to understanding galaxyevolution, as they regulate their star formation activity across cosmic time.We study the ISM kinematics of 330 CIII or HeII emitters, using far-UV ISMabsorption lines detected in the VANDELS spectra. These galaxies span a broadrange of stellar masses M$_\ast$ from $10^8$ to $10^{11}$ M$_\odot$, and SFRsfrom 1 to 500 M$_\odot$/yr, in the redshift range between 2 and 5. We find thatthe bulk ISM velocity v$_{ism}$ is globally in outflow, with v$_{ism}$ of -60$\pm$ 10 km/s for low ionization gas traced by SiII 1260 Angstrom, CII 1334,SiII 1526, and AlII 1670, and v$_{ism}$ of -160 $\pm$ 30 and -170 $\pm$ 30 km/sfor higher ionization gas traced respectively by AlIII 1854-1862 and SiIV1393-1402. Interestingly, BPASS models are able to better reproduce the stellarcontinuum around the SiIV doublet than other stellar population templates. Forindividual galaxies, $34\%$ of the sample has a positive ISM velocity shift,almost double the fraction reported at lower redshifts. Comparing v$_{ism}$ tothe host galaxies properties, we find no significant correlations with M$_\ast$or SFR, and only a marginally significant dependence (at $\sim 2\sigma$) onmorphology-related parameters, with slightly higher velocities in galaxies ofsmaller size (probed by the equivalent radius), higher concentration, andhigher SFR surface density. The outflows are consistent with models ofaccelerating, momentum-driven winds, with densities decreasing towards theoutskirts. Our moderately lower ISM velocities compared to those found insimilar studies at lower redshifts suggest that inflows and internal turbulencemight play an increased role at $z>2$. We estimate mass outflow ratescomparable to the SFRs of the galaxies, and an average escape velocity of 625km/s, suggesting that most of the ISM will remain bound to the galaxy halo.

Properties of the interstellar medium in star-forming galaxies at redshifts 2 < z < 5 from the VANDELS survey