English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We study the evolution of the star formation rate (SFR) - stellar mass(M_star) relation and specific star formation rate (sSFR) of star forminggalaxies (SFGs) since a redshift z~5.5 using 2435 (4531) galaxies with highlyreliable (reliable) spectroscopic redshifts in the VIMOS Ultra-Deep Survey(VUDS). It is the first time that these relations can be followed over such alarge redshift range from a single homogeneously selected sample of galaxieswith spectroscopic redshifts. The log(SFR) - log(M_star) relation for SFGsremains roughly linear all the way up to z=5 but the SFR steadily increases atfixed mass with increasing redshift. We find that for stellar masses M_star>3.2x 10^9 M_sun the SFR increases by a factor ~13 between z=0.4 and z=2.3. Weextend this relation up to z=5, finding an additional increase in SFR by afactor 1.7 from z=2.3 to z=4.8 for masses M_star > 10^10 M_sun. We observe aturn-off in the SFR-M_star relation at the highest mass end up to a redshiftz~3.5. We interpret this turn-off as the signature of a strong on-goingquenching mechanism and rapid mass growth. The sSFR increases strongly up toz~2 but it grows much less rapidly in 2<z<5. We find that the shape of the sSFRevolution is not well reproduced by cold gas accretion-driven models or thelatest hydrodynamical models. Below z~2 these models have a flatter evolution(1+z)^{Phi} with Phi=2-2.25 compared to the data which evolves more rapidlywith Phi=2.8+-0.2. Above z~2, the reverse is happening with the data evolvingmore slowly with Phi=1.2+-0.1. The observed sSFR evolution over a largeredshift range 0<z<5 and our finding of a non linear main sequence at high massboth indicate that the evolution of SFR and M_star is not solely driven by gasaccretion. The results presented in this paper emphasize the need to invoke amore complex mix of physical processes {abridge}

The evolving SFR-M_star relation and sSFR since z~5 from the VUDS spectroscopic survey