%0 Generic %1 tasca2014evolving %A Tasca, L. A. M. %A Fevre, O. Le %A Hathi, N. P. %A Schaerer, D. %A Ilbert, O. %A Zamorani, G. %A Lemaux, B. C. %A Cassata, P. %A Garilli, B. %A Brun, V. Le %A Maccagni, D. %A Pentericci, L. %A Thomas, R. %A Vanzella, E. %A Zucca, E. %A Amorin, R. %A Bardelli, S. %A Cassara, L. P. %A Castellano, M. %A Cimatti, A. %A Cucciati, O. %A Durkalec, A. %A Fontana, A. %A Giavalisco, M. %A Grazian, A. %A Paltani, S. %A Ribeiro, B. %A Scodeggio, M. %A Sommariva, V. %A Talia, M. %A Tresse, L. %A Vergani, D. %A Capak, P. %A Charlot, S. %A Contini, T. %A Cuby, J. G. %A de la Torre, S. %A Dunlop, J. %A Fotopoulou, S. %A Koekemoer, A. %A Lopez-Sanjuan, C. %A Mellier, Y. %A Pforr, J. %A Salvato, M. %A Scoville, N. %A Taniguchi, Y. %A Wang, P. W. %D 2014 %K evolution mass redshift relation sfr %T The evolving SFR-M_star relation and sSFR since z~5 from the VUDS spectroscopic survey %U http://arxiv.org/abs/1411.5687 %X We study the evolution of the star formation rate (SFR) - stellar mass (M_star) relation and specific star formation rate (sSFR) of star forming galaxies (SFGs) since a redshift z~5.5 using 2435 (4531) galaxies with highly reliable (reliable) spectroscopic redshifts in the VIMOS Ultra-Deep Survey (VUDS). It is the first time that these relations can be followed over such a large redshift range from a single homogeneously selected sample of galaxies with spectroscopic redshifts. The log(SFR) - log(M_star) relation for SFGs remains roughly linear all the way up to z=5 but the SFR steadily increases at fixed mass with increasing redshift. We find that for stellar masses M_star>3.2 x 10^9 M_sun the SFR increases by a factor ~13 between z=0.4 and z=2.3. We extend this relation up to z=5, finding an additional increase in SFR by a factor 1.7 from z=2.3 to z=4.8 for masses M_star > 10^10 M_sun. We observe a turn-off in the SFR-M_star relation at the highest mass end up to a redshift z~3.5. We interpret this turn-off as the signature of a strong on-going quenching mechanism and rapid mass growth. The sSFR increases strongly up to z~2 but it grows much less rapidly in 2<z<5. We find that the shape of the sSFR evolution is not well reproduced by cold gas accretion-driven models or the latest 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 rapidly with Phi=2.8+-0.2. Above z~2, the reverse is happening with the data evolving more slowly with Phi=1.2+-0.1. The observed sSFR evolution over a large redshift range 0<z<5 and our finding of a non linear main sequence at high mass both indicate that the evolution of SFR and M_star is not solely driven by gas accretion. The results presented in this paper emphasize the need to invoke a more complex mix of physical processes abridge

@misc{tasca2014evolving, abstract = {We study the evolution of the star formation rate (SFR) - stellar mass (M_star) relation and specific star formation rate (sSFR) of star forming galaxies (SFGs) since a redshift z~5.5 using 2435 (4531) galaxies with highly reliable (reliable) spectroscopic redshifts in the VIMOS Ultra-Deep Survey (VUDS). It is the first time that these relations can be followed over such a large redshift range from a single homogeneously selected sample of galaxies with spectroscopic redshifts. The log(SFR) - log(M_star) relation for SFGs remains roughly linear all the way up to z=5 but the SFR steadily increases at fixed mass with increasing redshift. We find that for stellar masses M_star>3.2 x 10^9 M_sun the SFR increases by a factor ~13 between z=0.4 and z=2.3. We extend this relation up to z=5, finding an additional increase in SFR by a factor 1.7 from z=2.3 to z=4.8 for masses M_star > 10^10 M_sun. We observe a turn-off in the SFR-M_star relation at the highest mass end up to a redshift z~3.5. We interpret this turn-off as the signature of a strong on-going quenching mechanism and rapid mass growth. The sSFR increases strongly up to z~2 but it grows much less rapidly in 2<z<5. We find that the shape of the sSFR evolution is not well reproduced by cold gas accretion-driven models or the latest 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 rapidly with Phi=2.8+-0.2. Above z~2, the reverse is happening with the data evolving more slowly with Phi=1.2+-0.1. The observed sSFR evolution over a large redshift range 0<z<5 and our finding of a non linear main sequence at high mass both indicate that the evolution of SFR and M_star is not solely driven by gas accretion. The results presented in this paper emphasize the need to invoke a more complex mix of physical processes {abridge}}, added-at = {2014-11-24T11:02:38.000+0100}, author = {Tasca, L. A. M. and Fevre, O. Le and Hathi, N. P. and Schaerer, D. and Ilbert, O. and Zamorani, G. and Lemaux, B. C. and Cassata, P. and Garilli, B. and Brun, V. Le and Maccagni, D. and Pentericci, L. and Thomas, R. and Vanzella, E. and Zucca, E. and Amorin, R. and Bardelli, S. and Cassara, L. P. and Castellano, M. and Cimatti, A. and Cucciati, O. and Durkalec, A. and Fontana, A. and Giavalisco, M. and Grazian, A. and Paltani, S. and Ribeiro, B. and Scodeggio, M. and Sommariva, V. and Talia, M. and Tresse, L. and Vergani, D. and Capak, P. and Charlot, S. and Contini, T. and Cuby, J. G. and de la Torre, S. and Dunlop, J. and Fotopoulou, S. and Koekemoer, A. and Lopez-Sanjuan, C. and Mellier, Y. and Pforr, J. and Salvato, M. and Scoville, N. and Taniguchi, Y. and Wang, P. W.}, biburl = {https://www.bibsonomy.org/bibtex/20a3bb275d6404570d5d46a29ff19d293/miki}, description = {[1411.5687] The evolving SFR-M_star relation and sSFR since z~5 from the VUDS spectroscopic survey}, interhash = {c7aa11bf5abfe58a0e3f95e78699420e}, intrahash = {0a3bb275d6404570d5d46a29ff19d293}, keywords = {evolution mass redshift relation sfr}, note = {cite arxiv:1411.5687Comment: 10 pages, 4 figures, submitted to A&A}, timestamp = {2014-11-24T11:02:38.000+0100}, title = {The evolving SFR-M_star relation and sSFR since z~5 from the VUDS spectroscopic survey}, url = {http://arxiv.org/abs/1411.5687}, year = 2014 }