The cosmic star formation rate evolution from z=5 to z=0 from the VIMOS VLT Deep Survey
Abstract
We present the evolution of the comoving SFR density in the redshift range 0 < z < 5 using the first epoch data release of the VVDS, that is 11564 spectra selected at I_AB=24 over 2200 arcmin^2 in two fields of view, the VVDS-0226-04 and the VVDS-CDFS-0332-27, and the cosmological parameters (Omega_M, Omega_L, h)=(0.3, 0.7, 0.7). We study the multi-wavelength non dust-corrected luminosity densities at 0 < z < 2 from the rest-frame FUV to the optical passbands, and the rest-frame 1500A luminosity functions and densities at 2.7 < z < 5. They evolve from z=1.2 to 0.05 according to (1+z)^{x} with x = 2.05, 1.94, 1.92, 1.14, 0.73, 0.42, 0.30 in the FUV-1500, NUV-2800, U-3600, B-4400, V-5500, R-6500, and I-7900 passbands, respectively. From z = 1.2 to 0.2 the B-band density for the irregular-like galaxies decreases markedly by a factor 3.5 while it increases by a factor 1.7 for the elliptical-like galaxies. We identify several SFR periods; from z = 5 to 3.4 the FUV-band density increases by at most 0.5dex, from z=3.4 to 1.2 it decreases by 0.08dex, from z=1.2 to 0.05 it declines steadily by 0.6dex. For the most luminous M_AB(1500) < -21 galaxies the FUV-band density drops by 2dex from z = 3.9 to 1.2, and for the intermediate -21 < M_AB(1500) < -20 galaxies it drops by 2dex from z = 0.2 to 0. Comparing with dust corrected surveys, at 0.4 < z < 2 the FUV seems obscured by a constant factor of ~1.8-2 mag, while at z < 0.5 it seems progressively less obscured by up to ~0.9-1 mag when the dust-deficient early-type population is increasingly dominating the B-band density. The VVDS results agree with a downsizing picture where the most luminous sources cease to efficiently produce new stars 12 Gyrs ago (at z~4), while intermediate luminosity sources keep producing stars until 2.5 Gyrs ago (at z~0.2).(abridged)
Keywords
Cite
@article{arxiv.astro-ph/0609005,
title = {The cosmic star formation rate evolution from z=5 to z=0 from the VIMOS VLT Deep Survey},
author = {L. Tresse and O. Ilbert and E. Zucca and G. Zamorani and S. Bardelli and S. Arnouts and S. Paltani and L. Pozzetti and D. Bottini and B. Garilli and V. Le Brun and O. Le Fevre and D. Maccagni and J. -P. Picat and R. Scaramella and M. Scodeggio and G. Vettolani and A. Zanichelli and C. Adami and M. Arnaboldi and M. Bolzonella and A. Cappi and S. Charlot and P. Ciliegi and T. Contini and S. Foucaud and P. Franzetti and I. Gavignaud and L. Guzzo and A. Iovino and H. J. McCracken and B. Marano and C. Marinoni and A. Mazure and B. Meneux and R. Merighi and R. Pello and A. Pollo and M. Radovich and M. Bondi and A. Bongiorno and G. Busarello and O. Cucciati and F. Lamareille and G. Mathez and Y. Mellier and P. Merluzzi and V. Ripepi},
journal= {arXiv preprint arXiv:astro-ph/0609005},
year = {2009}
}
Comments
Accepted A&A, April 26, 2007, 18 pages, 12 figures. Final version corrected for Langage Editing and for the Replacement of the caption of Fig 12