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Title:
The cosmic star formation rate evolution from z = 5 to z = 0 from the VIMOS VLT deep survey
Authors:
Tresse, L.; Ilbert, O.; Zucca, E.; Zamorani, G.; Bardelli, S.; Arnouts, S.; Paltani, S.; Pozzetti, L.; Bottini, D.; Garilli, B.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Picat, J.-P.; Scaramella, R.; Scodeggio, M.; Vettolani, G.; Zanichelli, A.; Adami, C.; Arnaboldi, M.; Bolzonella, M.; Cappi, A.; Charlot, S.; Ciliegi, P.; Contini, T.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Guzzo, L.; Iovino, A.; McCracken, H. J.; Marano, B.; Marinoni, C.; Mazure, A.; Meneux, B.; Merighi, R.; Pellò, R.; Pollo, A.; Radovich, M.; Bondi, M.; Bongiorno, A.; Busarello, G.; Cucciati, O.; Lamareille, F.; Mathez, G.; Mellier, Y.; Merluzzi, P.; Ripepi, V.
Affiliation:
AA(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France ), AB(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France; Institute for Astronomy, 2680 Woodlawn Dr., University of Hawaii, Honolulu, Hawaii 96822, USA), AC(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AD(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AE(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AF(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AG(Integral Science Data Centre, Ch. d'Écogia 16, 1290 Versoix, Switzerland ; Geneva Observatory, Ch. de Maillettes 51, 1290 Sauverny, Switzerland), AH(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AI(INAF-IASF, via Bassini 15, 20133 Milano, Italy), AJ(INAF-IASF, via Bassini 15, 20133 Milano, Italy), AK(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AL(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AM(INAF-IASF, via Bassini 15, 20133 Milano, Italy), AN(Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), CNRS-Université Paul Sabatier, 14 avenue E. Belin, 31400 Toulouse, France), AO(INAF-IRA, via Gobetti 101, 40129 Bologna, Italy ; INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy), AP(INAF-IASF, via Bassini 15, 20133 Milano, Italy), AQ(INAF-IRA, via Gobetti 101, 40129 Bologna, Italy), AR(INAF-IRA, via Gobetti 101, 40129 Bologna, Italy), AS(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), AT(INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy), AU(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AV(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AW(INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy), AX(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), AY(Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), CNRS-Université Paul Sabatier, 14 avenue E. Belin, 31400 Toulouse, France), AZ(Institut d'Astrophysique de Paris (UMR 7095), 98bis boulevard Arago, 75014 Paris, France), BA(INAF-IASF, via Bassini 15, 20133 Milano, Italy), BB(School of Physics & Astronomy, University of Nottingham, University Park, Nottingham NG72RD, UK), BC(Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany), BD(Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany), BE(INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy ; INAF-Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy), BF(Observatoire de Paris-LERMA, 61 avenue de l'Observatoire, 75014 Paris, France), BG(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France; Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italy), BH(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France), BI(INAF-IASF, via Bassini 15, 20133 Milano, Italy ; Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany), BJ(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy), BK(Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), CNRS-Université Paul Sabatier, 14 avenue E. Belin, 31400 Toulouse, France), BL(Laboratoire d'Astrophysique de Marseille (UMR 6110), CNRS-Université de Provence, BP 8, 13376 Marseille Cedex 12, France; Centre de Physique Théorique (UMR 6207), CNRS-Université de Provence, 13288 Marseille, France), BM(INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy), BN(INAF-IRA, via Gobetti 101, 40129 Bologna, Italy), BO(Observatoire de Paris-LERMA, 61 avenue de l'Observatoire, 75014 Paris, France), BP(INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy), BQ(Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany ; Centre de Physique Théorique (UMR 6207), CNRS-Université de Provence, 13288 Marseille, France), BR(Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), CNRS-Université Paul Sabatier, 14 avenue E. Belin, 31400 Toulouse, France), BS(Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (UMR 5572), CNRS-Université Paul Sabatier, 14 avenue E. Belin, 31400 Toulouse, France), BT(INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy ; INAF-Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy), BU(INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy), BV(INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy)
Publication:
Astronomy and Astrophysics, Volume 472, Issue 2, September III 2007, pp.403-419 (A&A Homepage)
Publication Date:
09/2007
Origin:
EDP Sciences
Keywords:
cosmology: observations, galaxies: evolution, galaxies: luminosity function, mass function
DOI:
10.1051/0004-6361:20066330
Bibliographic Code:
2007A&A...472..403T

Abstract

Context: The VIMOS VLT Deep Survey (VVDS) was undertaken to map the evolution of galaxies, large scale structures, and active galaxy nuclei from the redshift spectroscopic measurements of ~105 objects down to an apparent magnitude IAB = 24, in combination with a multi-wavelength acquisition for radio, infrared, optical, ultraviolet, and X-rays data.
Aims: We present the evolution of the comoving star formation rate (SFR) density in the redshift range 0 < z < 5 using the first epoch data release of the VVDS, that is 11564 spectra over 2200 arcmin2 in two fields of view, the VVDS-0226-04 and the VVDS-CDFS-0332-27, and the cosmological parameters (Ω_M, ΩΛ, h)=(0.3, 0.7, 0.7).
Methods: We study the multi-wavelength non dust-corrected luminosity densities at 0 < z < 2 from the rest-frame far ultraviolet to the optical passbands, and the rest-frame 1500 Å luminosity functions and densities at 2.7 < z < 5.
Results: They evolve from z=1.2 to z=0.05 according to (1+z)x with x = 2.05, 1.94, 1.92, 1.14, 0.73, 0.42, and 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 z=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 0.5 dex, from z=3.4 to 1.2 it decreases by 0.08 dex, from z=1.2 to z=0.05 it declines steadily by 0.6 dex. For the most luminous MAB(1500 Å)<-21 galaxies the FUV-band density drops by 2 dex from z=3.9 to z=1.2, and for the intermediate -21<MAB(1500 Å)<-20 galaxies it drops by 2 dex from z=0.2 to z=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.
Conclusions: 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). A modest contribution of dry mergers and morphologies evolving towards early-type galaxies might contribute to increase the number density of the bright early types at z<1.5. Our observed SFR density is not in agreement with a continuous smooth decrease since z˜4.

Based on observations collected at the European Southern Observatory Very Large Telescope,

Paranal, Chile, program 070.A-9007(A), and on data

obtained at the Canada-France-Hawaii Telescope, operated by the Institut National des Sciences de l'Univers of the

Centre National de la Recherche Scientifique of France, the National Research

Council of Canada, and the University of Hawaii.

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