The cosmic star formation rate evolution from z = 5 to z = 0 from the VIMOS VLT deep survey

L. Tresse, O. Ilbert, E. Zueca, G. Zamorani, S. Bardelli, S. Arnouts, S. Paltani, L. Pozzetti, D. Bottini, B. Garilli, V. Le Brun, O. Le Fèvre, D. Maccagni, J. P. Picat, R. Scaramella, M. Scodeggio, G. Vettolani, A. Zanichelli, C. Adami, M. AmaboldiM. Bolzonella, A. Cappi, S. Chariot, P. Ciliegi, T. Contini, S. Foucaud, P. Franzetti, I. Gavignaud, L. Guzzo, A. Iovino, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, R. Pellò, A. Polio, M. Radovich, M. Bondi, A. Bongiorno, G. Busarello, O. Cucciati, F. Lamareille, G. Mathez, Y. Mellier, P. Merluzzi, V. Ripepi

Resultado de la investigación: Article

61 Citas (Scopus)

Resumen

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 (ΩM, 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 Åluminosity 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 irregularlike 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 < M AB(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-l mag when the dust-deficient early-type population is increasingly dominating the 5-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.

Idioma originalEnglish
Páginas (desde-hasta)403-419
Número de páginas17
PublicaciónAstronomy and Astrophysics
Volumen472
N.º2
DOI
EstadoPublished - 1 sep 2007

Huella dactilar

star formation rate
galaxies
dust
luminosity
population type
wavelength
rate
stars
active galaxies
elliptical galaxies
field of view
wavelengths
merger
acquisition
time measurement
radio
nuclei

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Tresse, L., Ilbert, O., Zueca, E., Zamorani, G., Bardelli, S., Arnouts, S., ... Ripepi, V. (2007). The cosmic star formation rate evolution from z = 5 to z = 0 from the VIMOS VLT deep survey. Astronomy and Astrophysics, 472(2), 403-419. https://doi.org/10.1051/0004-6361:20066330
Tresse, L. ; Ilbert, O. ; Zueca, 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. ; Amaboldi, M. ; Bolzonella, M. ; Cappi, A. ; Chariot, 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. ; Polio, A. ; Radovich, M. ; Bondi, M. ; Bongiorno, A. ; Busarello, G. ; Cucciati, O. ; Lamareille, F. ; Mathez, G. ; Mellier, Y. ; Merluzzi, P. ; Ripepi, V. / The cosmic star formation rate evolution from z = 5 to z = 0 from the VIMOS VLT deep survey. En: Astronomy and Astrophysics. 2007 ; Vol. 472, N.º 2. pp. 403-419.
@article{722cab8baed44583b3abe8ceb371a362,
title = "The cosmic star formation rate evolution from z = 5 to z = 0 from the VIMOS VLT deep survey",
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 (ΩM, 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 {\AA}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 irregularlike 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 {\AA}) < -21 galaxies the FUV-band density drops by 2 dex from z = 3.9 to z = 1.2, and for the intermediate -21 < M AB(1500 {\AA}) < -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-l mag when the dust-deficient early-type population is increasingly dominating the 5-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.",
keywords = "Cosmology: observations, Galaxies: evolution, Galaxies: luminosity function, mass function",
author = "L. Tresse and O. Ilbert and E. Zueca and G. Zamorani and S. Bardelli and S. Arnouts and S. Paltani and L. Pozzetti and D. Bottini and B. Garilli and {Le Brun}, V. and {Le F{\`e}vre}, O. and D. Maccagni and Picat, {J. P.} and R. Scaramella and M. Scodeggio and G. Vettolani and A. Zanichelli and C. Adami and M. Amaboldi and M. Bolzonella and A. Cappi and S. Chariot and P. Ciliegi and T. Contini and S. Foucaud and P. Franzetti and I. Gavignaud and L. Guzzo and A. Iovino and McCracken, {H. J.} and B. Marano and C. Marinoni and A. Mazure and B. Meneux and R. Merighi and R. Pell{\`o} and A. Polio 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",
year = "2007",
month = "9",
day = "1",
doi = "10.1051/0004-6361:20066330",
language = "English",
volume = "472",
pages = "403--419",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "2",

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Tresse, L, Ilbert, O, Zueca, E, Zamorani, G, Bardelli, S, Arnouts, S, Paltani, S, Pozzetti, L, Bottini, D, Garilli, B, Le Brun, V, Le Fèvre, O, Maccagni, D, Picat, JP, Scaramella, R, Scodeggio, M, Vettolani, G, Zanichelli, A, Adami, C, Amaboldi, M, Bolzonella, M, Cappi, A, Chariot, S, Ciliegi, P, Contini, T, Foucaud, S, Franzetti, P, Gavignaud, I, Guzzo, L, Iovino, A, McCracken, HJ, Marano, B, Marinoni, C, Mazure, A, Meneux, B, Merighi, R, Pellò, R, Polio, A, Radovich, M, Bondi, M, Bongiorno, A, Busarello, G, Cucciati, O, Lamareille, F, Mathez, G, Mellier, Y, Merluzzi, P & Ripepi, V 2007, 'The cosmic star formation rate evolution from z = 5 to z = 0 from the VIMOS VLT deep survey', Astronomy and Astrophysics, vol. 472, n.º 2, pp. 403-419. https://doi.org/10.1051/0004-6361:20066330

The cosmic star formation rate evolution from z = 5 to z = 0 from the VIMOS VLT deep survey. / Tresse, L.; Ilbert, O.; Zueca, 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.; Amaboldi, M.; Bolzonella, M.; Cappi, A.; Chariot, 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.; Polio, A.; Radovich, M.; Bondi, M.; Bongiorno, A.; Busarello, G.; Cucciati, O.; Lamareille, F.; Mathez, G.; Mellier, Y.; Merluzzi, P.; Ripepi, V.

En: Astronomy and Astrophysics, Vol. 472, N.º 2, 01.09.2007, p. 403-419.

Resultado de la investigación: Article

TY - JOUR

T1 - The cosmic star formation rate evolution from z = 5 to z = 0 from the VIMOS VLT deep survey

AU - Tresse, L.

AU - Ilbert, O.

AU - Zueca, E.

AU - Zamorani, G.

AU - Bardelli, S.

AU - Arnouts, S.

AU - Paltani, S.

AU - Pozzetti, L.

AU - Bottini, D.

AU - Garilli, B.

AU - Le Brun, V.

AU - Le Fèvre, O.

AU - Maccagni, D.

AU - Picat, J. P.

AU - Scaramella, R.

AU - Scodeggio, M.

AU - Vettolani, G.

AU - Zanichelli, A.

AU - Adami, C.

AU - Amaboldi, M.

AU - Bolzonella, M.

AU - Cappi, A.

AU - Chariot, S.

AU - Ciliegi, P.

AU - Contini, T.

AU - Foucaud, S.

AU - Franzetti, P.

AU - Gavignaud, I.

AU - Guzzo, L.

AU - Iovino, A.

AU - McCracken, H. J.

AU - Marano, B.

AU - Marinoni, C.

AU - Mazure, A.

AU - Meneux, B.

AU - Merighi, R.

AU - Pellò, R.

AU - Polio, A.

AU - Radovich, M.

AU - Bondi, M.

AU - Bongiorno, A.

AU - Busarello, G.

AU - Cucciati, O.

AU - Lamareille, F.

AU - Mathez, G.

AU - Mellier, Y.

AU - Merluzzi, P.

AU - Ripepi, V.

PY - 2007/9/1

Y1 - 2007/9/1

N2 - 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 (ΩM, 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 Åluminosity 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 irregularlike 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 < M AB(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-l mag when the dust-deficient early-type population is increasingly dominating the 5-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.

AB - 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 (ΩM, 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 Åluminosity 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 irregularlike 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 < M AB(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-l mag when the dust-deficient early-type population is increasingly dominating the 5-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.

KW - Cosmology: observations

KW - Galaxies: evolution

KW - Galaxies: luminosity function, mass function

UR - http://www.scopus.com/inward/record.url?scp=34548645922&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20066330

DO - 10.1051/0004-6361:20066330

M3 - Article

AN - SCOPUS:34548645922

VL - 472

SP - 403

EP - 419

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 2

ER -