The VIMOS VLT Deep Survey*,** Evolution of the non-linear galaxy bias up to z = 1.5

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

Resultado de la investigación: Article

68 Citas (Scopus)

Resumen

We present the first measurements of the Probability Distribution Function (PDF) of galaxy fluctuations in the four-passes, first-epoch VIMOS-VLT Deep Survey (VVDS) cone, covering 0.4×0.4 deg between 0.4 < z < 1.5. We show that the PDF of density contrasts of the VVDS galaxies is an unbiased tracer of the underlying parent distribution up to redshift z = 1.5, on scales R = 8 and 10 h-1 Mpc. The second moment of the PDF, i.e., the rms fluctuations of the galaxy density field, is to a good approximation constant over the full redshift baseline investigated: we find that, in redshift space, σ8 for galaxies brighter than MB c = -20 + 5 log h has a mean value of 0.94 ± 0.07 in the redshift interval 0.7 < z < 1.5. The third moment, i.e., the skewness, increases with cosmic time: we find that the probability of having underdense regions is greater at z ∼ 0.7 than it was at z ∼ 1.5. By comparing the PDF of galaxy density contrasts with the theoretically predicted PDF of mass fluctuations we infer the redshift-, density- and scale-dependence of the biasing function b(z,δ,R) between galaxy and matter overdensities up to redshift z = 1.5. Our results can be summarized as follows: i) the galaxy bias is an increasing function of redshift: evolution is marginal up to z ∼ 0.8 and more pronounced for z ≳ 0.8; ii) the formation of bright galaxies is inhibited below a characteristic mass-overdensity threshold whose amplitude increases with redshift and luminosity; iii) the biasing function is non linear in all the redshift bins investigated with non-linear effects of the order of a few to ∼10% on scales >5 h-1 Mpc. By subdividing the sample according to galaxy luminosity and colors, we also show that: iv) brighter galaxies are more strongly biased than less luminous ones at every redshift and the dependence of biasing on luminosity at z ∼ 0.8 is in good agreement with what is observed in the local Universe; v) red objects are systematically more biased than blue objects at all cosmic epochs investigated, but the relative bias between red and blue objects is constant as a function of redshift in the interval 0.7 < z < 1.5, and its value (brel ∼ 1.4) is similar to what is found at z ∼ 0.

Idioma originalEnglish
Páginas (desde-hasta)801-825
Número de páginas25
PublicaciónAstronomy and Astrophysics
Volumen442
N.º3
DOI
EstadoPublished - 1 nov 2005

Huella dactilar

galaxies
luminosity
time measurement
probability distribution functions
cones
coverings
universe
intervals
color
distribution

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Marinoni, C., Le Fèvre, O., Meneux, B., Iovino, A., Pollo, A., Ilbert, O., ... Rizzo, D. (2005). The VIMOS VLT Deep Survey*,** Evolution of the non-linear galaxy bias up to z = 1.5. Astronomy and Astrophysics, 442(3), 801-825. https://doi.org/10.1051/0004-6361:20052966
Marinoni, C. ; Le Fèvre, O. ; Meneux, B. ; Iovino, A. ; Pollo, A. ; Ilbert, O. ; Zamorani, G. ; Guzzo, L. ; Mazure, A. ; Scaramella, R. ; Cappi, A. ; McCracken, H. J. ; Bottini, D. ; Garilli, B. ; Le Brun, V. ; Maccagni, D. ; Picat, J. P. ; Scodeggio, M. ; Tresse, L. ; Vettolani, G. ; Zanichelli, A. ; Adami, C. ; Arnouts, S. ; Bardelli, S. ; Blaizot, J. ; Bolzonella, M. ; Charlot, S. ; Ciliegi, P. ; Contini, T. ; Foucaud, S. ; Franzetti, P. ; Gavignaud, I. ; Marano, B. ; Mathez, G. ; Merighi, R. ; Paltani, S. ; Pellò, R. ; Pozzetti, L. ; Radovich, M. ; Zucca, E. ; Bondi, M. ; Bongiorno, A. ; Busarello, G. ; Colombi, S. ; Cucciati, O. ; Lamareille, F. ; Mellier, Y. ; Merluzzi, P. ; Ripepi, V. ; Rizzo, D. / The VIMOS VLT Deep Survey*,** Evolution of the non-linear galaxy bias up to z = 1.5. En: Astronomy and Astrophysics. 2005 ; Vol. 442, N.º 3. pp. 801-825.
@article{1975a0b4e4f54c6a84236cb3d7a2d0bd,
title = "The VIMOS VLT Deep Survey*,** Evolution of the non-linear galaxy bias up to z = 1.5",
abstract = "We present the first measurements of the Probability Distribution Function (PDF) of galaxy fluctuations in the four-passes, first-epoch VIMOS-VLT Deep Survey (VVDS) cone, covering 0.4×0.4 deg between 0.4 < z < 1.5. We show that the PDF of density contrasts of the VVDS galaxies is an unbiased tracer of the underlying parent distribution up to redshift z = 1.5, on scales R = 8 and 10 h-1 Mpc. The second moment of the PDF, i.e., the rms fluctuations of the galaxy density field, is to a good approximation constant over the full redshift baseline investigated: we find that, in redshift space, σ8 for galaxies brighter than MB c = -20 + 5 log h has a mean value of 0.94 ± 0.07 in the redshift interval 0.7 < z < 1.5. The third moment, i.e., the skewness, increases with cosmic time: we find that the probability of having underdense regions is greater at z ∼ 0.7 than it was at z ∼ 1.5. By comparing the PDF of galaxy density contrasts with the theoretically predicted PDF of mass fluctuations we infer the redshift-, density- and scale-dependence of the biasing function b(z,δ,R) between galaxy and matter overdensities up to redshift z = 1.5. Our results can be summarized as follows: i) the galaxy bias is an increasing function of redshift: evolution is marginal up to z ∼ 0.8 and more pronounced for z ≳ 0.8; ii) the formation of bright galaxies is inhibited below a characteristic mass-overdensity threshold whose amplitude increases with redshift and luminosity; iii) the biasing function is non linear in all the redshift bins investigated with non-linear effects of the order of a few to ∼10{\%} on scales >5 h-1 Mpc. By subdividing the sample according to galaxy luminosity and colors, we also show that: iv) brighter galaxies are more strongly biased than less luminous ones at every redshift and the dependence of biasing on luminosity at z ∼ 0.8 is in good agreement with what is observed in the local Universe; v) red objects are systematically more biased than blue objects at all cosmic epochs investigated, but the relative bias between red and blue objects is constant as a function of redshift in the interval 0.7 < z < 1.5, and its value (brel ∼ 1.4) is similar to what is found at z ∼ 0.",
keywords = "Cosmology: large-scale structure of Universe, Galaxies: distances and redshifts, Galaxies: evolution, Galaxies: statistics",
author = "C. Marinoni and {Le F{\`e}vre}, O. and B. Meneux and A. Iovino and A. Pollo and O. Ilbert and G. Zamorani and L. Guzzo and A. Mazure and R. Scaramella and A. Cappi and McCracken, {H. J.} and D. Bottini and B. Garilli and {Le Brun}, V. and D. Maccagni and Picat, {J. P.} and M. Scodeggio and L. Tresse and G. Vettolani and A. Zanichelli and C. Adami and S. Arnouts and S. Bardelli and J. Blaizot and M. Bolzonella and S. Charlot and P. Ciliegi and T. Contini and S. Foucaud and P. Franzetti and I. Gavignaud and B. Marano and G. Mathez and R. Merighi and S. Paltani and R. Pell{\`o} and L. Pozzetti and M. Radovich and E. Zucca and M. Bondi and A. Bongiorno and G. Busarello and S. Colombi and O. Cucciati and F. Lamareille and Y. Mellier and P. Merluzzi and V. Ripepi and D. Rizzo",
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journal = "Astronomy and Astrophysics",
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Marinoni, C, Le Fèvre, O, Meneux, B, Iovino, A, Pollo, A, Ilbert, O, Zamorani, G, Guzzo, L, Mazure, A, Scaramella, R, Cappi, A, McCracken, HJ, Bottini, D, Garilli, B, Le Brun, V, Maccagni, D, Picat, JP, Scodeggio, M, Tresse, L, Vettolani, G, Zanichelli, A, Adami, C, Arnouts, S, Bardelli, S, Blaizot, J, Bolzonella, M, Charlot, S, Ciliegi, P, Contini, T, Foucaud, S, Franzetti, P, Gavignaud, I, Marano, B, Mathez, G, Merighi, R, Paltani, S, Pellò, R, Pozzetti, L, Radovich, M, Zucca, E, Bondi, M, Bongiorno, A, Busarello, G, Colombi, S, Cucciati, O, Lamareille, F, Mellier, Y, Merluzzi, P, Ripepi, V & Rizzo, D 2005, 'The VIMOS VLT Deep Survey*,** Evolution of the non-linear galaxy bias up to z = 1.5', Astronomy and Astrophysics, vol. 442, n.º 3, pp. 801-825. https://doi.org/10.1051/0004-6361:20052966

The VIMOS VLT Deep Survey*,** Evolution of the non-linear galaxy bias up to z = 1.5. / Marinoni, C.; Le Fèvre, O.; Meneux, B.; Iovino, A.; Pollo, A.; Ilbert, O.; Zamorani, G.; Guzzo, L.; Mazure, A.; Scaramella, R.; Cappi, A.; McCracken, H. J.; Bottini, D.; Garilli, B.; Le Brun, V.; Maccagni, D.; Picat, J. P.; Scodeggio, M.; Tresse, L.; Vettolani, G.; Zanichelli, A.; Adami, C.; Arnouts, S.; Bardelli, S.; Blaizot, J.; Bolzonella, M.; Charlot, S.; Ciliegi, P.; Contini, T.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Marano, B.; Mathez, G.; Merighi, R.; Paltani, S.; Pellò, R.; Pozzetti, L.; Radovich, M.; Zucca, E.; Bondi, M.; Bongiorno, A.; Busarello, G.; Colombi, S.; Cucciati, O.; Lamareille, F.; Mellier, Y.; Merluzzi, P.; Ripepi, V.; Rizzo, D.

En: Astronomy and Astrophysics, Vol. 442, N.º 3, 01.11.2005, p. 801-825.

Resultado de la investigación: Article

TY - JOUR

T1 - The VIMOS VLT Deep Survey*,** Evolution of the non-linear galaxy bias up to z = 1.5

AU - Marinoni, C.

AU - Le Fèvre, O.

AU - Meneux, B.

AU - Iovino, A.

AU - Pollo, A.

AU - Ilbert, O.

AU - Zamorani, G.

AU - Guzzo, L.

AU - Mazure, A.

AU - Scaramella, R.

AU - Cappi, A.

AU - McCracken, H. J.

AU - Bottini, D.

AU - Garilli, B.

AU - Le Brun, V.

AU - Maccagni, D.

AU - Picat, J. P.

AU - Scodeggio, M.

AU - Tresse, L.

AU - Vettolani, G.

AU - Zanichelli, A.

AU - Adami, C.

AU - Arnouts, S.

AU - Bardelli, S.

AU - Blaizot, J.

AU - Bolzonella, M.

AU - Charlot, S.

AU - Ciliegi, P.

AU - Contini, T.

AU - Foucaud, S.

AU - Franzetti, P.

AU - Gavignaud, I.

AU - Marano, B.

AU - Mathez, G.

AU - Merighi, R.

AU - Paltani, S.

AU - Pellò, R.

AU - Pozzetti, L.

AU - Radovich, M.

AU - Zucca, E.

AU - Bondi, M.

AU - Bongiorno, A.

AU - Busarello, G.

AU - Colombi, S.

AU - Cucciati, O.

AU - Lamareille, F.

AU - Mellier, Y.

AU - Merluzzi, P.

AU - Ripepi, V.

AU - Rizzo, D.

PY - 2005/11/1

Y1 - 2005/11/1

N2 - We present the first measurements of the Probability Distribution Function (PDF) of galaxy fluctuations in the four-passes, first-epoch VIMOS-VLT Deep Survey (VVDS) cone, covering 0.4×0.4 deg between 0.4 < z < 1.5. We show that the PDF of density contrasts of the VVDS galaxies is an unbiased tracer of the underlying parent distribution up to redshift z = 1.5, on scales R = 8 and 10 h-1 Mpc. The second moment of the PDF, i.e., the rms fluctuations of the galaxy density field, is to a good approximation constant over the full redshift baseline investigated: we find that, in redshift space, σ8 for galaxies brighter than MB c = -20 + 5 log h has a mean value of 0.94 ± 0.07 in the redshift interval 0.7 < z < 1.5. The third moment, i.e., the skewness, increases with cosmic time: we find that the probability of having underdense regions is greater at z ∼ 0.7 than it was at z ∼ 1.5. By comparing the PDF of galaxy density contrasts with the theoretically predicted PDF of mass fluctuations we infer the redshift-, density- and scale-dependence of the biasing function b(z,δ,R) between galaxy and matter overdensities up to redshift z = 1.5. Our results can be summarized as follows: i) the galaxy bias is an increasing function of redshift: evolution is marginal up to z ∼ 0.8 and more pronounced for z ≳ 0.8; ii) the formation of bright galaxies is inhibited below a characteristic mass-overdensity threshold whose amplitude increases with redshift and luminosity; iii) the biasing function is non linear in all the redshift bins investigated with non-linear effects of the order of a few to ∼10% on scales >5 h-1 Mpc. By subdividing the sample according to galaxy luminosity and colors, we also show that: iv) brighter galaxies are more strongly biased than less luminous ones at every redshift and the dependence of biasing on luminosity at z ∼ 0.8 is in good agreement with what is observed in the local Universe; v) red objects are systematically more biased than blue objects at all cosmic epochs investigated, but the relative bias between red and blue objects is constant as a function of redshift in the interval 0.7 < z < 1.5, and its value (brel ∼ 1.4) is similar to what is found at z ∼ 0.

AB - We present the first measurements of the Probability Distribution Function (PDF) of galaxy fluctuations in the four-passes, first-epoch VIMOS-VLT Deep Survey (VVDS) cone, covering 0.4×0.4 deg between 0.4 < z < 1.5. We show that the PDF of density contrasts of the VVDS galaxies is an unbiased tracer of the underlying parent distribution up to redshift z = 1.5, on scales R = 8 and 10 h-1 Mpc. The second moment of the PDF, i.e., the rms fluctuations of the galaxy density field, is to a good approximation constant over the full redshift baseline investigated: we find that, in redshift space, σ8 for galaxies brighter than MB c = -20 + 5 log h has a mean value of 0.94 ± 0.07 in the redshift interval 0.7 < z < 1.5. The third moment, i.e., the skewness, increases with cosmic time: we find that the probability of having underdense regions is greater at z ∼ 0.7 than it was at z ∼ 1.5. By comparing the PDF of galaxy density contrasts with the theoretically predicted PDF of mass fluctuations we infer the redshift-, density- and scale-dependence of the biasing function b(z,δ,R) between galaxy and matter overdensities up to redshift z = 1.5. Our results can be summarized as follows: i) the galaxy bias is an increasing function of redshift: evolution is marginal up to z ∼ 0.8 and more pronounced for z ≳ 0.8; ii) the formation of bright galaxies is inhibited below a characteristic mass-overdensity threshold whose amplitude increases with redshift and luminosity; iii) the biasing function is non linear in all the redshift bins investigated with non-linear effects of the order of a few to ∼10% on scales >5 h-1 Mpc. By subdividing the sample according to galaxy luminosity and colors, we also show that: iv) brighter galaxies are more strongly biased than less luminous ones at every redshift and the dependence of biasing on luminosity at z ∼ 0.8 is in good agreement with what is observed in the local Universe; v) red objects are systematically more biased than blue objects at all cosmic epochs investigated, but the relative bias between red and blue objects is constant as a function of redshift in the interval 0.7 < z < 1.5, and its value (brel ∼ 1.4) is similar to what is found at z ∼ 0.

KW - Cosmology: large-scale structure of Universe

KW - Galaxies: distances and redshifts

KW - Galaxies: evolution

KW - Galaxies: statistics

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U2 - 10.1051/0004-6361:20052966

DO - 10.1051/0004-6361:20052966

M3 - Article

AN - SCOPUS:27344436098

VL - 442

SP - 801

EP - 825

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

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Marinoni C, Le Fèvre O, Meneux B, Iovino A, Pollo A, Ilbert O y otros. The VIMOS VLT Deep Survey*,** Evolution of the non-linear galaxy bias up to z = 1.5. Astronomy and Astrophysics. 2005 nov 1;442(3):801-825. https://doi.org/10.1051/0004-6361:20052966