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: Contribución a una revistaArtículo

69 Citas (Scopus)


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 originalInglés
Páginas (desde-hasta)801-825
Número de páginas25
PublicaciónAstronomy and Astrophysics
EstadoPublicada - 1 nov 2005

Áreas temáticas de ASJC Scopus

  • Astronomía y astrofísica
  • Ciencias planetarias y espacial

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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, H. J., Bottini, D., Garilli, B., Le Brun, V., Maccagni, D., Picat, J. P., Scodeggio, M., Tresse, L., ... 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.