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 original | English |
|---|---|
| Páginas (desde-hasta) | 801-825 |
| Número de páginas | 25 |
| Publicación | Astronomy and Astrophysics |
| Volumen | 442 |
| N.º | 3 |
| DOI | |
| Estado | Published - 1 nov 2005 |
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ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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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
UR - http://www.scopus.com/inward/record.url?scp=27344436098&partnerID=8YFLogxK
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
IS - 3
ER -