2015A&A...583A.128D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST08:17:09

2015A&A...583A.128D - Astronomy and Astrophysics, volume 583A, 128-128 (2015/11-1)

Evolution of clustering length, large-scale bias, and host halo mass at 2 < z < 5 in the VIMOS Ultra Deep Survey (VUDS).

DURKALEC A., LE FEVRE O., POLLO A., DE LA TORRE S., CASSATA P., GARILLI B., LE BRUN V., LEMAUX B.C., MACCAGNI D., PENTERICCI L., TASCA L.A.M., THOMAS R., VANZELLA E., ZAMORANI G., ZUCCA E., AMORIN R., BARDELLI S., CASSARA L.P., CASTELLANO M., CIMATTI A., CUCCIATI O., FONTANA A., GIAVALISCO M., GRAZIAN A., HATHI N.P., ILBERT O., PALTANI S., RIBEIRO B., SCHAERER D., SCODEGGIO M., SOMMARIVA V., TALIA M., TRESSE L., VERGANI D., CAPAK P., CHARLOT S., CONTINI T., CUBY J.G., DUNLOP J., FOTOPOULOU S., KOEKEMOER A., LOPEZ-SANJUAN C., MELLIER Y., PFORR J., SALVATO M., SCOVILLE N., TANIGUCHI Y. and WANG P.W.

Abstract (from CDS):

We investigate the evolution of galaxy clustering for galaxies in the redshift range 2.0<z<5.0 using the VIMOS Ultra Deep Survey (VUDS). We present the projected (real-space) two-point correlation function wp(rp) measured by using 3022 galaxies with robust spectroscopic redshifts in two independent fields (COSMOS and VVDS-02h) covering in total 0.8deg2. We quantify how the scale dependent clustering amplitude r0 changes with redshift making use of mock samples to evaluate and correct the survey selection function. Using a power-law model ξ(r)=(r/r0)–γ we find that the correlation function for the general population is best fit by a model with a clustering length r0=3.95+0.48–0.54 h–1Mpc and slope γ=1.8+0.02–0.06 at z∼2.5, r0=4.35±0.60 h–1Mpc and γ=1.6+0.12–0.13 at z∼3.5. We use these clustering parameters to derive the large-scale linear galaxy bias bLPL, between galaxies and dark matter. We find bLPL=2.68±0.22 at redshift z∼3 (assuming σ8=0.8), significantly higher than found at intermediate and low redshifts for the similarly general galaxy populations. We fit a halo occupation distribution (HOD) model to the data and we obtain that the average halo mass at redshift z∼3 is Mh=1011.75±0.23h–1M. From this fit we confirm that the large-scale linear galaxy bias is relatively high at bLHOD=2.82±0.27. Comparing these measurements with similar measurements at lower redshifts we infer that the star-forming population of galaxies at z∼3 should evolve into the massive and bright (Mr←21.5) galaxy population, which typically occupy haloes of mass <Mh≥ 1013.9h–1M at redshift z=0.

Abstract Copyright:

Journal keyword(s): large-scale structure of Universe - cosmology: observations - methods: statistical - galaxies: evolution

Simbad objects: 2

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Number of rows : 2

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Extended Chandra Deep Field South reg 03 32 30.0 -27 48 20           ~ 614 0
2 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 2069 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-08:17:09

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