English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We investigate the evolution of galaxy clustering for galaxies in theredshift range 2.0<$z$<5.0 using the VIMOS Ultra Deep Survey (VUDS). We presentthe projected (real-space) two-point correlation function $w_p(r_p)$ measuredby using 3022 galaxies with robust spectroscopic redshifts in two independentfields (COSMOS and VVDS-02h) covering in total 0.8 deg$^2$. We quantify how thescale dependent clustering amplitude $r_0$ changes with redshift making use ofmock samples to evaluate and correct the survey selection function. Using apower-law model $\xi(r) = (r/r_0)^{-\gamma}$ we find that the correlationfunction for the general population is best fit by a model with a clusteringlength $r_0$=3.95$^{+0.48}_{-0.54}$ h$^{-1}$Mpc and slope$\gamma$=1.8$^{+0.02}_{-0.06}$ at $z$~2.5, $r_0$=4.35$\pm$0.60 h$^{-1}$Mpc and$\gamma$=1.6$^{+0.12}_{-0.13}$ at $z$~3.5. We use these clustering parametersto derive the large-scale linear galaxy bias $b_L^{PL}$, between galaxies anddark matter. We find $b_L^{PL}$ = 2.68$\pm$0.22 at redshift $z$~3 (assuming$\sigma_8$ = 0.8), significantly higher than found at intermediate and lowredshifts. We fit an HOD model to the data and we obtain that the average halomass at redshift $z$~3 is $M_h$=10$^{11.75\pm0.23}$ h$^{-1}$M$_{\odot}$. Fromthis fit we confirm that the large-scale linear galaxy bias is relatively highat $b_L^{HOD}$ = 2.82$\pm$0.27. Comparing these measurements with similarmeasurements at lower redshifts we infer that the star-forming population ofgalaxies at $z$~3 should evolve into the massive and bright ($M_r$<-21.5)galaxy population which typically occupy haloes of mass $\langle M_h\rangle$ =10$^{13.9}$ h$^{-1}$ $M_{\odot}$ at redshift $z$=0.

The evolution of clustering length, large-scale bias and host halo mass at 2