1. Clustering in the Cosmic Evolution Survey (COSMOS) Luigi Guzzo (INAF, Milano) N. Scoville, A. El Zant, O. Le Fevre, B. Meneux, A. Pollo & COSMOS Team (Fundamental photometry and catalogue work: B. Mobasher, P. Capak, H. Aussel, H. Mc Cracken, S. Lilly, P. Shopbell, Y. Taniguchi, D. Thompson)

2. Basic goal of COSMOS: measure the interplay between the growth of large-scale structure and the formation and evolution of galaxy properties within it (morphology, SED, size, luminosity, presence of central black hole, …)  Quantify local structure via moments of the galaxy distribution: mean density, two-point correlation function, higher-order moments  Measure two-point correlation function as a function of redshift from photo-z COSMOS catalogue

3. COSMOS photo-z catalogue: U (CFHT) + BVriz (Subaru) + K (KPNO/CTIO)

4.  Redshift-space correlations simply destroyed by photo-z errors  Solution: treat redshift errors as (very large) redshift-space distortions and use projected function in z slices

7. I AB < 23 (to keep errors down) 150.83 < RA < 149.4 & 1.5 < DEC < 2.9 Redshift slices: 0.1 – 0.5  34973 galaxies 0.2 – 0.6  38084 galaxies 0.3 – 0.7  36940 galaxies 0.4 – 0.8  35481 galaxies 0.5 – 0.9  31809 galaxies 0.6 – 1.0  22363 galaxies (0.8 – 1.2  6590 galaxies) Current analysis facts

11. no apparent evolution of galaxy  (r) when a magnitude-limited sample is analyzed, consistent with results from the VVDS spectroscopic survey (Le Fevre et al. astro-ph/0409135)  combined effect of growth of structure, evolution of galaxy bias (e.g. Marinoni et al 2005) and dependence on luminosity of the latter Correlation length r 0 and slope g of  (r) recovered fairly well via the projected function w p (r p ) over thick redshift slices: mock sample experiments indicate ~20% under-estimate of r 0 To be further improved via: better photo-z via improved photometry (reduced systematics) 21-filter narrow-band SUBARU imaging (Taniguchi et al); VLT-VIMOS spectroscopic survey (60 nights) Next step: measure clustering of morphological classes Summary: