Astrophys. J., 609, 525-538 (2004/July-2)
The DEEP2 galaxy redshift survey: clustering of galaxies in early data.
COIL A.L., DAVIS M., MADGWICK D.S., NEWMAN J.A., CONSELICE C.J., COOPER M., ELLIS R.S., FABER S.M., FINKBEINER D.P., GUHATHAKURTA P., KAISER N., KOO D.C., PHILLIPS A.C., STEIDEL C.C., WEINER B.J., WILLMER C.N.A. and YAN R.
Abstract (from CDS):
We measure the two-point correlation function ξ(rp,π) in a sample of 2219 galaxies between z=0.7 and 1.35 to a magnitude limit of RAB=24.1 from the first season of the DEEP2 Galaxy Redshift Survey. From ξ(rp,π) we recover the real-space correlation function, ξ(r), which we find can be approximated within the errors by a power law, ξ(r)=(r/r0)–γ, on scales ∼0.1-10 h–1 Mpc. In a sample with an effective redshift of zeff=0.82, for a ΛCDM cosmology we find r0=3.53±0.81 h–1 Mpc (comoving) and γ=1.66±0.12, while in a higher redshift sample with zeff=1.14 we find r0=3.12±0.72 h–1 Mpc and γ=1.66±0.12. These errors are estimated from mock galaxy catalogs and are dominated by the cosmic variance present in the current data sample. We find that red, absorption-dominated, passively evolving galaxies have a larger clustering scale length, r0, than blue, emission-line, actively star-forming galaxies. Intrinsically brighter galaxies also cluster more strongly than fainter galaxies at z≃1. Our results imply that the DEEP2 galaxies have an effective bias b=0.96±0.13 if σ8DM=1 today or b=1.19±0.16 if σ8DM=0.8 today. This bias is lower than that predicted by semianalytic simulations at z≃1, which may be the result of our R-band target selection. We discuss possible evolutionary effects within our survey volume, and we compare our results with galaxy-clustering studies at other redshifts, noting that our star-forming sample at z≃1 has selection criteria very similar to the Lyman break galaxies at z≃3 and that our red, absorption-line sample displays a clustering strength comparable to the expected clustering of the Lyman break galaxy descendants at z≃1. Our results demonstrate that galaxy-clustering properties as a function of color, spectral type, and luminosity seen in the local universe were largely in place by z≃1.
Galaxies: Distances and Redshifts - Galaxies: Evolution - Galaxies: High-Redshift - Galaxies: Statistics - Cosmology: Large-Scale Structure of Universe - Surveys
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