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We present the initial imaging and spectroscopic data acquired as part of the Very Large Telescope (VLT) VIMOS Lyman‐break galaxy Survey.  UBR  (or  UBVI ) imaging covers five  ≈36 × 36  arcmin 2  fields centred on bright   z  &gt; 3  quasi‐stellar objects (QSOs), allowing  ≈21 000 2 &lt;  z  &lt; 3.5  galaxy candidates to be selected using the Lyman‐break technique. We performed spectroscopic follow‐up using VLT VIMOS, measuring redshifts for  1020  z  &gt; 2  Lyman‐break galaxies and  10  z  &gt; 2  QSOs from a total of 19 VIMOS pointings. From the galaxy spectra, we observe a  625 ± 510 km s −1   velocity offset between the interstellar absorption and Lyman α emission‐line redshifts, consistent with previous results. Using the photometric and spectroscopic catalogues, we have analysed the galaxy clustering at   z ≈ 3 . The angular correlation function,   w (θ) , is well fitted by a double power law with clustering scalelength,   r  0 = 3.19 +0.32  −0.54   h  −1  Mpc  and slope  γ= 2.45  for   r  &lt; 1  h  −1  Mpc  and   r  0 = 4.37 +0.43  −0.55   h  −1  Mpc  with  γ= 1.61 ± 0.15  at larger scales. Using the redshift sample we estimate the semiprojected correlation function,   w  p (σ),  and, for a  γ= 1.8  power law, find   r  0 = 3.67 +0.23  −0.24   h  −1  Mpc  for the VLT sample and   r  0 = 3.98 +0.14  −0.15   h  −1  Mpc  for a combined VLT+Keck sample. From  ξ( s )  and  ξ(σ, π) , and assuming the above  ξ( r )  models, we find that the combined VLT and Keck surveys require a galaxy pairwise velocity dispersion of  ≈700 km s −1  , higher than  ≈400 km s −1   assumed by previous authors. We also measure a value for the gravitational growth rate parameter of  β( z = 3) = 0.48 ± 0.17 , again higher than that previously found and implying a low value for the bias of   b = 2.06 +1.1  −0.5  . This value is consistent with the galaxy clustering amplitude which gives   b = 2.22 ± 0.16 , assuming the standard cosmology, implying that the evolution of the gravitational growth rate is also consistent with Einstein gravity. Finally, we have compared our Lyman‐break galaxy clustering amplitudes with lower redshift measurements and find that the clustering strength is not inconsistent with that of low‐redshift   L *  spirals for simple ‘long‐lived’ galaxy models.

The VLT LBG Redshift Survey – I. Clustering and dynamics of ≈1000 galaxies at z ≈ 3 ★