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We present measurements of galaxy clustering at redshift <z>=0.6 using 10360galaxies with photometric redshifts over an area of 0.78 square degree from theCOMBO-17 survey. To obtain a result that is unaffected by redshiftuncertainties, we calculate the projected correlation function w(r_p), givingresults for red sequence and blue cloud galaxies separately. The correlationfunction of the red galaxies displays clear deviations from a power law atcomoving separations around 1 to 3 h^-1 Mpc, and similar but weaker trends aresuggested by the data for the blue galaxies. To interpret these results, we fitthe correlation functions with analytical predictions derived from a simplehalo occupation model. This combines linear clustering of the underlying masswith a description of the number of galaxies occupying each dark-matter halo(the halo occupation distribution). If the occupation numbers are taken to be asimple power law with N proportional to M^alpha, then alpha ~ 0.5 and alpha ~0.2 for red and blue galaxies respectively. These figures are little differentfrom the values required to fit present-day clustering data. The power-spectrumshape is assumed to be known in this exercise, but we allow the data todetermine the preferred value of sigma_8, the linear power-spectrumnormalization. The average normalization inferred from red and blue galaxies at<z> =0.6 is sigma_8=1.02+-0.17 at zero redshift, consistent with independentestimates of this local value. This agreement can be regarded as a verificationof the hierarchical growth of the halo mass function.Comment: 12 pages, 10 figures, accepted for publication by A&

Galaxy clustering from COMBO-17: the halo occupation distribution at $\langle\textit{z}\rangle$ = 0.6