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We study the clustering of galaxies as function of luminosity and redshift inthe range $0.35 < z < 1.25$ using data from the Advanced Large Homogeneous AreaMedium Band Redshift Astronomical (ALHAMBRA) survey. The ALHAMBRA data used inthis work cover $2.38 \mathrm{deg}^2$ in 7 independent fields, after applying adetailed angular selection mask, with accurate photometric redshifts, $\sigma_z\lesssim 0.014 (1+z)$, down to $I_{\rm AB} < 24$. Given the depth of thesurvey, we select samples in $B$-band luminosity down to $L^{\rm th} \simeq0.16 L^{*}$ at $z = 0.9$. We measure the real-space clustering using theprojected correlation function, accounting for photometric redshiftsuncertainties. We infer the galaxy bias, and study its evolution withluminosity. We study the effect of sample variance, and confirm earlier resultsthat the COSMOS and ELAIS-N1 fields are dominated by the presence of largestructures. For the intermediate and bright samples, $L^{\rm med} \gtrsim0.6L^{*}$, we obtain a strong dependence of bias on luminosity, in agreementwith previous results at similar redshift. We are able to extend this study tofainter luminosities, where we obtain an almost flat relation, similar to thatobserved at low redshift. Regarding the evolution of bias with redshift, ourresults suggest that the different galaxy populations studied reside in haloescovering a range in mass between $\log_{10}[M_{\rmh}/(h^{-1}\mathrm{M}_{\odot})] \gtrsim 11.5$ for samples with $L^{\rm med}\simeq 0.3 L^{*}$ and $\log_{10}[M_{\rm h}/(h^{-1}\mathrm{M}_{\odot})] \gtrsim13.0$ for samples with $L^{\rm med} \simeq 2 L^{*}$, with typical occupationnumbers in the range of $\sim 1 - 3$ galaxies per halo.

The ALHAMBRA survey: evolution of galaxy clustering since $z \sim 1$