The ALHAMBRA survey: evolution of galaxy clustering since $z \sim 1$
  We study the clustering of galaxies as function of luminosity and redshift in
the range $0.35 < z < 1.25$ using data from the Advanced Large Homogeneous Area
Medium Band Redshift Astronomical (ALHAMBRA) survey. The ALHAMBRA data used in
this work cover $2.38 \mathrm{deg}^2$ in 7 independent fields, after applying a
detailed angular selection mask, with accurate photometric redshifts, $\sigma_z
\lesssim 0.014 (1+z)$, down to $I_{\rm AB} < 24$. Given the depth of the
survey, we select samples in $B$-band luminosity down to $L^{\rm th} \simeq
0.16 L^{*}$ at $z = 0.9$. We measure the real-space clustering using the
projected correlation function, accounting for photometric redshifts
uncertainties. We infer the galaxy bias, and study its evolution with
luminosity. We study the effect of sample variance, and confirm earlier results
that the COSMOS and ELAIS-N1 fields are dominated by the presence of large
structures. For the intermediate and bright samples, $L^{\rm med} \gtrsim
0.6L^{*}$, we obtain a strong dependence of bias on luminosity, in agreement
with previous results at similar redshift. We are able to extend this study to
fainter luminosities, where we obtain an almost flat relation, similar to that
observed at low redshift. Regarding the evolution of bias with redshift, our
results suggest that the different galaxy populations studied reside in haloes
covering a range in mass between $\log_{10}[M_{\rm
h}/(h^{-1}\mathrm{M}_{\odot})] \gtrsim 11.5$ for samples with $L^{\rm med}
\simeq 0.3 L^{*}$ and $\log_{10}[M_{\rm h}/(h^{-1}\mathrm{M}_{\odot})] \gtrsim
13.0$ for samples with $L^{\rm med} \simeq 2 L^{*}$, with typical occupation
numbers in the range of $\sim 1 - 3$ galaxies per halo.
