  Our goal is to study the evolution of the $B-$band luminosity function (LF)
since $z=1$ using ALHAMBRA data. We used the photometric redshift and the
$I-$band selection magnitude probability distribution functions (PDFs) of those
ALHAMBRA galaxies with $I\leq24$ mag to compute the posterior LF. We
statistically studied quiescent and star-forming galaxies using the template
information encoded in the PDFs. The LF covariance matrix in
redshift-magnitude-galaxy type space was computed, including the cosmic
variance. That was estimated from the intrinsic dispersion of the LF
measurements in the 48 ALHAMBRA sub-fields. The uncertainty due to the
photometric redshift prior is also included in our analysis. We modelled the LF
with a redshift-dependent Schechter function affected by the same selection
effects than the data. The measured ALHAMBRA LF at $0.2\leq z<1$ and the
evolving Schechter parameters both for quiescent and star-forming galaxies
agree with previous results in the literature. The estimated redshift evolution
of $M_B^* \propto Qz$ is $Q_{\rm SF}=-1.03\pm0.08$ and $Q_{\rm
Q}=-0.80\pm0.08$, and of $\log \phi^* \propto Pz$ is $P_{\rm SF}=-0.01\pm0.03$
and $P_{\rm Q}=-0.41\pm0.05$. The measured faint-end slopes are $\alpha_{\rm
SF}=-1.29\pm0.02$ and $\alpha_{\rm Q}=-0.53\pm0.04$. We find a significant
population of faint quiescent galaxies, modelled by a second Schechter function
with slope $\beta=-1.31\pm0.11$. We find a factor $2.55\pm0.14$ decrease in the
luminosity density $j_B$ of star-forming galaxies, and a factor $1.25\pm0.16$
increase in the $j_B$ of quiescent ones since $z=1$, confirming the continuous
build-up of the quiescent population with cosmic time. The contribution of the
faint quiescent population to $j_B$ increases from 3% at $z=1$ to 6% at $z=0$.
The developed methodology will be applied to future multi-filter surveys such
as J-PAS.
