  We consider the simplest scenario when black strings / cigars penetrate the
cosmological brane. As a result, the brane has a Swiss-cheese structure, with
Schwarzschild black holes immersed in a
Friedmann-Lema\^{\i}tre-Robertson-Walker brane. There is no dark radiation in
the model, the cosmological regions of the brane are characterized by a
cosmological constant $\Lambda $ and flat spatial sections. Regardless of the
value of $\Lambda $, these brane-world universes forever expand and forever
decelerate. The totality of source terms in the modified Einstein equation sum
up to a dust, establishing a formal equivalence with the general relativistic
Einstein-Straus model. However in this brane-world scenario with black strings
the evolution of the cosmological fluid strongly depends on $\Lambda $. For
$\Lambda \leq 0$ it has positive energy density $\rho $ and negative pressure
$p$ and at late times it behaves as in the Einstein-Straus model. For (not too
high) positive values of $\Lambda $ the cosmological evolution begins with
positive $\rho $ and negative $p$, but this is followed by an epoch with both
$\rho $ and $p$ positive. Eventually, $\rho $ becomes negative, while $p$ stays
positive. A similar evolution is present for high positive values of $\Lambda
$, however in this case the evolution ends in a pressure singularity,
accompanied by a regular behaviour of the cosmic acceleration. This is a novel
type of singularity appearing in brane-worlds.
