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By means of direct N-body simulations and simplified numerical models, westudy the formation and characteristics of the tidal tails around Palomar 5,along its orbit in the Milky Way potential. Unlike previous findings, we areable to reproduce the substructures observed in the stellar streams of thiscluster, without including any lumpiness in the dark matter halo. We show thatoverdensities similar to those observed in Palomar 5 can be reproduced by theepicyclic motion of stars along its tails, i.e. a simple local accumulation oforbits of stars that escaped from the cluster with very similar positions andvelocities. This process is able to form stellar clumps at distances of severalkiloparsecs from the cluster, so it is not a phenomenon confined to the innerpart of Palomar 5's tails, as previously suggested. Our models can reproducethe density contrast between the clumps and the surrounding tails found in theobserved streams, without including any lumpiness in the dark halo, suggestingnew upper limits on its granularity.

Clumpy streams in a smooth dark halo: the case of Palomar 5