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(Abridged) Context. Core condensation is a critical step in thestar-formation process, but is still poorly characterized observationally.Aims. We have studied the 10 pc-long L1495/B213 complex in Taurus toinvestigate how dense cores have condensed out of the lower-density cloudmaterial. Results. From the N$_2$H$^+$ emission, we identify 19 dense cores,some starless and some protostellar. They are not distributed uniformly, buttend to cluster with relative separations on the order of 0.25 pc. From theC$^{18}$O emission, we identify multiple velocity components in the gas. Wehave characterized them by fitting gaussians to the spectra, and by studyingthe distribution of the fits in position-position-velocity space. In thisspace, the C$^{18}$O components appear as velocity-coherent structures, and wehave identified them automatically using a dedicated algorithm (FIVe: FriendsIn Velocity). Using this algorithm, we have identified 35 filamentarycomponents with typical lengths of 0.5 pc, sonic internal velocity dispersions,and mass-per-unit-length close to the stability threshold of isothermalcylinders at 10 K. Core formation seems to have occurred inside the filamentarycomponents via fragmentation, with a small number of fertile components withlarger mass-per-unit-length being responsible for most cores in the cloud. Atlarge scales, the filamentary components appear grouped into families, which werefer to as bundles. Conclusions. Core formation in L1495/B213 has proceeded byhierarchical fragmentation. The cloud fragmented first into several pc-scaleregions. Each of these regions later fragmented into velocity-coherentfilaments of about 0.5 pc in length. Finally, a small number of these filamentsfragmented quasi-statically and produced the individual dense cores we seetoday.

Cores, filaments, and bundles: hierarchical core formation in the L1495/B213 Taurus region