observe many head-tail structures of stellar body vs. stripped-off ISM? Several candidates exist which, however, are characterized as BCDs with decentered bright star-forming knots (see e.g. [@noe00]). The recently detected best candidate in the rapid phase of RPS in the Virgo cluster is VCC1217/IC4318 [@fum11]: A main almost old stellar body of $3 \times 10^8 \Msun$ leaves behind a bundle of $\Ha$ and near-UV emitting knots. Nevertheless, the gas distribution and SF progression within some blobs are not fully understandable. It is still, in general, unclear to what extent the ram pressure can trigger SF by compression of the ISM.

Other BCDs are observed although their gas is already exhausted [@del08]. Peebles et al. [@pee08] find a number of dIrrs with excessively high metallicity, what they interpret as the last stage of gas consumption before they reach the dE state.

On the other hand, rejuvenation of a fraction of cluster dEs seems also to occur which are found to harbour central warm gas [@mic04]. Whether this fact is indicative of a possible re-transformation from gas-free to gaseous DGs by gas accretion is a matter of debate, since it seems impossible within cluster environments, but plausible in less dense regions where 