It is observationally and theoretically well established that galaxy clusters grow through the accretion of isolated galaxies and galaxy groups. By accretion to a cluster, consecutive pericenter passages expose a cluster galaxy to strong environmental effects that transform its star formation activity, morphology, and perhaps its internal kinematics. Nevertheless, it is still not entirely clear how the galaxy environment transforms newly accreted satellites into early-type dwarf galaxies (dEs). If host halos such as clusters are in charge of any transformation in the kinematics of dE's progenitors, then at a fixed stellar mass range, do dEs with different infalling time to the host halo show different internal kinematics? This question can be addressed by members of a recently accreted group of galaxies to the Virgo cluster, discovered by Lisker et al. (2018). In this talk, I will present a kinematic analysis of 9 dEs in this particular group. I will compare their kinematics with other dEs in high and low-density environments, using the specific angular momentum (λR) parameter. I will show that recent dE infallers to a cluster such as Virgo exhibit (λR) profiles intermediate between ancient dE infallers and equally massive field galaxies. Moreover, I will discuss the role of pre-processing to explain the spread (λR) profiles we observed in these 9 dEs.