  Nuclei of early-type dwarf galaxies (dEs) are usually younger than the galaxy
main body, and such discrepancy in age has been a puzzle. To explore the origin
of young nuclei in dEs, we study a sample of dEs having compact star-forming
blobs that are visually similar to dEs' nuclei but by far bluer. We find that
(1) the compact star-forming blobs have a typical stellar mass of one percent
of the host galaxy stellar mass; (2) some of the blobs are positioned slightly
off from the center of the galaxies; (3) the H$\alpha$ equivalent width
measured from the publicly available Sloan Digital Sky Survey fiber
spectroscopy shows their formation ages being an order of few Mega-year; and
(4) their emission line metallicities, 12\,+\,log(O/H), are as high as the
solar value, while the underlying galaxies have the typical stellar populations
of dEs, i.e., log(Z/Z$_{\sun}$)\,$\sim$\,$-0.8$. Based on the results, we argue
that the central star-forming blobs can provide a caught-in-the-act view of
nuclei formation in dEs, and discussing possible formation mechanisms of young
nuclei in old dEs. We particularly propose that these off-centered compact
star-forming regions may act as seeds of nuclei as proposed in the `wet
migration' scenario of \cite{Guillard16}.
