THE KNOTTY STRUCTURE OF THE HII DWARF GALAXY F348

[OIII] images and blue spectra of the emission-line dwarf galaxy F348 are presented. In [OIII] light, the object contains two knots about 9 '' NE of the nucleus and one large extended knot 11 '' to the SW. The nuclear region is hundred times less luminous in emission-line light t han the knots. Despite the presence of line intensity ratios [OIII]lam bda 5007/H beta > 3 the prior classification as a Seyfert-2 object can not be upheld. This clinches an earlier suggestion by Veron-Cetty & Ve ron (1986). In particular, we show that the line spectra can be modele d with photoionization models employing stellar input continua. Also, the line luminosities of the extranuclear knots are typical for giant HII regions. There is neither evidence for tidal tails nor for high ve locity differences between the knots. In addition, the linear arrangem ent of the knots does not support interaction. It rather suggests self -propagating star formation In this picture, the faintness of the nucl ear region can be understood by an edge-on view. In addition, the nucl ear starburst appears to be fading in contrast to the young extranucle ar star formation regions. Within the scheme of Melnick (1987), F348 h as to be classified as a multiple-system HII galaxy.