Kinematical analysis of the ionized gas in the nuclear region of NGC 4214

We present in this paper a detailed study of the kinematical properties of the ionized gas around the young massive star clusters in the nucleus of NG C 4214. The analysis is based on bidimensional spectroscopical data, allowi ng to derive the spatial Variation of different properties (intensity, velo city and width / line splitting) of the emission lines Ha and [O III] lambd a 5007 dong the nuclear region. We have found that the Giant H II region ar ound the two most massive clusters in NHC 4214 (A and B) is resolved into t wo clearly separated regions. We have not detected superbubbles with the pr operties we would expect according to the evolutionary state of the stellar clusters, but just a partial ring feature around the most massive one and two expanding shells around cluster B. The first expanding shell seems to h ave experienced blowout, whereas the second one is still complete. A possib le explanation to this phenomenon is that the most massive stars in a starb urst spend a large fraction of their lives buried inside their original mol ecular clouds. Champagne flows might have formed at the borders of the regi ons, especially on the SE complex, explaining the existence of the diffuse ionized gas around the galaxy. As a consequence of these results we postula te that NGC 4214 is indeed a dwarf spiral galaxy, with a thin (similar to 2 00 pc) disk that inhibits the formation of large scale structures in the IS M. The mechanical input deposited by the star formation complexes, in a var iety of physical processes that include the free expanding bubbles liberate d after blowout and photoevaporation of the parent clouds, have succeeded i n generating the structures now detected far from the disk, giving place to the large-scale structure which now enriches the optical appearance of the galaxy.