In galaxies, the relation between star formation rate (SFR) and morphological type is controversial [1–4]. See also contribution of Hameed & Devereux in these proceedings. To attempt to understand the physical mechanisms that control the morphology of galaxies (thru measurements of structural parameters) and to provide an objective and quantitative method of measuring the flocculency in galaxies, I have explored a novel technique which bears a simple physical interpretation: Star forming regions within a galaxy have a clumpy distribution and can be measured from a galaxy image as the high-spatial frequency (hsf ) power [5,6]. This power must be proportional to the number of HII regions within the galaxy. In this contribution, I present a quantitative measurement of the hsf-power of 30 distant field galaxies from the Hubble Deep Field (HDF) [7] in the UF300W, BF450W, VF606W, and IF814W bands. Galaxies were taken from the redshift catalog of Cowie [8] and have typically z∼0.5 (0.1