We present Gemini North GMOS/IFU observations of the roots of the NGC 1569 super-galactic wind. This forms part of a larger and on-going study of the formation and collimation mechanisms of galactic winds. Four IFU pointings cover the base of the outflows originating from the central super-star clusters; we present a preliminary analysis for two positions. The choice of single-slit mode and the R831 grating (dispersion = 0.34 Å pix-) allowed us to cover the spectral range 4740-6860Å through 500 object fibres. We observe the nebular diagnostic lines of Hα, Hβ, [OIII]λλ4959,5007, [NII]λλ6548,6583, [SII]λλ6716, 6731. The data were reduced using the standard Gemini pipeline included with IRAF, and corrected for differential atmospheric refraction. We find emission lines clearly composed of multiple components—in most cases a bright narrow feature (intrinsic FWHM = 50 kms-1) superimposed on a fainter broad component (FWHM ≤ 300 kms-1). We discuss the origin of these components, in the context of the wind/interstellar medium interaction.