As an observational science, astronomy is benefited from technological developments that allow improvements in the way light is gathered and analyzed. Integral field spectroscopy (IFS) is a modern observational technique that allows to simultaneously obtain spectroscopic and spatial information on a given area on the sky. In this work IFS is used to observe extragalactic Hii regions in the nearby and face on spiral galaxies M33 and M101. For M33 the central zone was observed together with the external region IC 132, located ∼4.7kpc away from the galaxy center, the PMAS instrument was used in the 3.5m telescope at the Calar Alto (CAHA) observatory. For M101 observations where gathered with the GMOS-N instrument at the Gemini 8m telescope in Mauna Kea. The distance to each galaxy, in combination with the field of view of each instrument gives a similar spatial sampling for both sets of regions. Reduction was performed with the tools provided by the telescopes. In the case of PMAS the packages R3D and E3D were used while for GMOS-N the reduction was based on the Gemini routines for IRAF. Additional corrections to compensate for differential atmospheric refraction and atmospheric telluric absorption were applied. With the reduced and corrected data, 2D maps were produced. These maps were in turn used to estimate the distribution of physical conditions along the nebulae, as well as the ionic and total abundances from the direct method, together with empirical indicators based in strong lines. Ionization structure was studied with the ionization sensitive ratios [OIII]/Hβ, [NII]/Hα and [SII]/Hα. The 2D maps where complemented with zones analysis where the regions are divided in shells of equal integrated Hα surface brightness. Given the Hα distribution this is equivalent to a radial analysis. The shells are studied first as single entities and then adding them from the center to the border, simulating increasing apertures. The BPT diagnostic diagram show different locations for the regions, with some spatial resolution elements (spaxels), crossing the stellar photoionization boundaries. These spaxels are part of the diffuse ionized gas (DIG) beyond the Str¨omgren sphere limits, nevertheless this indicates extra precaution required for the use of BPT diagnostic diagram with spatially resolved data.