Integral field spectroscopy of a sample of nearby galaxies II. Properties of the H ∥ regions

We analyse the spectroscopic properties of thousands of H II regions identified in 38 face-on spiral galaxies. All galaxies were observed out to 2.4 effective radii using integral field spectroscopy (IFS) over the wavelength range similar to 3700 to similar to 6900 angstrom. The near uniform sample has been assembled from the PPAK IFS Nearby Galaxy (PINGS) survey and a sample described in Paper I. We develop a new automatic procedure to detect H II regions, based on the contrast of the Ha intensity maps extracted from the datacubes. Once detected, the algorithm provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for similar to 2600 independent H II regions/complexes. This is by far the largest H II region survey of its kind. Our selection criteria and the use of 3D spectroscopy guarantee that we cover the regions in an unbiased way. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [O II] lambda 3727 to [S II] lambda 6731). A final catalogue of the spectroscopic properties of H II regions has been created for each galaxy, which includes information on morphology, spiral structure, gas kinematics, and surface brightness of the underlying stellar population. In the current study, we focus on the understanding of the average properties of the H II regions and their radial distributions. We find a significant change in the ionisation characteristics of H II regions within r < 0.25 r(e) due to contamination from sources with different ionising characteristics, as we discuss. We find that the gas-phase oxygen abundance and the Ha equivalent width present a negative and positive gradient, respectively. The distribution of slopes is statistically compatible with a random Gaussian distribution around the mean value, if the radial distances are measured in units of the respective effective radius. No difference in the slope is found for galaxies of different morphologies, e. g. barred/non-barred, grand-design/flocculent. Therefore, the effective radius is a universal scale length for gradients in the evolution of galaxies. Some properties have a large variance across each object and between galaxies (e. g. electron density) without a clear characteristic value. But other properties are well described by an average value either galaxy by galaxy or among the different galaxies (e. g. dust attenuation).