  We present a nonparametric morphology analysis of the stellar continuum and
nebular emission lines for a sample of local galaxies. We explore the
dependence of the various morphological parameters on wavelength and
morphological type. Our goal is to quantify the difference in morphology
between the stellar and nebular components. We derive the nonparametric
morphological indicators of 364 galaxies from the CALIFA Survey. To calculate
those indicators, we apply the StatMorph package on the high-quality integral
field spectroscopic data cubes, as well as to the most prominent nebular
emission-line maps, namely [OIII]$\lambda$5007, H$\alpha$, and
[NII]$\lambda$6583. We show that the physical size of galaxies, M$_{20}$ index,
and concentration have a strong gradient from blue to red optical wavelengths.
We find that the light distribution of the nebular emission is less
concentrated than the stellar continuum. A comparison between the nonparametric
indicators and the galaxy physical properties revealed a very strong
correlation of the concentration with the specific star-formation rate and
morphological type. Furthermore, we explore how the galaxy inclination affects
our results. We find that edge-on galaxies show a more rapid change in physical
size and concentration with increasing wavelength due to the increase in
optical free path. We conclude that the apparent morphology of galaxies
originates from the pure stellar distribution, but the morphology of the ISM
presents differences with respect to the morphology of the stellar component.
Our analysis also highlights the importance of dust attenuation and galaxy
inclination in the measurement of nonparametric morphological indicators,
especially in the the wavelength range 4000-5000 \r{A}.
