  The general consensus is that LTGs undergo intense star-formation activity,
while ETGs are mostly inactive. We question this general rule and investigate
the existence of star-forming ETGs and quiescent LTGs in the local Universe. By
computing the physical properties of 2,209 such galaxies in the GAMA survey
being morphologically classified and using information on their structural
properties as well as the density of their local environment, we seek for
understanding the differences from their 'typical' counterparts.
  We separate galaxies into subsets based on their dominant ionising process,
making use of criteria based on the WH$_{\alpha}$ width and the
[NII/H$_{\alpha}$] ratio. Taking advantage of the SED fitting code CIGALE we
derive galaxy properties, such as the $M_\text{star}$, $M_\text{dust}$, and SFR
and also estimate the unattenuated and the dust-absorbed stellar emission, for
both the young and old stellar populations.
  Ongoing star-formation activity is found in 47% of ETGs and 8% of LTGs are
quiescent. The star-forming E galaxies, together with the LBSs, constitute a
population that follows very well the SFMS of spiral galaxies. The fraction of
the luminosity originating from young stars in the star-forming ETGs is quite
substantial ($\sim$ 25%) and similar to that of the star-forming LTGs.
Investigating possible differences between star-forming and quiescent galaxies
we find that the intrinsic shape of the SED of the star-forming galaxies is, on
average, very similar for all morphological types. Concerning their structural
parameters, quiescent galaxies tend to show larger values of the S\'ersic index
and larger $R_\text{eff}$ (compared to star-forming galaxies). Finally, we find
that star-forming galaxies preferably reside in lower-density environments
compared to the quiescent ones, which exhibit a higher percentage of sources
being members of groups.
