  Spatially resolved MaNGA's optical spectra of 1072 present-day lenticular
(S0) galaxies, dimensionally reduced from a principal component analysis (PCA),
are used to determine their radial activity structure shaped by any possible
nebular ionization source. Activity profiles within $1.5\,R_{\mathrm e}$ are
examined in tandem with the mass, age, ellipticity and kinematics of the stars,
as well as environmental density. Among the results of this comparison, we find
that the sign of the radial activity gradient of S0s is tightly related to
their PCA classification, BPT designation, and star formation status.
PCA-passive lenticulars often show low-level, flat activity profiles, although
there is also a significant number of systems with positive gradients, while
their less common active counterparts generally have negative gradients,
usually associated with high SSFRs and, sometimes, moderate Seyfert emission. A
fraction of the latter also shows radial activity profiles with positive
gradients, which become more abundant with increasing stellar mass regardless
of environmental density. Our analysis also reveals that the subset of active
S0s with negative gradients experiences at all galactocentric radii a
systematic reduction in its median activity level with stellar mass, consistent
with expectations for main sequence galaxies. In contrast, passive S0s with
positive gradients show the opposite behaviour. Furthermore, systems whose
activity is dominated by star formation are structurally rounder than the rest
of S0s, while those classified as Seyfert exhibit higher rotational support.
The possibility that negative and positive activity gradients in S0s may result
from rejuvenation by two distinct types of minor mergers is raised.
