  The connection between quenching mechanisms, which rapidly turn star-forming
systems into quiescent, and the properties of the galaxy population remains
difficult to discern. In this work we investigate the physical properties of
MaNGA and SAMI galaxies at different stages of their star formation history.
Specifically, we compare galaxies with signatures of recent quenching
(Quenched) -- $\rm H(\alpha)$ in absorption and low $D_n(4000)$ -- with the
rest of the low star-forming and active population (Retired and Ageing,
respectively). The analysis is performed in terms of characteristics such as
the total stellar mass, half-light radius, velocity-to-dispersion ratio,
metallicity, and environment. We find that the Ageing population comprises a
heterogeneous mixture of galaxies, preferentially late-type systems, with
diverse physical properties. Retired galaxies, formerly Ageing or Quenched
systems, are dominated by early-type high-mass galaxies found both at low and
dense environments. Most importantly, we find that recently quenched galaxies
are consistent with a population of compact low-mass satellite systems, with
higher metallicities than their Ageing analogues. We argue that this is
compatible with being quenched after undergoing a star-burst phase induced by
environmental processes (e.g. ram pressure). However, we also detect a
non-negligible fraction of field central galaxies likely quenched by internal
processes. This study highlights that, in order to constrain the mechanisms
driving galaxy evolution, it is crucial to distinguish between old (Retired)
and recently quenched galaxies, thus requiring at least two estimates of the
specific star formation rate over different timescales.
