  We use Gaia DR3 data to study the Collinder 132-Gulliver 21 region via the
machine learning algorithm StarGO, and find eight subgroups of stars (ASCC 32,
Collinder 132 gp 1--6, Gulliver 21) located in close proximity. Three co-moving
populations were identified among these eight subgroups: (i) a coeval 25
Myr-old moving group (Collinder 132); (ii) an intermediate-age (50--100 Myr)
group; and (iii) the 275 Myr-old dissolving cluster Gulliver 21. These three
populations form parallel diagonal stripe-shape over-densities in the U--V
distribution, which differ from open clusters and stellar groups in the solar
neighborhood. We name this kinematic structure the Collinder 132-Gulliver 21
stream, as it extends over 270 pc in the 3D space. The oldest population
Gulliver21 is spatially surrounded by the Collinder 132 moving group and the
intermediate-age group. Stars in the Collinder 132-Gulliver 21 stream have an
age difference up to 250 Myr. Metallicity information shows a variation of 0.3
dex between the youngest and oldest populations. The formation of the
Collinder132-Gulliver 21 stream involves both star formation and dynamical
heating. The youngest population (Collinder 132 moving group) with homogeneous
metallicity is probably formed through filamentary star formation. The
intermediate-age and the oldest population were then scatted by the Galactic
bar or spiral structure resonance to intercept Collinder 132's orbit. Without
mutual interaction between each population, the three populations are flying by
each other currently and will become distinct three groups again in
approximately ~50Myr.
