  Recent studies suggested that the ejecta velocity of Type Ia supernova (SN
Ia) is a promising indicator in distinguishing the progenitor systems and
explosion mechanisms. By classifying the SNe Ia based on their ejecta
velocities, studies found SNe Ia with high Si II $\lambda$6355 velocities (HV
SNe Ia; v>12000 km/s) tend to be physically different from their
normal-velocity counterparts (NV SNe Ia). In this work, we revisit the low-$z$
sample studied in previous work and closely look into the spatially resolved
environment local to the site of SN explosion. Our results reveal a possible
trend (at $2.4\sigma$ significance) that HV SNe Ia are likely associated with
older stellar populations than NV SNe Ia. While the trend is inconclusive, the
local host-galaxy sample studied in this work is likely skewed toward massive
galaxies, limiting the parameter space that we would like to investigate from
the original parent sample. Nevertheless, our results do not rule out the
possibility that parameters other than the host-galaxy age (such as
metallicity) could be the underlying factors driving the differences between HV
and NV SNe Ia due to the limitation of our dataset.
