A WFC3 study of globular clusters in NGC 4150 - an early-type minor
  merger
  We combine near-ultraviolet (NUV; 2250 {\AA}) and optical (U, B, V, I)
imaging from the Wide Field Camera 3 (WFC3), on board the Hubble Space
Telescope (HST), to study the globular cluster (GC) population in NGC 4150, a
sub-L* (M_B ~ -18.48 mag) early-type minor-merger remnant in the Coma I cloud.
We use broadband NUV-optical photometry from the WFC3 to estimate individual
ages, metallicities, masses and line-of-sight extinctions [E_(B-V)] for 63
bright (M_V < -5 mag) GCs in this galaxy. In addition to a small GC population
with ages greater than 10 Gyr, we find a dominant population of clusters with
ages centred around 6 Gyr, consistent with the expected peak of stellar mass
assembly in faint early-types residing in low-density environments. The old and
intermediate-age GCs in NGC 4150 are metal-poor, with metallicities less than
0.1 ZSun, and reside in regions of low extinction (E_(B-V) < 0.05 mag). We also
find a population of young, metal-rich (Z > 0.3 ZSun) clusters that have formed
within the last Gyr and reside in relatively dusty (E_(B-V) > 0.3 mag) regions
that are coincident with the part of the galaxy core that hosts significant
recent star formation. Cluster disruption models (in which ~80-90% of objects
younger than a few 10^8 yr dissolve every dex in time) suggest that the bulk of
these young clusters are a transient population.
