We combine near-ultraviolet ( NUV ; 2250Ã ) 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 } \sim - 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 Z _ { \odot } , 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 Z _ { \odot } ) 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 \sim 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 .