Low-resolution , ultraviolet-to-visual spectra of two candidate globular clusters in the merger remnant NGC 3921 ( cz _ { { } _ { LG } } = 6021 km s ^ { -1 } ) are presented .
These two clusters of apparent magnitude V \approx 22.2 
( M _ { V } \approx - 12.5 ) lie at projected distances of about 5 kpc ( 0.9 R _ { eff } ) from the center and move with halo-type radial velocities relative to the local galaxy background .
Their spectra show strong Balmer absorption lines [ EW ( H \beta – H \delta ) = 11 – 13 Å ] indicative of main-sequence turnoffs dominated by A-type stars .
Comparisons with model-cluster spectra computed by Bruzual & Charlot and others yield cluster ages in the range of 200 – 530 Myr , and metallicities about solar to within a factor of three .
Given their small half-light radii ( \mbox { $R _ { eff } $ } \lesssim 5 pc ) and ages corresponding to \sim 10 ^ { 2 } core-crossing times , these clusters are gravitationally bound and , hence , indeed young globulars .
Assuming that they had Chabrier-type initial mass functions , their estimated current masses are ( 2.3 \pm 0.1 ) \times 10 ^ { 6 } \mbox { $ { \cal M } _ { \odot } $ } and ( 1.5 \pm 0.1 ) \times 10 ^ { 6 } \mbox { $ { \cal M } _ { \odot } $ } , respectively , or roughly half the mass of \omega Cen .
Since NGC 3921 itself shows many signs of being a 0.7 \pm 0.3 Gyr old protoelliptical , these two young globulars of roughly solar metallicity and their many counterparts observed with the Hubble Space Telescope 
provide supporting evidence that , in the process of forming elliptical-like remnants , major mergers of gas-rich disks can also increase the number of metal-rich globular clusters .