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The globular cluster (GC) systems of low-mass late-type galaxies, such as NGC2403, have been poorly studied to date. As a low mass galaxy (M$_{\ast}$ = 7$\times$ 10$^{9}$ M$_{\odot}$), cosmological simulations predict NGC 2403 tocontain few, if any, accreted GCs. It is also isolated, with a remarkablyundisturbed HI disk. Based on candidates from the literature, Sloan Digital SkySurvey and Hyper Suprime-Cam imaging, we selected several GCs for follow-upspectroscopy using the Keck Cosmic Web Imager. From their radial velocities,and other properties, we identify 8 bona-fide GCs associated with either theinner halo or the disk of this bulgeless galaxy. A stellar population analysissuggests a wide range of GC ages from shortly after the Big Bang until thepresent day. We find all of the old GCs to be metal-poor with [Fe/H] $\le$ --1.The age--metallicity relation for the observed GCs suggests that they wereformed over many Gyr from gas with a low effective yield, similar to thatobserved in the SMC. Outflows of enriched material may have contributed to thelow yield. With a total system of $\sim$50 GCs expected, our study is the firststep in fully mapping the star cluster history of NGC 2403 in both space andtime.

Low-Metallicity Globular Clusters in the Low-Mass Isolated Spiral Galaxy NGC 2403