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In this paper we present the results of a wide-field imaging study of theglobular cluster (GC) system of the field S0 galaxy NGC 7457. To derive theglobal properties of the GC system, we obtained deep BVR images with the WIYN3.5 m telescope and Minimosaic Imager and studied the GC population of NGC 7457to a projected radius of approximately 30 kpc. Our ground-based data werecombined with archival and published Hubble Space Telescope data to probe theproperties of the GC system close to the galaxy center and reduce contaminationin the GC candidate sample from foreground stars and background galaxies. Weperformed surface photometry of NGC 7457 and compared the galaxy's surfacebrightness profile with the surface density profile of the GC system. Theprofiles have similar shapes in the inner 1 arcminute (3.9 kpc), but the GCsystem profile appears to flatten relative to the galaxy light at larger radii.The GC system of NGC 7457 is noticeably elliptical in our images; we measure anellipticity of 0.66 +/- 0.14 for the GC distribution, which is consistent withour measured ellipticity of the galaxy light. We integrated the radial surfacedensity profile of the GC system to derive a total number of GCs N_GC = 210 +/-30. The GC specific frequency normalized by the galaxy luminosity and mass areS_N = 3.1 +/- 0.7 and T = 4.8 +/- 1.1, respectively. Comparing the derived GCsystem properties and other empirical data for NGC 7457 to S0 formationscenarios suggests that this field S0 galaxy may have formed in an unequal-massmerger.

The Globular Cluster Population of NGC 7457: Clues to the Evolution of Field S0 Galaxies