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We survey globular clusters (GCs) in M85 using $ugi$-band images of a$1^{\circ} \times 1^{\circ}$ field obtained with the MegaCam at the 3.6 mCanada-France-Hawaii Telescope. We identify 1318 GC candidates with 20.0 mag $<g_0 <$ 23.5 mag in the entire survey region. Their radial number densityprofile is well fit by a S{\'e}rsic profile with $n$ = 2.58$^{+0.43}_{-0.33}$and effective radius $R_{\rm e,GCS}$ = 4$\rlap{.}{'}$14 (= 22 kpc), showingthat the candidates at $R < 20'$ are mostly genuine GCs in M85. We estimate thetotal number of GCs, $N$(total) = $1216^{+82}_{-50}$, and the specificfrequency, $S_N = 1.41^{+0.10}_{-0.06}$. The overall color distribution of theGCs in M85 is bimodal, but the GCs in the central region at $R < 2'$ do notshow a bimodal distribution clearly. The radial number density profile andsurface number density map of the blue GCs (BGCs) show more extended structuresthan those of the red GCs (RGCs). The spatial distributions of both BGCs andRGCs are elongated, similar to that of the galaxy stellar light. The numberfraction of the RGCs in the central region is much smaller compared to those inother early-type galaxies of similar luminosity. The mean $(g-i)_0$ color ofthe RGCs in M85 is about 0.1 mag bluer than typical values for other Virgoearly-type galaxies of similar luminosity, indicating that a significantfraction of the RGCs in M85 may be younger than typical GCs. These resultsindicate that M85 might have undergone a major wet merger recently.

A Wide-field Photometric Survey of Globular Clusters in the Peculiar Early-type Galaxy M85