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M104 (NGC 4594, the Sombrero galaxy) is a mysterious massive early-typegalaxy that shows a dominant bulge and a prominent disk. However, the presenceof a halo in M104 has been elusive, and it is not yet known how M104 hasacquired such a peculiar structure. Using wide ($\sim2$ deg$^2$) and deep $ugi$images of M104 obtained with the CFHT/MegaCam, we detect a large number ofglobular clusters (GCs) found out to $R\approx35'$ ($\sim100$ kpc). The colordistribution of these GCs shows two subpopulations: a blue (metal-poor) systemand a red (metal-rich) system. The total number of GCs is estimated to be$N_{GC}=1610\pm30$ and the specific frequency to be $S_{N}=1.8\pm0.1$. Theradial number density profile of the GCs is steep in the inner region at$R<20'$, and becomes shallow in the outer region at $20'<R<35'$. The outerregion is dominated by blue GCs and is extended out to $R\approx35'$. Thisshows clearly the existence of a giant metal-poor halo in M104. The innerregion is composed of a bulge hosting a disk, corresponding to a metal-richhalo as seen in early-type galaxies. At least two clumps of blue GCs are foundin the outer region. One clump is overlapped with a faint stellar streamlocated in the south west, indicating that it may be a remnant of a disrupteddwarf galaxy. Our results imply that the metal-rich inner halo of M104 formedfirst via major mergers, and the metal-poor outer halo grew via numerous minormergers.

Tracing the Giant Outer Halo of the Mysterious Massive Disk Galaxy M104 I. Photometry of the Extended Globular Cluster Systems