| Deep, wide-field images in B and R-band from the Canada-France-Hawaii Telescope (CFHT) are used to study the globular cluster system (GCS) of the Sombrero galaxy (also known as M104). M104 is a nearby (9 Mpc) spiral galaxy of type Sa, viewed nearly edge-on. The major properties of the system investigated are the globular cluster luminosity function (GCLF), colour distribution or metallicity distribution function (MDF), the spatial distribution, and the total population of globular clusters. The data extend nearly two magnitudes past the GCLF turnover magnitudes, which are measured to be B0 = 23.09 +/- 0.12 and R0 = 21.78 +/- 0.10. The colour distribution is found to be bimodal in structure, with peaks at (B - R) 0 = 1.22 +/- 0.02 and (B - R)0 = 1.50 +/- 0.04. The colour distribution is also converted into a metallicity or abundance distribution, to which is fit a two-phase accreting-box chemical enrichment model. Spatially, the GCS is found to be nearly round, and having a general power-law shape radially. A global power-law index of alpha = -1.32 +/- 0.06 is found for the entire system, but for the two populations an index of alpha = -1.05 +/- 0.04 and alpha = -1.70 +/- 0.09 is found for the blue and red populations respectively. As a system, the Sombrero galaxy is estimated to have a total population of Ncl = 2000 +/- 200, with a corresponding specific frequency of SN = 2.3 +/- 0.2. Overall, the GCS of M104 is found to be normal, though large for a spiral galaxy.; Also achieved in this thesis were some technical highlights. Artificial star tests with over a million stars were performed along with a methodology to make the process feasible and efficient. A direct benefit of the huge artificial star tests was the ability to assess the photometric magnitude uncertainties. Some numerical techniques were also used, such as several methods to determine the turnover magnitude of the GCLF, and fitting an azimuthal profile while exploring the spatial distribution. |
